Author name code: kotov
ADS astronomy entries on 2022-09-14
author:"Kotov, Valery A." 
------------------------------------------------------------------------  

Title: The fine structure of the rotational periods of the solar
    mean magnetic field
Authors: Haneychuk, Vasily Ivanovich; Kotov, Valery Alexandrovich
Bibcode: 2021OAst...30..176H
Altcode:
  The data of mean magnetic field (MMF) of the Sun obtained at the Wilcox
  Solar Observatory (Stanford, USA) in 1975-2020 are analysed. It was
  concluded that the MMF maximum occurs, on average, 1.5-2 years later
  relative to the maximum of Wolf numbers. To analyze the changes
  in the MMF, a new method for searching for periodicities has been
  developed, which takes into account the change in the sign of the
  magnetic field from cycle to cycle. This method made it possible to
  find the main synodic periods of rotation of the magnetic field with
  values of 27<SUP>d</SUP>.021 ± 0<SUP>d</SUP>.008, 26<SUP>d</SUP>.796
  ± 0<SUP>d</SUP>.008 and 27<SUP>d</SUP>.260 ± 0<SUP>d</SUP>.008, each
  of which has two splitting components associated with a change in the
  polarity of the magnetic field during the transition from one cycle of
  solar activity to another. The stability of these periodicities for more
  than 45 years indicates that the Sun as a star looks like a horizontal
  magnetic dipole (in addition to the observed vertical one), which
  changes its sign every 11 years and rotates with different periods.

Title: Oscillations of solar photosphere: 45 years of observations
Authors: Kotov, Valery A.; Haneychuk, Vasilij I.
Bibcode: 2020AN....341..595K
Altcode:
  A summary of the long-term, 1974-2018, measurements of the
  line-of-sight velocity of the solar photosphere, performed at the
  Crimean Astrophysical Observatory, is presented. The work shows that
  the Sun is pulsating with two periods: P<SUB>0</SUB> = 9,600.606(12)
  s and P<SUB>1</SUB> = 9,597.924(13) s. The new measurements, 1996-2018,
  confirm the remarkable phase stability of the second period. The true
  origin of both pulsations is unknown, but their beatings are noted to
  have occurred with a period of 397.7(2.6) days, coinciding well with
  the synodic period of Jupiter, 398.9 days. A hypothesis is advanced
  that the shift from P<SUB>0</SUB> to P<SUB>1</SUB> is induced by the
  gravity field of Jupiter.

Title: Rotation anomaly of the Sun
Authors: Kotov, Valery A.
Bibcode: 2020AN....341..588K
Altcode:
  Does the Sun always rotate correctly? On the basis of the measurements
  of its mean magnetic field (more than 27 thousand daily values,
  obtained by seven observatories during 1968-2018) and resonance
  relations of the solar system, the sidereal spin period of the Sun as
  a star is determined as 25.165(6) days and that of the solar equator
  as 25.081(7) days. After 1993, however, a remarkable violation of
  the solar equatorial rate, through an unknown cause, has happened:
  the spin coherency of the mean field disintegrated and made way for
  nearly chaotic variations with quasi-periods of 24.7-25.4 days. The
  phenomenon is thought to be tied to anomaly of the Wolf cycles 23 and
  24, accompanied presumably by a global change of the Earth's climate
  (with unclear mechanism of the Sun-Earth influence).

Title: Superfast Exoplanets and 9600 s
Authors: Kotov, V. A.
Bibcode: 2019EM&P..123....1K
Altcode: 2019EM&P..tmp....6K
  Motion of a substantial part of the superfast exoplanets is found
  to be in the close resonance with the well-known "solar" timescale
  P<SUB>0</SUB> ≈ 0.11 days and/or the timescale 2P_0/π ≈ 0.07 days
  (at 99.9% confidence for exoplanet periods P &lt; 2 days). There is
  also a noticeable lack of the exoplanetary "unstable" orbits with
  P ≈ 3 π P_0 ≈ 1.05 days, which copies the famous "period gap"
  of the cataclysmic variables at P ≈ 0.11 days; strangely enough,
  the ratio of the central periods of these two gaps is equal to π
  ^2. The exoplanet phenomenon is supposed to be caused by a coherent,
  with the P_0 timescale, oscillation of gravity, operating within the
  extra-solar planetary systems.

Title: Is the Earth's orbital motion linked to the spin rotation of
    the Sun?
Authors: Kotov, V. A.
Bibcode: 2019AdSpR..63.3385K
Altcode:
  Time variations of the magnetic field of the Sun, seen as a star (the
  data 1968-2018, with more than 27 thousand daily measurements of the
  solar mean magnetic field), allowed to specify the rotation period of
  the gravitating solar mass: 27.027(6) days, synodic. This indicates
  a presumably unknown physical connection between motions of the Sun
  and the Earth: in the course of a year our star accomplishes nearly
  27 half-revolutions, while the planet itself performs an identical
  number of its spinnings during one complete axial revolution of the
  Sun. True origin of this strange Sun-Earth resonance is unknown,
  but it is supposed the phenomenon might be caused by slight coherent
  perturbations of gravity within the solar system.

Title: Near-annual variation of the magnetic Sun
Authors: Kotov, V. A.
Bibcode: 2019Ap&SS.364...45K
Altcode:
  Over past 51 years (1968-2018) the general magnetic field of the Sun
  was measured nearly each day by the Crimean Astrophysical Observatory,
  the Wilcox Solar Observatory and five others. It is shown that the
  annual variation of this field (longitudinal component), thought to be
  caused by the inclination of the Sun's axis to ecliptic, is splitted
  into two components with periods 0.954(3) years and 1.034(4) years
  (with mean amplitudes ≈ 0.044 G). But while the first one agrees
  well with the expected period 0.957(4) years (caused by the 11-year
  polar field reversals and coupled to the yearly projection effect),
  the second one is shifted relative to its theoretical value, 1.047(4)
  years, by Δ = 0.013(5) years (99% confidence). The beat period of the
  two observed components, 12.3(7) years, agrees well with the Jovian
  period 11.9 years, being close also to the length of the 11-year
  cycle. Since the modern astronomy rejects a planetary influence on
  the Sun, the origin of both the 1.034-year periodicity and the shift
  Δ remains to be mysterious.

Title: Fast Spinning of Planets
Authors: Kotov, V. A.
Bibcode: 2018EM&P..122...43K
Altcode: 2018EM&P..tmp...15K
  Spin periods of Jupiter, Saturn, Uranus and Neptune are specified by
  the analysis of the resonant motion of large satellites: P = 0.445(2)
  d, 0.448(1) d, 0.673(9) d and 0.561(7) d, respectively. They occur to
  be near-commensurate with P_0=9600.606(12) s, the period of the "cosmic"
  oscillation, discovered first in the Sun, then in other variable objects
  of the Universe. The like analysis of spin rates of the total set of the
  largest and fastest rotators of the Solar system (with mean diameters
  ≥ 500 km and P &lt; 2 d,—of planets, asteroids and satellites)
  resulted in the best commensurable, or "synchronizing", timescale
  9594(65) s, coinciding fairly well with P_0 too (the probability that
  the two timescales could agree by chance, is less than 10^{-5}). True
  origin of this odd common resonance of our planetary system is unknown.

Title: Harmony of the solar system
Authors: Kotov, V. A.
Bibcode: 2018AN....339..513K
Altcode:
  From 1968 to 2017, the Crimean Astrophysical Observatory, the Wilcox
  Solar Observatory, and five other observatories performed more
  than 27 thousand daily measurements of the mean magnetic field of
  the Sun-as-a-star. These data reveal the presence of the long-term
  coherent periodicity P<SUB>S</SUB> = 13.4582(25) days, characterizing
  the four-sector pattern of the magnetic Sun. To clear up the origin
  of this periodicity, motions of planets and massive satellites are
  considered in detail. It is shown that the best commensurate timescale
  of all those periodic motions is equal to P<SUB>G</SUB> = 13.4577(10)
  days, which agrees fairly well with P<SUB>S</SUB> (the probability
  of a chance coincidence is less than 2 × 10<SUP>-9</SUP>). Physical
  nature of this odd P<SUB>S</SUB>-P<SUB>G</SUB> resonance is unknown,
  but it is supposed that the phenomenon is caused by coherent periodic
  fluctuations of the gravity field within the solar system.

Title: Motion of the fast exoplanets
Authors: Kotov, Valery A.
Bibcode: 2018Ap&SS.363...55K
Altcode:
  It is shown that a number of superfast, with periods &lt; 2 d,
  exoplanets revolve around parent stars with periods, near-commensurate
  with P<SUB>E</SUB> and/or 2 P<SUB>E</SUB> / π, where the exoplanet
  resonance timescale P<SUB>E</SUB>=9603(85) s agrees fairly well with
  the period P<SUB>0</SUB>= 9600.606(12) s of the so-called "cosmic
  oscillation" (the probability that the two timescales would coincide
  by chance is near 3 ×10^{-4}; the P<SUB>0</SUB> period was discovered
  first in the Sun, and later on—in other objects of Cosmos). True
  nature of the exoplanet P<SUB>0</SUB> resonance is unknown.

Title: Rotation of the Solar Equator
Authors: Kotov, V. A.
Bibcode: 2017SoPh..292...76K
Altcode:
  Regular measurements of the general magnetic field of the Sun, performed
  over about half a century at the Crimean Astrophysical Observatory,
  the J. Wilcox Solar Observatory, and five other observatories, are
  considered in detail for the time 1968 - 2016. They include more
  than twenty-six thousand daily values of the mean line-of-sight field
  strength of the visible solar hemisphere. On the basis of these values,
  the equatorial rotation period of the Sun is found to be 26.926(9)
  d (synodic). It is shown that its half-value coincides within error
  limits with both the main period of the magnetic four-sector structure,
  13.4577(25) d, and the best-commensurate period of the slow motions of
  the major solar system bodies, 13.479(22) d (sidereal). The probability
  that the two periods coincide by chance is estimated to be about
  10<SUP>−7</SUP>. The true origin of this odd resonance is unknown.

Title: Solar 22 years cycle
Authors: Kotov, Valery A.; Sanchez, Francis M.
Bibcode: 2017Ap&SS.362....6K
Altcode:
  Seven observatories performed in 1968-2015 numerous daily measurements
  of general magnetic field of the Sun seen as a star (of a mean
  line-of-sight field component of the visible solar hemisphere). The
  new data 2013-2015 confirmed the recent prediction about saw-edged
  profile of the mean curve of the Hale's 22 years magnetic cycle and,
  thus, a hypothesis about its cosmological (partial) origin. This is
  supported by a special analysis of epochs of extrema of Wolf's sunspot
  number, demonstrating a remarkable stability, since Galileo's time,
  of the initial phase of the cycle, which can hardly be explained by
  dynamo theory exclusively.

Title: The Jovian period in the Sun?
Authors: Kotov, V. A.
Bibcode: 2015AdSpR..56.1276K
Altcode:
  The 41-year measurements of the Doppler effect of the photosphere
  performed at the Crimean Astrophysical Observatory, discovered
  two periods of global oscillations of the Sun: 9600.606(12) s and
  9597.929(15) s. Their beat period, 398.4(2.9) d, well agrees with a
  synodic orbital period of Jupiter, P<SUB>J</SUB> = 398.9 d, raising a
  new problem for solar physics, cosmogony and cosmology. A hypothesis
  is advanced that the P<SUB>J</SUB> beating of the Sun is induced by
  gravitation of Jupiter, revolving in a privileged reference system
  "the Sun - the Earth".

Title: On the origin of the 22 years solar cycle
Authors: Kotov, V. A.
Bibcode: 2015AdSpR..55..979K
Altcode:
  Measurements of the general magnetic field of the Sun seen as
  a star were performed over last 45 years by the CrAO and five
  other observatories (1968-2012, nearly 23 thousand daily strengths
  B). Analysis of the B time series showed that the most substantial
  long-term period of the field variation is the Hale's cycle 22 years,
  which cannot be explained by dynamo theory. It reveals a saw-edged
  profile, indicating perhaps a cosmic origin of the cycle.

Title: Extrasolar worlds: We should contact aliens?
Authors: Kotov, V. A.
Bibcode: 2013BCrAO.109..136K
Altcode:
  More than 840 exoplanets have been discovered and many people
  believe that on some of these planets there may be extraterrestrial
  civilizations. Astronomers, however, warn against contacts with
  aliens because of the possible dangers to humankind… In this paper
  I show that the solar system is a unique phenomenon in the universe
  and there cannot be any extraterrestrial civilizations. Being the
  "anthropic center" of the world, the earth and the sun are "designed"
  for the development of humankind and the cosmos as a supercomputer. This
  conclusion follows from an analysis of exoplanet orbits that is based
  on a coherent cosmic oscillation with a period of P <SUB>0</SUB> ≈
  9600.6 s (discovered in the sun and some extragalactic sources). The
  non-Doppler nature of the P <SUB>0</SUB> phenomenon is emphasized;
  this phenomenon appears to be related to the absolute time of the
  universe in the Newtonian sense.

Title: The newtonian constant
Authors: Kotov, V. A.
Bibcode: 2013BCrAO.109..142K
Altcode:
  The data on the coherent cosmic oscillation (with a period of 9600.6 s)
  and the finely tuned relationships between the constants of the micro-
  and macroworlds is used to adjust the Newtonian constant: G = 6.67543(2)
  × 10<SUP>-8</SUP> cm<SUP>3</SUP> g<SUP>-1</SUP> s<SUP>-2</SUP>.

Title: Whether There is an Astrophysical Source in the Oscillations
    of Geophysical Parameters with a Period of 160 Minutes?
Authors: Samsonov, S.; Miroshnichenko, L.; Kotov, V.; Skryabin, N.;
   Timofeev, V.; Baishev, D.
Bibcode: 2013OAP....26..279S
Altcode:
  Oscillations with a period of 160 minutes in the ground pressure and
  Z-component of the geomagnetic field revealed by authors earlier are
  studied the regular ground measurements. For the analysis the data
  of five stations on the territory of Europe (Moscow, Apatity, Oulu)
  and Siberia (Yakutsk, Tixie) obtained in December, 2003 are used. It
  is shown that the specified oscillations revealed by authors earlier,
  are manifested in Europe and Siberia synchronously. For December, 2003
  the mean amplitude of oscillations in the ground pressure accounts for
  0.012±0.002 mb; in a Z-component their value is equal to 0.323±0.070
  nT. Authors discuss the possible nature of pulsations.

Title: Enigmas in measurements of solar magnetic field
Authors: Kotov, V. A.
Bibcode: 2012BCrAO.108...20K
Altcode:
  The mean magnetic field (MMF) of the photosphere of the Sun as a star
  was measured in 2001-2010 at the Crimean Astrophysical Observatory
  using two Fe I absorption lines with λ = 524.7 nm and λ = 525.0
  nm. The regression coefficient b for 1054 pairs of daily values measured
  simultaneously on both lines equals 0.82 (a correlation coefficient is
  0.94; magnetic field strengths determined by the line with λ = 525.0
  nm are lower than those for the line with λ = 524.7 nm). However,
  the b value varied significantly along with phases of the 11-year
  cycle from 0.88 in 2003 to 0.49 in 2009. It is difficult to ascribe
  these variations to purely instrumental or solar causes. Moreover,
  the semiannual value of b decreased with the decrease in the absolute
  strength of the MMF, which contradicts the model of thin magnetic flux
  ropes of the photosphere. Similar behavior of b was also observed in
  the comparison of MMF measured at the Crimean Astrophysical Observatory
  and Stanford by the line with λ = 525.0 nm. The inconsistency of the
  results obtained by these two iron lines on different instruments
  has been noted. It has been concluded that the variance in and odd
  behavior of b are predetermined not only by the instrument and the Sun
  (by the so-called fine structure of the photosphere field), but also
  by the act of measuring. When recording solar (and stellar) magnetic
  fields and modeling atmospheric processes, quantum effects have to be
  taken into account, such as nonlocality, indistinguishability, and the
  entanglement of photons, as well as that a photon only acquires its
  properties at the exact moment of its detection. The best approximation
  to reality can be achieved by averaging the MMF measurements carried
  out with different magnetographs and in different spectral lines.

Title: Comments on ultrafast neutrinos (December 2011)
Authors: Kotov, V. A.; Sanchez, F. M.
Bibcode: 2012BCrAO.108..115K
Altcode:
  The striking news released in the fall of 2011 about the detection
  of a neutrino travelling faster than light has stunned physicists
  and cosmologists. We explain the phenomenon based on a holographic
  stationary model of the Universe that implies the existence of
  supraluminal speeds and Grand Cosmos external to the Hubble sphere.

Title: The sun and exoplanets: The solitude of man
Authors: Kotov, V. A.
Bibcode: 2012BCrAO.108...30K
Altcode:
  Solar pulsations with a period of P <SUB>0</SUB> = 9600.606(12)
  were discovered in 1974. A more recent discovery is that planetary
  distances in the solar system are subject to spatial resonance with
  the parameter L <SUB>0</SUB> ≡ cP <SUB>0</SUB> ≈ 9600 ls and that
  the P <SUB>0</SUB> pulsation itself has cosmological significance
  (coherent cosmic oscillation, or the pace of absolute time of the
  universe; c is the speed of light). As of June 2011, 552 extrasolar
  planets have been discovered. Statistical analysis shows that the
  distribution of the semimajor axes of alien planets does not have
  L <SUB>0</SUB> resonance. Moreover, it appears to have no resonance
  at all. This frustrates the 20th-century hopes for the existence of
  extraterrestrial civilizations and possible contact with them. They are
  simply not there. This explanation of the Fermi paradox, or the Great
  Silence, appears to rest on the triumph of the anthropic principle,
  which has been successfully implemented by nature within our planetary
  system. This leads to a vision whereby the cosmos seems to be created
  specially for us. The scale L <SUB>0</SUB> indicates that the sun is
  a special quantum object, where L <SUB>0</SUB> is a wave function
  parameter that is not subject to the rational principles of the
  classical world, but rather follows a peculiar, quantum logic.

Title: On possible cosmic origin of the 11-year solar cycle
Authors: Kotov, V. A.; Sanchez, F. M.; Bizouard, K.
Bibcode: 2012BCrAO.108...36K
Altcode:
  In order to test Dicke's idea of a clock hidden inside the Sun and
  determine the initial phase of the solar cycle, the epochs of the
  extrema of the Wolf numbers observed over the past 400 years are
  examined. It is shown that extrema that obey the period P <SUB> W
  </SUB> equaled 11.07(4) years retain the initial phase, which cannot be
  explained in terms of local physics and concepts of the past century
  regarding the mechanism of the solar cycle based on the theory of a
  magnetic dynamo and the phenomenological model of the Babcock-Leighton
  cycle. It is suggested that the cycle has a cosmic (cosmological)
  origin. This is clearly indicated by the correlation of the cycle
  period with a holographic time-scale of the Universe, ( a <SUB>0</SUB>
  R <SUP>3</SUP>)<SUP>1/4</SUP>/ c ≈ 11.0(4) years, where a <SUB>0</SUB>
  and R are the radii of the first Bohr orbit of a hydrogen atom and the
  observable Universe, respectively, and c is the speed of light. It is
  noted that there are other strict holographic relations that include
  a <SUB>0</SUB>, R, P <SUB> W </SUB>, the wavelength of the microwave
  background radiation (with a temperature of 2.7 K), and a period of the
  global solar pulsations equal to 9600.6 s. The true physical nature
  of the governing mechanism for the 11-year cycle can perhaps only
  be understood based on modern concepts about the nonlocality of our
  world, which follows from Bell's theorem, which is grounded on the
  achievements of quantum mechanics at the turn of the 20th and 21st
  centuries, as well as using a model of a holographic Universe free of c.

Title: Commentary on the OPERA Superluminal Neutrinos
Authors: Sancheza, Francis M.; Kotov, Valery A.
Bibcode: 2012JCos...18.8081S
Altcode:
  No abstract at ADS

Title: Towards a synthesis of two cosmologies: the steady-state
    flickering Universe
Authors: Sanchez, Francis M.; Kotov, Valery A.; Bizouard, Christian
Bibcode: 2011JCos...17.7225S
Altcode:
  A gravitation/electricity symmetry gives directly the Hubble radius
  (within its 4% indetermination), while a "black atom" model confirms
  the time-invariance of the radius of a critical steady-state
  Universe. This refutes the Primordial Big Bang model and permits
  to apply the holographic principle to the invariant Hubble sphere,
  with the extension to a holophysics principle, introducing a tachyonic
  scanning in a critical steady-state flickering Universe. This suggests a
  transient validity of the Big Bang approach, announcing a reconciliation
  of the two main cosmologies. Several main fine-tuning relations are
  shown to be of a holophysical character, i.e. a topological conservation
  involving the main physical lengths. The elimination of light speed
  from the interaction formulae defines both a timescale 13.7 Gyr
  (within 1% of the so-called age of the Universe, which is interpreted
  rather as the temporal regeneration constant of the steady-state model)
  and, within 10-4 uncertainty of 𝐺, the coherent cosmic oscillation
  period 9600.61(3) s. The latter is shown to be intrinsically connected
  by holophysics with the redshift periodicity 71.7 km/s and the Wolf
  solar period 11.05 years. The flickering concept opens the door for
  a cosmic interpretation of particle physics; for instance, the parity
  violation would be tied to a scanning chirality.

Title: Cosmic vibration of the sun and quasar 3C 273
Authors: Kotov, V. A.
Bibcode: 2011BCrAO.107...70K
Altcode:
  The hypothesis that some extragalactic objects pulsate with a period
  of P <SUB>0</SUB> = 9600.606(12) s, which was first discovered in the
  Sun, is tested with data on quasar 3C 273. Observations of its rapid
  photometric variability were made by different observers in 1968-2005
  within several spectral bands. At the 4σ confidence level, these data
  show that there is a period of 9600.624(18) s, which is consistent,
  within the error limits, with P <SUB>0</SUB> (mean harmonic amplitude
  0.006 B magnitude). Its independence from the redshift z is a sign
  of a cosmological origin of the P <SUB>0</SUB> pulsation, which is
  sometimes understood as the "rhythm" of cosmos' absolute time. This
  phenomenon is also shown to be deeply connected—via the Sanchez
  formula—to the fundamental constants of physics and cosmology. This
  refutes the standard Big Bang hypothesis and confirms the Steady State,
  c-free model of the Universe ( c is the speed of light).

Title: Pulsations of the sun and a beat period of 399 days
Authors: Kotov, V. A.; Khaneichuk, V. I.
Bibcode: 2011BCrAO.107...67K
Altcode:
  Measurements of the Doppler effect of the solar photosphere have
  been carried out at the Crimean Astrophysical Observatory for 37
  years, beginning in 1974 (in total, 2188 days or 13 247 h). The
  measurements use the differential center-to-limb method of registration
  of line-of-sight velocity with a solar magnetograph (in the iron
  absorption line λ512.4 nm). As a result of the experiment, two global
  pulsations of the sun with periods P <SUB>0</SUB> = 9600.606(12) and
  P <SUB>1</SUB> = 9597.936(16) s have been discovered. The nature of
  the periods is unknown. The first pulsation was detected in 1974-1982;
  the second, during nearly all the 37 years. The 2008-2010 data confirm
  the stability of the initial phase of the P <SUB>1</SUB> pulsation
  with a mean (differential) amplitude of 0.25 m/s. The fact that the
  beat period of the two pulsations coincides with the synodic period
  of Jupiter's orbital revolution, i.e., 399 days, raises a new, complex
  problem for solar physics and cosmogony.

Title: Minimum of 2008 or the ``quantum'' Sun-2
Authors: Kotov, V. A.
Bibcode: 2010BCrAO.106..137K
Altcode:
  The prolonged 2007-2009 minimum is a big surprise for solar physics. In
  order to reveal the causes, we analyze the variability of the general
  magnetic field (GMF) of the Sun as a star measured by CrAO and five
  other observatories since 1968 (more than 19000 daily field strengths
  B were obtained in 41 years). Sharp yearly mean extrema of the negative
  (S) field took place in 1969, 1990, and 2008, with the third extremum,
  in contrast to the two previous ones, having coincided with the sunspot
  minimum. This explains both the long duration of the minimum and the
  record (over the last 100 years) increase in the length of the Wolf
  cycle (no. 23) to 12 or more years. The S-field extrema followed with
  a period of 19.5 ± 1.1 yr—some mean between the 22.1 ± 0.3-yr
  sunspot cycle, the 18.6-yr saros, and the 19.9-yr Jupiter-Saturn
  conjunction period. It is pointed out that, for some unclear reason,
  the negative polarity dominated on the Sun in 1968-2008: the overall
  mean B = -0.021 ± 0.015 G. The existence of a second Sun that obeys
  the laws of quantum mechanics is hypothesized. The “quantum” model
  of the Sun-2 explains many properties of the “classical” Sun-1,
  including the coronal heating, cyclic activity, periodic variations
  in GMF, and its sector structure.

Title: An absolute clock of the cosmos?
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 2010BCrAO.106..127K
Altcode:
  In 1968-2005 different observers (mainly, one of the
  authors—V.M. Lyuty) performed numerous measurements of luminosity
  of the nucleus of the Seyfert galaxy NGC 4151. It is shown that (
  a) luminosity of the object pulsated over 38 years with a period of
  160.0106(7) min coinciding, within the error limits, with the well-known
  period P <SUB>0</SUB> = 160.0101(2) min of the enigmatic “solar”
  pulsations, and ( b) when registering oscillations of luminosity
  of NGC 4151 nucleus with the P <SUB>0</SUB> period, time moments of
  observations must be reduced to the earth instead of the sun, i.e.,
  to the reference frame of the observer. The coherent P <SUB>0</SUB>
  oscillation is characterized, therefore, by invariability of both
  frequency and phase with respect to redshift z and the earth’s orbital
  motion, respectively. From these results it, thus, follows that the
  coherent P <SUB>0</SUB> oscillation seems to be of a true cosmological
  origin. The P <SUB>0</SUB> period itself might represent a course of
  the “cosmic clock” related to the existence of an absolute time
  of the Universe in Newton’s comprehension.

Title: Forty years of measurements of the mean magnetic field of
the Sun: View from today
Authors: Kotov, V. A.
Bibcode: 2009BCrAO.105...45K
Altcode:
  No abstract at ADS

Title: Solar system, exoplanets, and anthropic principle
Authors: Kotov, V. A.
Bibcode: 2009BCrAO.105..119K
Altcode:
  No abstract at ADS

Title: The Sun and the transcendental world of binaries
Authors: Kotov, V. A.
Bibcode: 2008BCrAO.104..125K
Altcode:
  The theory of gravity says that a binary with orbital frequency ν
  should be a source of gravitational waves at the double frequency and
  higher harmonics. This implies that long-term exposure of an ensemble
  of binaries to gravity waves with frequency ν<SUB>G</SUB> can result in
  (a) a lack of binaries with frequencies near frequency ν<SUB>G</SUB>/2
  and its higher harmonics (the effect of unstable orbits) and/or (b)
  an excess of binaries whose orbital frequencies are "absolutely"
  incommensurable with ν<SUB>G</SUB>/2 and its higher harmonics
  (the effect of stable orbits). It is assumed that the stable-orbit
  frequencies are almost equal to multiples of πν<SUB>G</SUB>/2
  and ν<SUB>G</SUB>/2π, where π plays the role of a "perfect"
  factor ensuring the best antiresonance of binaries. The statistical
  analysis of frequencies of 5774 Galactic close binary systems (CBSs)
  with periods P less than 10 days is based on calculating the resonance
  spectrum that indicates the best common multiple for a given set of
  frequencies with allowance for the factor π. The CBS distribution
  turns out to be modulated by the frequency ν<SUB>G</SUB> = 104.4(5)
  μHz, and this effect is the most pronounced for superfast and compact
  rotators, such as cataclysmic variables (CVs) and related objects. The
  frequency ν<SUB>G</SUB> is, within the error, equal to the "enigmatic"
  frequency ν<SUB>0</SUB> = 104.160(1) μHz com discovered earlier in the
  power spectra of the Sun and brightness variations of some extragalactic
  sources. This confirms the existence of a "coherent cosmic oscillation"
  of the Universe with frequency ν<SUB>0</SUB>(ν<SUB>G</SUB>). The
  new astrophysical phenomenon naturally explains an "CV period gap"
  at frequencies ≈πν<SUB>G</SUB>/3 (P ≈ 153 min) and maxima at the
  neighboring frequencies ≈πν<SUB>G</SUB>/2 and ≈πν<SUB>G</SUB>/4
  (P ≈ 102 and ≈204 min, respectively). The remarkable and
  "mysterious" role of the transcendental number π for the world of
  binaries is emphasized, and the mystery of physical nature of the
  "universal" oscillation ν<SUB>0</SUB>(ν<SUB>G</SUB>) is highlighted.

Title: A paradox in measuring the magnetic field of the Sun
Authors: Kotov, V. A.
Bibcode: 2008BCrAO.104...79K
Altcode:
  Significant discrepancies are often observed among the values of the
  mean magnetic field (MMF) of the Sun as a star observed by various
  instruments using various spectral lines. This is conventionally
  attributed to the measurement errors and "saturation" of a solar
  magnetograph in fine-structure photospheric elements with a strong
  magnetic field. Measurements of the longitudinal MMF performed in
  1968-2006 at six observatories are compared in this paper. It is
  shown that the degree of discrepancy (slopes b of linear regression
  lines) varies significantly over the phase of the 11-year cycle. This
  gives rise to a paradox: the magnetograph calibration is affected
  by the state of the Sun itself. The proposed explanation is based
  on quantum properties of light, namely, nonlocality and "coupling"
  of photons whose polarization at the telescope-spectrograph output
  is determined by spacious parts of the solar disk. In this case,
  the degree of coupling, or "identity," of photons depends on the field
  distribution in the photosphere and the instrument design (as Bohr said,
  "the instrument inevitably affects the result"). The "puzzling" values
  of slope b are readily explained by the dependence of the coupling
  on the solar-cycle phase. The very statistical nature of light makes
  discrepancies unavoidable and requires the simple averaging of data
  to obtain the best approximation of the actual MMF. A 39-year time
  series of the MMF absolute value is presented, which is indicative of
  significant variations in the magnitude of the solar magnetic field
  with a cycle period of 10.5(7) yr.

Title: Oscillations of the Sun: Results of observations in 1974 2007
Authors: Kotov, V. A.; Haneychuk, V. I.
Bibcode: 2008BCrAO.104...45K
Altcode:
  Doppler measurements of the photosphere of the entire Sun carried out
  at the Crimean Astrophysical Observatory (CrAO) in 1974-2007 by the
  differential technique showed the presence of an enigmatic periodicity
  of P<SUB>1</SUB> = 159.967(4) min. The phase of this oscillation
  was constant over the entire 34-year of surveys and interval. The
  true nature of this phenomenon is unknown. Pulsation with the former
  period P<SUB>0</SUB> = 160.0101(15) min has been reliably detected
  only in the first nine years, from 1974 to 1982. It is noted that (a)
  the average amplitude of the P<SUB>1</SUB> oscillation in the first
  half of the data was nearly 34% higher than in the second half and (b)
  the beat period of 400(14) d of these two pulsations is equal within
  error to the Jovian synodic period (399 d). A hypothesis is discussed
  relating the P<SUB>1</SUB> oscillation to the superfast rotation of
  the inner solar core.

Title: Mean absolute strength of the solar magnetic field in 1968 2006
Authors: Kotov, V. A.
Bibcode: 2008ARep...52..419K
Altcode: 2008AZh....85..471K
  Measurements of the mean magnetic field of the Sun as a star (the
  line-of-sight component of the magnetic field of the visible hemisphere
  for a given day) carried out at six observatories are used to compile
  a catalog of the mean magnetic field for 1968 2006 (containing about
  18 000 daily values). The cataloged data are compared with direct
  daily measurements of the absolute line-of-sight field made at the
  Kitt Peak Observatory in 2003 2006 (original data with a resolution
  of 1″ averaged over the solar disk). The true absolute mean field
  strength averaged over the visible solar hemisphere is determined for
  1968 2006 to be B <SUB>0</SUB> = 7.7 ± 0.2 G. This figure exceeds
  previous estimates by almost a factor of four. B <SUB>0</SUB> exhibits
  no appreciable slow trend over the entire 39-year interval, but varies
  substantially with the cycle. The period of this variation is 10.5
  ± 0.7 yr, and its harmonic amplitude is 1.7 G. The magnetic flux of
  spots and active regions makes B <SUB>0</SUB> almost twice the field
  strength in the “normal” photosphere at the solar minimum, i.e.,
  for the “quiet” Sun.

Title: The sun, the cosmic vibration, and the nucleus of the
    galaxy 4151
Authors: Kotov, V. A.; Lyuty, L. M.
Bibcode: 2007BCrAO.103...69K
Altcode:
  Numerous U and V magnitude measurements were performed for the nucleus
  of the Seyfert galaxy NGC 4151 at the Crimean Laboratory of the SAI
  (Moscow University) in 1994-2005. Adding them to the previous data for
  1968-1997 has led to a substantial increase in the confidence level of
  the light variations in NGC 4151 with a stable period of P<SUB>G</SUB>
  = 160.0108(7) min and a mean amplitude of 0.007 U mag (in the "active"
  state of the nucleus). The period of NGC 4151 agrees well with the
  period of 160.0101(15) min found previously in the oscillations of the
  Sun. It is treated as the period of a "coherent cosmic oscillation"
  independent of redshift z or as the period of "free cosmic vibrations"
  of the hydrogen atom, the main element of the Universe. The period and
  initial phase of the P<SUB>G</SUB> oscillation have been constant for
  38 years of NGC 4151 observations. The new astrophysical phenomenon
  appears to be closely related to the quantum nonlocality of photons
  and is of particular interest in physics and cosmology.

Title: There are ten, not eight planets
Authors: Kotov, V. A.
Bibcode: 2007BCrAO.103...75K
Altcode:
  In 1946, E. Sevin postulated the global vibrations of the Sun with
  a period P<SUB>0</SUB> = 1/9 day and a "wavelength" L<SUB>0</SUB>
  = c × P<SUB>0</SUB> = 19.24 AU and predicted the tenth planet at
  a mean distance of 4.0 × L<SUB>0</SUB> ≈ 77.0 AU from the Sun (c
  is the speed of light). The global vibrations of the Sun, precisely
  with the period of 1/9 day, were actually detected in 1974. Recently,
  the largest Kuiper Bell object 2003 UB<SUB>313</SUB>, or Eris, with
  an orbital semimajor axis ≈ 3.5 × L<SUB>0</SUB> ≈ 67.5 AU was
  discovered. We adduce arguments for the status of Eris as our tenth
  planet: (i) the object is larger and farther from the Sun than Pluto
  and (ii) the semimajor axis of Eris agrees well with the sequence of
  planetary distances that follows from the resonance spectrum of the
  Solar system dimensions (with the scale L<SUB>0</SUB> and for all 11
  orbits, including those of Pluto, Eris, and the asteroid belt). We point
  to a mistake of the Prague (2006) IAU Assembly, which excluded Pluto
  from the family of planets by introducing a new, highly controversial
  class of objects—"dwarf planets."

Title: On the Near-One-Year Variation of the Sun's Mean Magnetic Field
Authors: Kotov, V. A.
Bibcode: 2006SoPh..239..461K
Altcode: 2006SoPh..tmp...70K
  The mean magnetic field (MMF) of the Sun-as-a-star was measured over the
  last 38 years by six observatories (about 17 000 MMF daily records, 1968
  - 2005). The MMF power spectrum reveals the presence of an enigmatic
  1.029(7) year periodicity whose origin requires explanation. We show
  that this quasi-annual variation is not produced by modulation of the
  MMF signal due to the annual change of the Earth's helio-latitude
  (one-year change of visibility of the Sun's polar regions) as
  commonly accepted. The nature of this new solar phenomenon is open
  for discussion.

Title: Pulsations of the sun: 30 years of measurements
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 2004KFNT...20..408K
Altcode:
  Regular measurements of oscillations of the Sun-as-a-star's photosphere
  have been performed at the Crimean Astrophysical Observatory since
  1974. In this experiment, a Babcock solar magnetograph detects Doppler
  effect difference between the central part and the limb part of the
  solar disk (using the Fraunhofer absorption line Fe I λ 512.4 nm). Over
  last 30 years the measurements were made during 1807 days (in aggregate
  more than 11 thousand hours). The most significant peak of the power
  spectrum of the line-of-sight velocity variations corresponds to the
  period P = 159.9655±0.0005 min. The period is in good agreement,
  within the error limit, with the Stanford value 159.9663±0.0008
  min, inferred before from the independent 1977-1994 measurements,
  which supports strongly solar origin of the period. This oscillation
  has nearly constant initial phase over the total 30-year interval and
  reveals substantially non-harmonic mean profiles of both, velocity and
  radius, perturbations. The true physical nature of the P phenomenon
  and the source of its excitation are unknown. It is supposed that the
  periodic oscillation of the Sun's photosphere is caused by superfast
  rotation of the central solar core.

Title: On rotation of Uranus and Neptune
Authors: Kotov, V. A.
Bibcode: 2004KFNT...20..142K
Altcode:
  The "resonance-spectra" of the revolution frequencies of massive
  satellites are computed in order to determine the rotation periods of
  gravitating masses of the giant planets. Based upon the tidal theory,
  it is supposed that the best common multiple of the satellite sidereal
  frequencies should be close to the rotation frequency of the central
  planet. A new "dynamical" period of Uranus, 16.14± 0.20 h (95% C.L.),
  coincides well, within the error limits, with the period 16.16± 0.33
  h determined earlier by spectroscopic technique. The most probable
  Neptune's period, 13.43± 0.16 h (99%), agrees with its dynamical
  oblateness. It is shown that the frequencies of all six fast-rotating
  planets and major asteroids occur to be in near-resonance with the
  frequency ν<SUB>0</SUB> = 103±2 μHz. The nature of the mysterious
  ν<SUB>0</SUB> -resonance in the solar system is unknown.

Title: Solar pulsation 1974-2003: the evidence for a fast rotating
    core
Authors: Kotov, V. A.
Bibcode: 2004IAUS..223..115K
Altcode: 2005IAUS..223..115K
  The measurements of the Doppler effect of the photosphere showed
  the presence of the persistent periodicity 159.9655(5) min. It is
  interpreted as by-product of the fast-rotating central solar core.

Title: On stability of rotation of the mean magnetic field of the Sun
Authors: Haneychuk, V. I.; Kotov, V. A.; Tsap, T. T.
Bibcode: 2003A&A...403.1115H
Altcode:
  New data on the mean magnetic field of the Sun (MMFS) as a star measured
  at the Crimean Astrophysical Observatory in 1998-2001 are presented. The
  34-year time series of the MMFS using similar data from three other
  observatories (1968-2001, with the total number of daily MMFS values N =
  12 428), is considered. It is found that (a) the primary synodic period
  of the equatorial rotation of solar magnetic field, P<SUB>sun</SUB> =
  26.929 +/- 0.015 days, did not vary over the last 34 years, but (b)
  the average intensity H<SUB>0</SUB> of the photospheric large-scale
  fields, by modulus, decreased by about 4.5% (with a confidence level
  of about 80%). The conclusion is made that the longer, 90-year,
  cycle might be responsible for this potential gradual decrease of
  H<SUB>0</SUB>. The average curve of MMFS variation as plotted with
  the primary rotational period P<SUB>sun</SUB> demonstrates an obvious
  N-S asymmetry of polarities, perhaps associated with the quadrupole
  component and ``magnetic disequilibrium'' of the Sun as a whole.

Title: Daily measurements of the mean magnetic field of the Sun,
1968-2001: Anomalous distribution?
Authors: Kotov, V. A.
Bibcode: 2003A&A...402.1145K
Altcode:
  The mean magnetic field (MMF) of the Sun was measured in 1968-2001 by
  four Babcock magnetographs: of the Crimean Astrophysical Observatory,
  CrAO, of the Mount Wilson Observatory, MWO, of the Wilcox Solar
  Observatory, WSO, and of the Sayan Solar Observatory, SSO (in all
  nearly 13 thousand daily records). The MMF strengths recorded by these
  instruments on the same day, often deviate substantially from each
  other; this can hardly be explained by purely instrumental/solar causes
  alone. It is pointed out that (a) each magnetograph represents a linear
  electro-optical device detecting diminutive, { ~ } 10<SUP>-5</SUP>
  - 10<SUP>-4</SUP>, Zeeman circular polarization of a solar spectral
  line, with (b) no essential nonliner effects are expected, and (c)
  the observed MMF daily values must be normally distributed around
  a zero mean. The actual MMF distribution appears to be quite normal
  for records of the CrAO and SSO. Those of the MWO and WSO, however,
  deviate remarkably from the normal. The exact physical nature of this
  abnormity is unknown. It is suggested that the true cause might be
  connected with (a) the use of an image-slicer (at MWO and WSO), (b)
  entanglement of photons, (c) the statistical origin of light itself
  (due to the principle of uncertainty: ``the instrument inevitably
  influences the output''), and (d) some instrumental/solar causes of
  poorly known origin and action.

Title: Towards Calibration of the Mean Magnetic Field of the sun
Authors: Kotov, V. A.; Kotov, S. V.; Setyaev, V. V.
Bibcode: 2002SoPh..209..233K
Altcode:
  The 1968-2000 data on the mean magnetic field (MMF, longitudinal
  component) of the Sun are analysed to study long-time trends of
  the Sun's magnetic field and to check MMF calibration. It is found
  that, within the error limits, the mean intensity of photospheric
  magnetic field (the MMF strength, |H|), did not change over the
  last 33 years. It clearly shows, however, the presence of an 11-year
  periodicity caused by the solar activity cycle. Time variations of |H|
  correlate well with those of the radial component, |B<SUB>r</SUB>|,
  of the interplanetary magnetic field (IMF). This correlation (r=0.69)
  appears to be significantly higher than that between |B<SUB>r</SUB>|
  and the results of a potential source-surface extrapolation, to the
  Earth's orbit, of synoptic magnetic charts of the photosphere (using
  the so-called `saturation' factor δ<SUP>−1</SUP> for magnetograph
  measurements performed in the line Fe i λ525.0 nm; Wang and Sheeley,
  1995). It seems therefore that the true source surface of IMF is the
  `quiet' photosphere - background fields and coronal holes, like those
  for MMF. The average `effective' magnetic strength of the photospheric
  field is determined to be about 1.9 G. It is also shown that there
  is an approximate linear relation between |B<SUB>r</SUB>| and MMF
  intensity |H| (in gauss)

Title: On the measurements of the magnetic disbalance of the Sun
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 2002KFNT...18..205K
Altcode:
  The 1968-2000 time sequence of the mean magnetic field of the Sun as a
  star is analysed (MMF, more than 12 thousands of daily measurements). It
  is shown that nominally -- on the basis of the total MMF measurements
  set -- the southern polarity of the magnetic field predominates on the
  Sun, with the average value -1.9± 1.1 μ T (the magnetic asymmetry
  is significant at about 91%; however, its instrumental origin cannot
  be completely excluded). The MMF changes with the 22-year cycle, so
  that its predominant polarity tends to coincide with that of the Sun's
  northern pole; the mean amplitude of this variation is equal to 6 μ
  T. It is concluded that the northern pole polarity tends to "determine"
  the dominant polarity of solar background fields for the most area of
  the photosphere (at heliolatitudes higher than -50<SUP>0</SUP>).

Title: Sources of the Global Magnetic Field of the Sun
Authors: Kotov, V. A.; Setyaeva, I. V.
Bibcode: 2002ARep...46..246K
Altcode:
  Data on the global magnetic field (GMF) of the Sun as a star for
  1968 1999 are used to determine the correlation of the GMF with the
  radial component of the interplanetary magnetic field (IMF) |B r|;
  all data were averaged over a half year. The time variations in the
  GMF |H| are better correlated with variations in |B r|; than the
  results of extrapolating the field from the “source surface” to
  the Earth’s orbit in a potential model based on magnetic synoptic
  maps of the photosphere. Possible origins for the higher correlation
  between the GMF and IMF are discussed. For both the GMF and IMF, the
  source surface actually corresponds to the quiet photosphere—i.e.,
  background fields and coronal holes—rather than to a spherical surface
  artificially placed ≈2.5 R ⊙ from the center of the Sun, as assumed
  in potential models (R ⊙ is the solar radius). The mean effective
  strength of the photospheric field is about 1.9 G. There is a nearly
  linear dependence between |H| and |B r|. The strong correlation between
  variations in |H| and |B r| casts doubt on the validity of correcting
  solar magnetic fields using the so-called “saturation” factor δ-1
  (for magnetograph measurements in the λ 525.0 nm FeI line).

Title: The active core of Seyfert galaxy NGC 4151 and the true origin
    of the 160-minute oscillation.
Authors: Kotov, V. A.; Khaneichuk, V. I.; Merkulova, N. I.; Metik,
   L. P.; Lyutyi, V. M.
Bibcode: 2002BCrAO..98...32K
Altcode:
  No abstract at ADS

Title: Anomalous magnetic field of the sun at the beginning of
    cycle 23
Authors: Kotova, I. V.; Kotov, S. V.; Kotov, V. A.
Bibcode: 2001A&AT...20..505K
Altcode:
  Measurements of the mean magnetic field (MMF) of the Sun from
  1968-1999 showed that (1) the Sun's magnetic field has a predominance
  of S-polarity, (2) it changes with periods 1.04, 1.60 and 23 yr, (3)
  the yearly-mean index of MMF energy reached the peak value in 1991,
  and after that (4) a significant decrease of MMF was observed. It is
  supposed that (a) the magnetic asymmetry of the Sun is a fundamental
  property of solar magnetism, (b) there are near-resonances between
  the MMF and orbital motions of Mercury, Venus and Earth which arose
  at early stages of formation of the Solar system, and (c) cycle 23
  will display an anomalously low magnetic and sunspot activity.

Title: On the Sun's magnetic field prior to maximum of the cycle 23
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 2001IzKry..97...60K
Altcode:
  The large number of measurements of the mean magnetic field (MMF) of
  the Sun were made in the CrAO in 1999. These data are analysed together
  with the like measurements performed at four solar observatories in
  1968 - 1999. It is shown that (1) during total 32-year interval the
  predominance of longitudinal magnetic field of southern polarity was
  observed on the Sun with the mean value of -0.009±0.005 Gs, (2) in
  1999, MMF exhibited 4-sector structure which is more characteristic
  of epochs near minima of solar activity, (3) the standard deviation
  of MMF in 1999 equals to 0.48 Gs was significantly lower than that
  usually observed before solar activity maximum (≍0.82 Gs).

Title: On rotation of Jupiter and Saturn
Authors: Kotova, I. V.; Kotov, V. A.
Bibcode: 2001KFNT...17..157K
Altcode:
  The method based on analysis of mean motion of massive satellites is
  proposed to deduce rotation periods of giant planets. A computation of
  the so-called "resonance-spectrum" is applied for analysis of satellite
  frequencies. It is found that the Saturn's "dynamical" period is equal
  to 10.76± 0.15(h) . It agrees fairly well with the value 10.66(h)
  determined earlier by the Voyager-1 spacecraft (reflecting rotation of
  magnetic field of the planet), and thus gives a good check-up of the
  method. But the new period of Jupiter, 10.69±0.15(h) , significantly
  differs from the commonly accepted value ≈ 9.9(h) , determined also
  by the magnetic field rotation, or from radio-observations. It is
  concluded that periods of giant planets determined by variations of
  magnetic field, can not necessarily reflect rotation rate of the main
  gravitating body of a planet. The cause might be differential rotation
  of magnetosphere and magnetic field of a planet - the phenomenon
  analogous to differential rotation of magnetic field of the Sun.

Title: Does the Solar Magnetic Field Increase?
Authors: Kotov, V. A.; Kotova, I. V.
Bibcode: 2001AstL...27..260K
Altcode:
  We consider measurements of the general magnetic field (GMF) of the Sun
  as a star at four world observatories from 1968 until 1999. We show
  that, within the error limits, the mean strength of the photospheric
  magnetic field H (of its longitudinal component, in magnitude) has
  not changed over the last 32 years. This is in conflict with the
  recent conclusion by Lockwood et al. (1999) that the solar coronal
  magnetic field increased by 40% from 1964 until 1996 and has almost
  doubled in the last 100 years. The causes of discrepancies in the
  results are discussed. At the same time, the GMF exhibits a natural
  11-year variation associated with the solar cycle. The strength of the
  photospheric longitudinal magnetic field (in absolute value) averaged
  over 32 years is 0.46 G (at an rms GMF strength of 0.57 G). The mean
  GMF for all years of measurements had a south polarity: &lt;H&gt;
  = - 0.030 +/- 0.018 G. The difference from zero is statistically
  significant at 1.7 sigma (90%) and may be directly related to the
  outstanding problem of the solar magnetic "monopole".

Title: Two states of the nucleus of the NGC 4151 Galaxy quiet
    and active
Authors: Kotov, V. A.; Lyuty, V. M.; Metlov, V. G.; Haneychuk, V. I.
Bibcode: 2000KFNT...16..558K
Altcode:
  The most interesting phenomenon in the studies of active galactic
  nuclei is their rapid variability over one night whose origin remains
  mysterious, and of special interest is the search for the presence of
  a periodic component. The oscillation with the period P<SUB>0</SUB>
  ≈ 160.010 min was found earlier in the emission of the nucleus of
  the Seyfert galaxy NGC 4151, but its authenticity is often doubted. The
  reasons for the scepticism are a small amplitude of the signal and the
  fact that the oscillation is absent during some nights. In 1985-1996 the
  observers of the P. K. Sternberg State Astronomical Institute and the
  Crimean Astrophysical Observatory carried out long series of photometric
  observations of NGC 4151 (in all, 39 and 51 nights in the U and V bands,
  respectively). Less than a half of the nights a significant variability
  over a night which exceeded 0.03-mag threshold (it was treated with no
  relation to any a priori periodicity). But the most important is that
  the P<SUB>0</SUB>-oscillation was clearly seen exactly during those
  "active" nights; other, "quiet", nights did not reveal any noticeable
  periodic signal. The mean harmonic amplitude of the P<SUB>0</SUB>
  -oscillation during the active state of the NGC 4151 nucleus is found
  to be about 0.009<SUP>m</SUP> (U-band), while it is not larger than
  0.0008<SUP>m</SUP> in the same band during the quiet state. The nature
  of such a strange modulation is unknown. The arguments are given in
  favour of a cosmological origin of the P<SUB>0</SUB>-oscillation.

Title: Solar oscillations in 1999
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 2000BCrAO..96..166K
Altcode:
  No abstract at ADS

Title: Oscillations of the sun with a period of 159.966 minutes in
    the Crimean 25-year observations
Authors: Kotov, V. A.; Khaneychuk, V. I.; Tsap, T. T.
Bibcode: 2000KFNT...16...49K
Altcode:
  Measurements of low-degree oscillations of the Sun were carried out
  at the Crimean Astrophysical Observatory during 25 years (1974-1998;
  in all 1530 days, about 9733 hours). These data showed that within
  the frequency range near the 9th daily harmonic the most significant
  oscillation corresponds to the period P<SUB>1</SUB> = 159.9660±
  0.0010 min. It agrees well with the main periodicity P<SUB>St</SUB> =
  159.9663±0.0014 min found earlier in the similar Doppler measurements
  of the solar photosphere performed at the Stanford University in
  1977-1994. The initial phase of the P<SUB>1</SUB> oscillation is
  found to be remarkably stable over the entire 25-year interval. This
  phenomenon cannot be ascribed to some terrestrial cause or to an
  artifact of the data reduction procedure. It presents a challenging
  problem for the physics of the Sun and models of its interior structure.

Title: New measurements of the mean magnetic field of the Sun and
    its rotation
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 1999ARep...43..185K
Altcode:
  A list of 152 new measurements of the mean magnetic field (MMF) of
  the Sun as a star obtained at the Crimean Astrophysical Observatory
  (CAO) in 1991-1997 are presented. They increase the total number of
  CAO MMF measurements to N = 1549 (since 1968). This time series is
  studied together with similar data from the Mount Wilson Observatory
  (1970-1982, N = 2457). A (synodic) period P_R = 26.95 +/- 0.06 days
  dominates in the power spectrum of the merged data for 1968-1997,
  revealing remarkable phase coherence over 30 years. This stability of
  the rotation of the "magnetic" Sun independent of the 11-year cycle
  is difficult to explain in the framework of current theories for the
  generation of the global solar magnetic field that gives rise to the
  solar cycle. There are two other periods in the solar MMF (~161 days
  and 1.0 year), whose origin is not yet clear.

Title: Is the 160-minute mode of oscillation of the sun returning?
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.
Bibcode: 1999BCrAO..95....1K
Altcode:
  No abstract at ADS

Title: The mean magnetic field of the Sun and the Sun-Mercury
    resonance.
Authors: Kotov, V. A.; Tsap, T. T.
Bibcode: 1999KPCB...15..313K
Altcode:
  More than 11000 measurements of the mean magnetic field of the Sun as
  a star (MMFS) were made at four observatories: Crimea, Mount Wilson,
  Sayan, and Stanford. The main period of rotation of the solar magnetic
  field (26.92±0.03<SUP>d</SUP>) which dominates these data reveals
  a surprising phase stability. Such stability is incompatible with
  the current phenomenological model of the solar cycle, which assumes
  a polarity reversal in the dipole field every 11 years. The authors
  ascribe this strict 27-day MMFS periodicity to the toroidal magnetic
  field of the Sun which is concentrated under the convection zone. Of
  particular interest also is the 7:2 resonance between the MMFS rotation
  and the orbital motion of Mercury; this resonance might have arisen
  in the distant past when the protoplanetary nebula existed.

Title: Observations of low-degree solar global oscillations at the
    Crimean Astrophysical Observatory.
Authors: Tsap, T. T.; Haneychuk, V. I.; Kotov, V. A.
Bibcode: 1998KFNT...14..520T
Altcode: 1998KNFT...14..520T
  Observations of low-degree p-modes obtained at the Crimean Astrophysical
  Observatory are presented. The observed frequencies are found to
  agree satisfactorily with the calculated frequencies of the standard
  solar model.

Title: Magnetic Field of the Sun as a Star: The Mount Wilson
    Observatory Catalog 1970-1982
Authors: Kotov, V. A.; Scherrer, P. H.; Howard, R. F.; Haneychuk, V. I.
Bibcode: 1998ApJS..116..103K
Altcode:
  Measurements of the mean magnetic field of the Sun (MMFS) seen as
  a star were regularly conducted at the Mount Wilson Observatory
  from 1970 October through 1982 December. A listing is presented of
  all these data (2457 daily values) suitable for comparison with
  similar data of other observatories and for studies of magnetic
  variability and rotation of the Sun. The scatter-plot diagrams and
  power spectra of the Mount Wilson data and also of the total data
  1968-1991 (collected from three observatories: Crimean Astrophysical
  Observatory, Mount Wilson Observatory, and Wilcox Solar Observatory)
  are also presented. Time variations of the MMFS connected with solar
  rotation at periods ~27-28 days and also an enigmatic 1 yr variation
  are briefly discussed. <P />The power spectrum of the 24 yr data set
  shows that the most significant and phase-coherent synodic periods of
  the MMFS variations are 26.92 +/- 0.02 and 27.13 +/- 0.02 days (both
  are thought to be associated with rotation of the large-scale surface
  magnetic field near equator of the Sun) and 28.13 +/- 0.02 days. It
  is suggested that the latter period reflects ``rigid'' rotation of
  the global magnetic field concentrated under the bottom of the solar
  convection zone. The arguments are given in favor of reality and high
  confidence level of major periodicities exhibited by MMFS variations.

Title: Five Thousand Galactic Binaries as a Detector of Gravitational
    Waves
Authors: Kotov, V. A.; Kotov, S. V.
Bibcode: 1998A&AT...15..185K
Altcode:
  No abstract at ADS

Title: A common resonance of delta SCT stars and ellipsoidal binaries.
Authors: Kotov, S. V.; Kotov, V. A.
Bibcode: 1998KFNT...14..543K
Altcode: 1998KFNT...14f.543K
  No abstract at ADS

Title: New data on the P<SUB>0</SUB>-oscillation of the nucleus of
    the Seyfert galaxy NGC 4151.
Authors: Kotov, V. A.; Lyutyj, V. M.; Merkulova, N. I.; Metik, L. P.;
   Metlov, V. G.; Khanejchuk, V. I.
Bibcode: 1998KFNT...14...67K
Altcode: 1998KNFT...14...67K; 1998KFNT...14a..67K
  The presence of the periodicity P<SUB>0</SUB> = 160.0101±0.0001
  min in the brightness variations of active galactic nuclei is often
  subjected to criticism by some astrophysicists. With the aim to
  check the P<SUB>0</SUB>-effect, an extensive series of photometric
  observations of the Seyfert galaxy NGC 4151 was obtained in 1987 -
  1994 using two Crimean reflectors. These new data confirmed the
  presence of the P<SUB>0</SUB>-periodicity with the stable (over 26
  yr) initial phase and the mean harmonic amplitude ≍7 mmag (in the
  V filter). This conclusion is supported by analysis of the X-ray data
  (1975 - 1991) obtained by satellites Ariel-5, EXOSAT and Ginga. Since
  just the same period has been detected earlier in the power spectrum
  of global oscillations of the Sun, the conclusion is drawn about its
  cosmological origin.

Title: 160-minute oscillations of active galactic nuclei: new data
    for 3C 273 and NGC 4151
Authors: Kotov, V. A.; Merkulova, N. I.; Metik, L. P.; Khaneichuk,
   V. I.; Lyutyi, V. M.
Bibcode: 1998BCrAO..94...83K
Altcode:
  No abstract at ADS

Title: 25 years of investigating the magnetic field of the sun as
    a star
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.; Demidov, M. L.;
   Grigor'ev, V. M.
Bibcode: 1998BCrAO..94...79K
Altcode:
  No abstract at ADS

Title: Observations of low-degree p-modes at the Crimean Astrophysical
    Observatory.
Authors: Tsap, T. T.; Khaneichuk, V. I.; Kotov, V. A.
Bibcode: 1998BCrAO..94..129T
Altcode:
  The results of observations of solar acoustic modes of low degree l
  during the period 1978 - 1992 are presented. The observed frequencies
  are compared with those calculated for the standard solar model.

Title: New data on the P<SUB>0</SUB>-oscillation of the nucleus of
    the Seyfert galaxy NGC 4151.
Authors: Kotov, V. A.; Lyutyj, V. M.; Merkulova, N. I.; Metik, L. P.;
   Metlov, V. G.; Khanejchuk, V. I.
Bibcode: 1998KPCB...14...52K
Altcode:
  The periodicity P<SUB>0</SUB> = 160.0101±0.0001 min in brightness
  variations of active galactic nuclei is questioned by some
  astrophysicists. Extensive photometric observations of the Seyfert
  galaxy NGC 4151 were made with two reflectors at the Crimean Observatory
  in an effort to verify the existence of the P<SUB>0</SUB>-effect. The
  new data confirmed the presence of the P<SUB>0</SUB>-periodicity
  with a phase stable over 26 years and a mean harmonic amplitude of
  0.007<SUP>m</SUP> in the V band. This result is also substantiated
  by an analysis of the X-ray observations from the Ariel-5, EXOSAT,
  and Ginga satellites (1975 - 1991). Since the same period was found
  in the power spectrum of global oscillations of the Sun, the authors
  infer that it is of cosmological origin.

Title: Solar oscillations according to CrAO 1974 - 1994 data.
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.
Bibcode: 1998BCrAO..94..132K
Altcode:
  Observations of solar oscillations as a whole were carried out at the
  Crimean Astrophysical Observatory (CrAO) by the differential method in
  1974 - 1994. The first nine years showed that the Sun oscillated with
  period P0 = 160<SUP>m</SUP>0101±0<SUP>m</SUP>0016. Later, however,
  a new value of the fundamental period was established, P<SUB>0</SUB>
  = 159<SUP>m</SUP>9662±0<SUP>m</SUP>0007.

Title: Consistency of measurements of the magnetic field of the sun
    as a star and its annual variation
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.; Demidov, M. L.
Bibcode: 1998BCrAO..94...71K
Altcode:
  No abstract at ADS

Title: Upper limit for the amplitude of the solar 160-minute
    oscillation in 1982 - 1989.
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.
Bibcode: 1998BCrAO..94..102K
Altcode:
  Crimean observations of global solar oscillations show that in
  1982 - 1989 the known 160-min oscillation was on average almost
  absent. Arguments are given in behalf that after the "fading" interval,
  the solar oscillation with a period of 160<SUP>m</SUP>010 can evidently
  intensify in the next years to come.

Title: Evidence for a cosmological oscillation of the nucleus of
    the Seyfert galaxy NGC 4151
Authors: Kotov, V. A.; Lyuty, V. M.; Haneychuk, V. I.; Merkulova,
   N. I.; Metik, L. P.; Metlov, V. G.
Bibcode: 1998A&AT...16...15K
Altcode:
  Long-term observations of global oscillations of the Sun revealed the
  existence of the phasecoherent periodicity P0 = 160.0101 ± 0.0001
  min seen in the Doppler shift of a photospheric spectral line. The
  true nature of the phenomenon is yet unknown. But the most intriguing
  aspect seems to be the recent discovery of the same periodicity in
  luminosity variations of several AGNs which makes the puzzle of the
  "ubiquitous" P0-oscillation much more mysterious. The present analysis
  of all available data on the rapid variability of the nucleus of NGC
  4151 fully confirms the AGN P0-oscillation (with a mean amplitude
  0.01 mag). It is argued that this oscillation must have a cosmological
  origin - due to, e.g., its independence of the AGN redshift. In terms
  of general relativity the P0-oscillation is treated as a characteristic
  time scale of metric fluctuations of the Universe. The conclusion is
  made that this new astrophysical phenomenon severely contradicts today's
  cosmological model of the Universe based on the Big Bang paradigm.

Title: Observations of solar global low-degree oscillations at the
    Crimean Astrophysical Observatory.
Authors: Tsap, T. T.; Khanejchuk, V. I.; Kotov, V. A.
Bibcode: 1998KPCB...14..400T
Altcode:
  Presents some results of the observations of the low-degree p-modes
  made at the Crimean Astrophysical Observatory. The observed frequencies
  are found to agree satisfactorily with the frequencies calculated for
  the standard solar model.

Title: Investigation of the solar pulsation at the CrAO.
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 1998IBUAA..12...19K
Altcode:
  No abstract at ADS

Title: A resonance common to the δ Scuti stars and ellipsoidal
    binaries.
Authors: Kotov, S. V.; Kotov, V. A.
Bibcode: 1998KPCB...14..419K
Altcode:
  Is there a characteristic frequency common to a large number of variable
  stars? Statistical analysis of 613 pulsation frequencies of 358 δ Sct
  stars reveals the best resonance (the best commensurability) frequency -
  ν<SUB>p</SUB> = 104.4±0.7 μHz. The same frequency happens to be the
  best resonant rotation frequency for 43 ellipsoidal binary systems
  as well ν<SUB>R</SUB> = 104.6±0.6 μHz (with a priori confidence
  levels of 3.8σ and 3.4σ for both resonances, respectively). It
  is intriguing that both these frequencies coincide, to within the
  errors, with the frequency ν<SUB>sun</SUB> = 104.1601±0.0001 μHz
  of the global oscillations of the Sun discovered about two decades ago
  (the oscillation period P<SUB>0</SUB> = 160 min), the nature of these
  oscillations still remains unknown. The observed P<SUB>0</SUB>-resonance
  can hardly be reasonably explained within the scope of contemporary
  astrophysical theories.

Title: The Splitting Or Disappearance of the Solar 160-Min Mode?
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.; Hoeksema, J. T.
Bibcode: 1997SoPh..176...45K
Altcode:
  The `CrAO-WSO'-network experiment was designed for detection of
  low-degree oscillations of the Sun representing either its normal
  g -modes or those driven by, e.g., rapid (hypothetical) rotation of
  the central solar core. The Doppler-shift measurements were made in
  1974-1995 at both sites during about 13600 hr, in all. Taking into
  account the upper limit (≈0.08 m s<SUP>-1</SUP>) for amplitudes
  of potential g-modes, attention is paid to the Sun's behaviour at
  frequencies near the 9th daily harmonic (period P ≈160.

Title: The Long-Term Periodic Oscillation of the NGC 4151 Nucleus
Authors: Kotov, V. A.; Lyuty, V. M.; Haneychuk, V. I.; Merkulova,
   N. I.; Metik, L. P.; Metlov, V. G.
Bibcode: 1997ApJ...488..195K
Altcode:
  The hypothesis that the luminosity of the nucleus of the Seyfert
  1 galaxy NGC 4151 varies with a period of P<SUB>0</SUB> ~ 160.0101
  minutes is revised. In 1987-1994 a series of photometric observations
  of the NGC 4151 has been carried out in the U and V filters at several
  instruments. In the total sample of 27 nights, the U data of 15 nights
  showed an appreciable intranight variability of the AGN flux. Being
  detrended and folded with the a priori period P<SUB>0</SUB>, those data
  exhibited significant P<SUB>0</SUB> signal coinciding in phase with
  that found in previous studies. Nearly the same result is obtained
  for 39 nights in the V-filter. The average harmonic amplitudes of
  the P<SUB>0</SUB> oscillation (for the total interval 1968-1994) are
  found to be ~7 and ~2 mmag in the U and V filters, respectively. <P
  />The power spectrum was computed for the total data series 1968-1994
  (in all 2771 measurements including X-ray data from Ariel 5, EXOSAT,
  and Ginga satellites). It reveals a prominent peak corresponding
  to a period of 160.0104 +/- 0.0005 minutes (with the lower level
  of confidence 3.6 σ). The latter fairly well coincides with the
  P<SUB>0</SUB> period discovered much earlier in the power spectrum of
  global oscillations of the Sun. This analysis thus strongly supports
  a cosmological interpretation of the ``ubiquitous'' oscillation with
  the P<SUB>0</SUB> period.

Title: The frequency 104μHz in the orbital motion of close binary
    stars.
Authors: Kotov, V. A.; Kotov, S. V.
Bibcode: 1997A&A...322..177K
Altcode:
  According to General Relativity, a stellar binary generates
  gravitational waves at a primary frequency twice the orbital one; these
  waves however have not yet been detected. If the Universe contains
  gravitational radiation at discrete frequency(ies) - particularly
  with the period of 160 minutes discovered in the 70-th in the Sun,
  corresponding resonances might be found in the distribution of orbital
  frequencies of binaries. With this in mind, we analyse all available
  data on orbital frequencies of close binaries of the Galaxy. In the
  frequency range 5 to 160μHz, we find one significant frequency
  ν_0_=~104.2μHz - at the 4σ confidence level -which modulates
  the distribution of about 5000 binaries with periods P&lt;5.5d. The
  corresponding ``resonant'' period, 160.0+/-0.5min, coincides with that
  of solar pulsation P_0_=160.0+/-0.5min. The question on its origin and
  also the hypothesis of a cosmological nature of the P_0_ oscillation
  are briefly discussed.

Title: On rotation of ellipsoidal binary systems.
Authors: Kotov, S. V.; Kotov, V. A.; Kuvshinov, V. M.; Nikulin, I. F.
Bibcode: 1997CRASB.324..659K
Altcode: 1997CR2...324..659K
  The origin of pulsation of the Sun with period P<SUB>0</SUB> ≍
  160 min is as yet unknown. Statistical treatment of data on the
  rotation of 43 ellipsoidal binary systems with P<SUB>orb</SUB> &lt;
  7 days showed that the most resonant frequency of these stars equals
  104.6±0.6 μHz. This agrees well with the frequency ν<SUB>0</SUB>
  = P<SUB>0</SUB><SUP>-1</SUP> = 104.1601±0.0001 μHz found earlier
  in global solar oscillations, and also in: (1) pulsation frequencies
  of δ Sct stars and (2) in rapid variability of AGNs. These findings
  thus strongly favour a cosmological interpretation of the "ubiquitous"
  160-min periodicity.

Title: The most resonant pulsation frequency of delta Scuti stars
Authors: Kotov, S. V., Jr.; Kotov, V. A.
Bibcode: 1997AN....318..121K
Altcode:
  Pulsation of the Sun with a period of P<SUB>0</SUB> ~ 160 min
  discovered about two decades ago, is still waiting explanation. In
  view of the hypothesis about its cosmological origin, and attempting
  to find signature of this \p\ periodicity among other (short--period
  variable) stars, the pulsation frequencies of \del stars are subjected
  to specific analysis. With a confidence level ~ 3.8sigma it is found
  that the frequency nu_ {0} be the most ``resonant'' one for the total
  sample of 318 pulsating stars of del type (the most commensurable, or
  ``synchronizing'', period for all these stars occurs to be 162 \pm 4
  min). We conjecture that a) the p \ oscillation might be connected with
  periodic fluctuations of gravity field (metrics), and b) the primary
  excitation mechanism of pulsations of del stars, reflected by this
  ``ubiquitous'' p \ resonance, must be attributed perhaps to superfast
  rotation of their inner cores (their rates tend to be in near--resonance
  with the ``universal'' \nu<SUB>0</SUB>$ frequency). The arguments are
  given favouring a cosmological nature of the \p\ oscillation.

Title: Modern Magnetooptics and Magnetooptical Materials: Studies
    in Condensed Matter
Authors: Zvezdin, A. K.; Kotov, V. A.
Bibcode: 1997mmmm.book.....Z
Altcode:
  No abstract at ADS

Title: The first results of solar observations made in the Crimean
    Astrophysical Observatory using a magneto-optical filter
Authors: Didkovskii, L. V.; Dolgushin, A. I.; Kotov, V. A.; Khaneychuk,
   V. I.; Tsap, T. T.; Rhodes, E. J.; Korzennik, S. G.; Johnson, N. M.;
   Rose, P. J.
Bibcode: 1996R&QE...39..916D
Altcode:
  The results of observations of Doppler velocities and solar magnetic
  fields using a magneto- optical filter (MOF) are presented. The
  MOF-based instrument was manufactured and supplied to the Crimean
  Astrophysical Observatory (CrAO) by the University of Southern
  California. It is one of three similar instruments designed to
  establish the helioseismology network „Mount Wilson —CrAO —
  AFiF” (Fesenkov Astrophysical Institute in Alma- Ata.) Apart from its
  main purpose — obtaining a long time series of the Doppler velocity
  measurements to study the internal solar structure and recording the
  magnetic fields for the ground- based support of the SOHO project —
  the instrument allows us to study different structural formations in
  the solar atmosphere in Na D1 and D2 spectral lines. This conclusion
  relies on the comparison between the magnetic field and beam velocity
  maps calculated using the filtergram pairs, which were recorded twice
  a minute by 512×512 video-camera (1024×1024 camera will be used in
  the future studies).

Title: A pulsar inside the Sun?
Authors: Kotov, V. A.
Bibcode: 1996R&QE...39..811K
Altcode:
  The Crimean observation of solar oscillations in 1974 1982 showed that
  the basic period of pulsation of the Sun hidden in its deep interior
  was equal to P <SUB>0</SUB>=160.0101±0.0001 min. More recently, the
  period was changed to the new value P <SUB>1</SUB>=159.9662±0.0006 min,
  which almost coincided with the annual sidelobe of the former period
  P <SUB>0</SUB>. The amplitude of the P<SUB>1</SUB> oscillation has
  increased considerably over 1994 1995. We substantiate the hypothesis
  that a) the change in the period was caused by the interaction of the
  P<SUB>0</SUB> oscillation with the rapid rotation of the solar core
  and that b) the latter has the form of a compact, highly magnetized
  object like a neutron star rotating with sidereal period P<SUB>1</SUB>.

Title: From solar seismology to restrictions on the standard cosmology
Authors: Kotov, V. A.; Kotov, S. V.
Bibcode: 1996R&QE...39..807K
Altcode:
  One and the same period, P <SUB>0</SUB>=160.0101±0.0001 min, was
  discovered in the global oscillation of the Sun and in the rapid
  variability of several active galactic nuclei (AGN). According to
  Kotov and Lyuty's hypothesis [1], the P <SUB>0</SUB> oscillation must
  have a cosmological nature, since the period is independent of the AGN
  redshift. The “universal” P<SUB>0</SUB> osculation can represent a
  fundamental scale of “cosmic time,” that is, a true cosmological
  invariant which does not depend on the source moving with respect to
  the observer. The phenomenon of the P<SUB>0</SUB> oscillation (the
  metrics of the Universe) brings the Big Bang paradigm into challenge.

Title: Oscillations of the Sun and AGN's: restrictions on the
    standard cosmology
Authors: Kotov, V. A.
Bibcode: 1996cosm.conf..389K
Altcode:
  No abstract at ADS

Title: The period P<SUB>0</SUB> in the power spectrum of active
    galactic nuclei.
Authors: Kotov, V. A.; Lyutyj, V. M.
Bibcode: 1996IzKry..93...79K
Altcode:
  The high resolution power spectrum of rapid variations of luminosities
  of four active galactic nuclei, NGC 3516, NGC 4151, BL Lac and PKS
  2155-304, was computed near 160-min period on the basis of optical
  and X-ray data 1968 - 1990. It is found that the maximal and only
  statistically significant peak, within the frequency range considered,
  corresponds to a period of 160.0102 (±6) min (with the confidence
  level of nearly 5σ). Within the error limits it coincides with the
  well-known period of global pulsation of the Sun, P<SUB>0</SUB> =
  160.0101 (±1) min, and thus strongly supports the hypothesis about
  a cosmological nature of the P<SUB>0</SUB>-oscillation.

Title: Period P<SUB>0</SUB> in the oscillation power spectrum of
    active galactic nuclei
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1996BCrAO..93...67K
Altcode:
  No abstract at ADS

Title: Periodic P<SUB>0</SUB> oscillations of the Sun and of ten
    active galactic nuclei. A possible cosmological explanation
Authors: Kotov, V. A.; Khaneychuk, V. I.; Lyuty, V. M.
Bibcode: 1996BCrAO..93...77K
Altcode:
  No abstract at ADS

Title: Oscillations of the Sun in 1974-1994
Authors: Kotov, V. A.
Bibcode: 1996MmSAI..67..973K
Altcode:
  No abstract at ADS

Title: Periodic P<SUB>0</SUB>-oscillations of the Sun and ten AGN's
    and possibility for cosmological explanation.
Authors: Kotov, V. A.; Lyutyj, V. M.; Chanejchuk, V. I.
Bibcode: 1996IzKry..93...90K
Altcode:
  The photometric data on rapid, intranight variability of ten
  AGN's are analysed with the aim to search for a phase-coherent
  periodicity. To the Crimean 1968 - 1991 observations the authors
  added all available (and suitable for analysis) world data including
  X-ray measurements made by satellites HEAO-1, Ariel-5, EXOSAT
  and Ginga (in total 4931 separate luminosity measurements for 10
  extragalactic objects). Statistical analysis shows the presence of
  the 160-min periodicity for each AGN. It fairly well coincides with
  the value P<SUB>0</SUB> = 160<SUP>m</SUP>0101±0<SUP>m</SUP>0001
  known as period of global oscillations of the Sun, and therefore
  gives more credit for a cosmological hypothesis about origin of the
  "universal" P<SUB>0</SUB>-oscillation. A possible explanation of
  the apparent independence of the observed frequency ν<SUB>0</SUB> =
  P<SUB>0</SUB><SUP>-1</SUP> on the AGN redshift is briefly discussed.

Title: Periodic P0-oscillations of the Sun and ten AGN'sa and
    possibility for cosmological explanation.
Authors: Kotov, V. A.; Lyuty, V. M.; Haneychuk, V. I.
Bibcode: 1996IzKAO..93...90K
Altcode:
  No abstract at ADS

Title: First Results of Solar Oscillations Made in Crimean
    Astrophysical Observatory Using Magneto-Optical Filter
Authors: Didkovsky, L. V.; Rhodes, E. J., Jr.; Dolgushin, A. I.;
   Haneychuk, V. I.; Johnson, N. M.; Korzennik, S. G.; Kotov, V. A.;
   Rose, P. J.; Tasp, T. T.
Bibcode: 1996RaF....39...11D
Altcode:
  No abstract at ADS

Title: From Solar Oscillations to Restrictions on the Standard
    Cosmology
Authors: Kotov, V. A.
Bibcode: 1995ESASP.376b.305K
Altcode: 1995help.confP.305K; 1995soho....2..305K
  No abstract at ADS

Title: A Superfast Rotation of the Central Solar Core?
Authors: Kotov, V. A.
Bibcode: 1995ESASP.376b.299K
Altcode: 1995help.confP.299K; 1995soho....2..299K
  No abstract at ADS

Title: General magnetic field of the Sun as a star
Authors: Kotov, V. A.
Bibcode: 1995BCrAO..91..102K
Altcode:
  No abstract at ADS

Title: A Cosmological Origin of the P_0 Oscillation of the Sun
Authors: Kotov, V. A.
Bibcode: 1995ASPC...76..220K
Altcode: 1995gong.conf..220K
  No abstract at ADS

Title: Observation of the Sun as a star: cosmological aspect.
Authors: Kotov, V. A.
Bibcode: 1995BRASP..59.1612K
Altcode:
  Measurements of the general magnetic field of the Sun in 1968 -
  1992 revealed a predominance of two synodic rotation periods, 28.96
  and 28.20 days. The first period is conditioned by the photosphere
  magnetic structure rotation, the second one possibly reflects a
  rigid-body rotation of the radiative zone. Of particular interest is
  the yearly variation, which cannot be explained by any terrestrial
  apparatus. It can be a consequence of the star rotation in an
  inertial space if its interior structure radically differs from the
  standard model. Observation of solar oscillations as a whole led to
  the discovery of 160-min pulsations. Later the same period was found
  in the brightness variations of galaxy's active nuclei, which shows
  evidence for a cosmological origin of the oscillations.

Title: Academician A. B. Severnyi and his contribution to modern
    astrophysics
Authors: Kotov, V. A.
Bibcode: 1995BCrAO..92....7K
Altcode:
  No abstract at ADS

Title: Universal occultations of the Sun and active galactic nuclei
    and an attempt of interpretation.
Authors: Kotov, V. A.; Larionov, M. G.; Lyuty, V. M.; Haneychuk, V. I.
Bibcode: 1995IzKry..92..126K
Altcode:
  No abstract at ADS

Title: On Possible Resonance Frequency (4.9 Hz) of Neutron Stars
Authors: Kotov, V. A.; Fomin, V. P.
Bibcode: 1995pns..book..267K
Altcode:
  No abstract at ADS

Title: The oscillations of the Sun and new evidence of rapid rotation
    of the central core
Authors: Kotov, V. A.; Khaneichuk, V. I.; Tsap, T. T.
Bibcode: 1995BCrAO..92...94K
Altcode:
  No abstract at ADS

Title: Summary of the Crimean 20-Year Observation of Solar Global
    Oscillations
Authors: Kotov, V. A.; Haneychuk, V. I.; Tsap, T. T.
Bibcode: 1995ASPC...76...82K
Altcode: 1995gong.conf...82K
  No abstract at ADS

Title: Universal oscillations of the Sun and active galactic nuclei
    and an attempt at interpretation
Authors: Kotov, V. A.; Larionov, M. G.; Lyutyi, V. M.; Khaneichuk,
   V. I.
Bibcode: 1995BCrAO..92..109K
Altcode:
  No abstract at ADS

Title: Rapid variability of active galactic nuclei : the 160min
    periodicity in NGC 3516, NGC 4151 and quasar 3C 273.
Authors: Kotov, V. A.; Haneychuck, V. I.; Lyuty, V. M.
Bibcode: 1994AN....315..333K
Altcode:
  The analysis of tall the available data between 1968 and 1991 on rapid
  variability of optical and X-ray luminosity of three Active Galactic
  Nuclei (AGNs), NGC 3516, NGC 4151 and 3C 273, shows the presence
  of small-amplitude (approximately 1%) but statistically confident
  (approximately = 5(sigma) periodicity of 160.0105 (+/- 6) min. Within
  the error limits it coincides with the period P<SUB>o</SUB> = 160.0101
  (+/-1) min of global oscillations of the Sun. An independence of
  the observed period on AGN red shift z favors the hypothesis about a
  cosmological origin of the 160min oscillation.

Title: Ground-Based Near-Infrared Observations of Global Solar
    Oscillations
Authors: Didkovsky, L. V.; Kotov, V. A.
Bibcode: 1994IAUS..154..277D
Altcode:
  No abstract at ADS

Title: On Sunspot and Facular Contrast Variations Near 2 MU M and
    4 MU M
Authors: Kotov, V. A.; Koutchmy, S.
Bibcode: 1994IAUS..154..265K
Altcode:
  No abstract at ADS

Title: The general magnetic field of the Sun as a star.
Authors: Kotov, V. A.
Bibcode: 1994IzKry..91..124K
Altcode:
  The author presents informations on measurements of the general magnetic
  field of the Sun as a star and its correlations with the interplanetary
  magnetic field. Results of an analysis of the magnetic asymmetry of
  the Sun are given. The rotation of the global magnetic field of the Sun
  and the interplanetary magnetic field is studied. Results of long-term
  observations of the 160-min oscillations of the general magnetic field
  of the Sun are discussed.

Title: A Puzzle of the 160-MINUTE Periodicity in the Sun Binaries
    Rr-Lyrae Stars and Active Galactic Nuclei - the Signatures of a
    Cosmological Origin
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1993ASPC...42..289K
Altcode: 1993gong.conf..289K
  No abstract at ADS

Title: The Search for 160-MINUTE Oscillations in the Stanford and
    Crimean Solar Velocity Observations - 1974-1991
Authors: Kotov, V. A.; Scherrer, P. H.; Hoeksema, J. T.; Haneychuk,
   V. I.; Tsap, T. T.
Bibcode: 1993ASPC...42..293K
Altcode: 1993gong.conf..293K
  No abstract at ADS

Title: Oscillations of the active galactic nuclei with the 160 minute
    period and antimatter hypothesis.
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1993IzKry..87..144K
Altcode:
  No abstract at ADS

Title: A Striking Similarity Between the Sun, Binaries and RR Lyrae
    stars in globular clusters
Authors: Kotov, Valery A.
Bibcode: 1993npsp.conf..160K
Altcode: 1993IAUCo.139..160K
  No abstract at ADS

Title: New evidences of the 160-minute oscillations in active
    galactic nuclei.
Authors: Kotov, V. A.; Lyuty, V. M.; Haneychuk, V. I.
Bibcode: 1993IzKry..88...47K
Altcode:
  No abstract at ADS

Title: New evidence of 160-minute oscillations in active galactic
    nuclei
Authors: Kotov, V. A.; Lyutyi, V. M.; Khaneichuk, V. I.
Bibcode: 1993BCrAO..88...40K
Altcode:
  No abstract at ADS

Title: Oscillations of active galactic nuclei with 160-minute period
    and the antimatter hypothesis
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1993BCrAO..87..132K
Altcode:
  No abstract at ADS

Title: Plans for MT.WILSON - Crimean Observatory High-Degree
    Helioseismology Network
Authors: Rhodes, E. J., Jr.; Cacciani, A.; Dappen, W.; Didkovsky,
   L. V.; Hill, F.; Korzennik, S. G.; Kosovichev, A. G.; Kotov, V. A.;
   Scherrer, P. H.
Bibcode: 1993ASPC...42..477R
Altcode: 1993gong.conf..477R
  No abstract at ADS

Title: On the Upper Limit for Detecting G-Mode Oscillations of the Sun
Authors: Scherrer, P. H.; Hoeksema, J. T.; Kotov, V. A.
Bibcode: 1993ASPC...42..281S
Altcode: 1993gong.conf..281S
  No abstract at ADS

Title: Pulsations of active galactic nuclei and problem of antimatter
    in the universe
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1992BCrAO..86..101K
Altcode:
  No abstract at ADS

Title: Universal oscillations of active galactic nuclei and anomalous
    distribution of the initial phases.
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1992IzKry..85...91K
Altcode:
  No abstract at ADS

Title: Short-period variations in the Sun's global magnetic field.
Authors: Demidov, M. L.; Kotov, V. A.; Grigor'ev, V. M.
Bibcode: 1992BCrAO..82..135D
Altcode:
  Measurements have been made on the Sun's general magnetic field in 1975
  - 1978 and in 1987 at the Crimean and Sayan observatories and at Mount
  Wilson; these have shown that there are more or less stable oscillations
  with periods of about 47, 60, 85, and 160 min with mean amplitudes of
  about 1 μT. The new Sayan observations of 1987 confirm the previous
  conclusion that there is long-time coherence in the oscillation with
  period 160.0101 min.

Title: Solar pulsations: effects due to the 22-year activity cycle?
Authors: Kotov, V. A.; Tsap, T. T.; Didkovskij, L. V.
Bibcode: 1992BCrAO..82..127K
Altcode:
  Regular measurements have been made on the differential Doppler
  velocity in the Crimea between 1974 and 1987 (in all, 902 days, 5612 hr
  of observation), which confirm the long-term phase-coherent pulsation
  with a period of 160.01 min. The new data also suggest that the 160-min
  pulsation may have a multiplet fine structure. In particular, there
  have been large changes in the amplitude and phase of the pulsation
  in the period 1983 - 1987, which may mean that after 1982 - 1983 one
  has observed the 160 min oscillations related to the second half of
  the 22-year magnetic activity cycle. This new and unexpected feature
  opens up scope for probing the solar interior, and also for researching
  the internal rotation and the 11 (22)-year solar cycle.

Title: On the 160-minute variability of NGC 4151: a rebuttal
Authors: Lyutyi, V. M.; Kotov, V. A.
Bibcode: 1992BCrAO..84...95L
Altcode:
  No abstract at ADS

Title: Study of the Sun's interior: pulsation of the Sun and
    22-year cycle
Authors: Kotov, V. A.; Kaneychuk, V. I.; Tsap, T. T.
Bibcode: 1992BCrAO..85....1K
Altcode:
  No abstract at ADS

Title: Question of the 160-minute variability of the NGC 4151 :
    the answer to opponents.
Authors: Lyuty, V. M.; Kotov, V. A.
Bibcode: 1992IzKry..84..104L
Altcode:
  No abstract at ADS

Title: Universal oscillations of active galactic nuclei and anomalous
    distribution of initial phases
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1992BCrAO..85...86K
Altcode:
  No abstract at ADS

Title: Pulsations of the active galactic nuclei and problem of the
    antimatter in the universe.
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1992IzKry..86..108K
Altcode:
  No abstract at ADS

Title: Fast periodic fluctuations of the Sun's general magnetic field
Authors: Kotov, V. A.; Demidov, M. L.; Grigor'ev, V. M.; Khaneichuk,
   V. I.; Tsap, T. T.
Bibcode: 1992BCrAO..84..149K
Altcode:
  No abstract at ADS

Title: 160-MINUTE Pulsation of the Sun - New Observational Results
Authors: Kotov, V. A.; Tsap, T. T.; Ganeichuk, V. I.
Bibcode: 1991SoPh..133...95K
Altcode:
  The 1974-1988 Crimean measurements of the solar line-of-sight velocity
  continue to show the presence of a statistically significant periodicity
  P<SUB>1</SUB> = 160.009 (±) min with an average harmonic amplitude
  of about 21 cm s<SUP>−1</SUP>. The period is supposed to be that
  of the global pulsation of the Sun but with a little-known physical
  mechanism of excitation.

Title: 160-minute oscillations of certain extragalactic objects
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1991BCrAO..83..197K
Altcode:
  No abstract at ADS

Title: The helioseismology experiment on the Phobos planetary
    mission. Preliminary results
Authors: Frohlich, C.; Bonnet, R. M.; Bruns, A. V.; Vial, J. C.;
   Delaboudiniere, J. P.; Domingo, V.; Kollath, Z.; Kotov, V. A.;
   Rachkovskii, D. N.; Wehrli, Ch.; Toulain, T.; Shumko, S. M.
Bibcode: 1991BCrAO..83...18F
Altcode:
  No abstract at ADS

Title: Solar gravity modes.
Authors: Hill, H.; Froehlich, C.; Gabriel, M.; Kotov, V. A.
Bibcode: 1991sia..book..562H
Altcode:
  The internal gravity modes, or g-modes, of the Sun may be important
  both in affecting the internal structure of the Sun and in furnishing a
  diagnostic probe of the solar interior. The internal structure could be
  altered by core mixing due to unstable g-modes or by nonlinear effects
  due to large-amplitude g-modes located in the core. On the other hand,
  small-amplitude g-modes operating in the linear regime offer the
  possibility of studying in detail the present state of internal solar
  structure such as the internal rotation rate, the Brunt-Väisälä
  frequency, the speed of sound and the mean molecular weight. In all
  of these roles, the solar g-modes may be important. The g-modes may
  be a contributor to the solar neutrino paradox and/or they may be a
  source of information leading to a more complete understanding of the
  physics responsible for the paradox. The observational work on solar
  g-modes does not exclude any of these possibilities at this time.

Title: The 160-minute period in differential measurements of the
    brightness of the Sun (1976-1987)
Authors: Kotov, V. A.; Didkovskii, L. V.; Khaneichuk, V. I.
Bibcode: 1991BCrAO..83...27K
Altcode:
  No abstract at ADS

Title: The helioseismological experiment at the Phobos interplanetary
    station - Preliminary results
Authors: Froehlich, C.; Bonnet, R. M.; Bruns, A. V.; Vial, J. C.;
   Delaboudiniere, J. P.; Domingo, V.; Kollath, Z.; Kotov, V. A.;
   Rachkovskii, D. N.; Wehrli, Ch.
Bibcode: 1991IzKry..83...22F
Altcode:
  Preliminary results obtained from IPHIR (Interplanetary Helioseismology
  by Irradiance Measurements), a solar irradiance experiment on board
  the Soviet planetary mission Phobos-2, are presented. During the
  spacecraft's flight to Mars, the instrument gathered valuable data on
  tiny variations of solar irradiance over the course of six months. The
  data clearly show 5-min oscillations with relative amplitudes of about
  10 exp -5 and with a well-defined pattern of discrete peaks in the
  power spectrum. The data of the red channel (it exhibited the lowest
  degradation of sensitivity over time) reveal remarkable temporal changes
  of amplitudes of discrete peaks within a period range of about 5 min,
  but with excellent frequency stability.

Title: The 160-minute oscillations of some extragalactic objects.
Authors: Kotov, V. A.; Liutyi, V. M.
Bibcode: 1991IzKry..83..216K
Altcode:
  An analysis of the UBV photometric and X-ray data on the rapid
  variability of active galactic nuclei (AGN) shows that there is a
  statistically significant (from 2- to 5-sigma confidence level) period
  of 160.1 min for several AGN, with an average harmonic amplitude of
  about 4 percent for X-rays and 1 percent for optical data. EXOSAT
  measurements showed the presence of 160-min periodicity in NGC 4051,
  NGC 4151, Mrk 335, and possibly NGC 6814 and MCG-6-30-15. The initial
  phases of this 160-min variability in the X-ray fluxes for five AGN are
  found to coincide with the phase of the 160-min oscillations of the sun.

Title: A 160-minute period in differential measurements of solar
    brightness (1976-1987)
Authors: Kotov, V. A.; Didkovskii, L. V.; Khaneichuk, V. I.
Bibcode: 1991IzKry..83...34K
Altcode:
  Differential (center-to-limb) measurements of the sun's brightness
  were performed at the Crimean Astrophysical Observatory with a solar
  magnetograph, a near-IR brightness monitor, and photodiode arrays. An
  analysis of all the measurements (487 days of observations, 2661 hours
  in all) made from 1976 through 1987 in different spectral passbands
  (from 0.51 to 1.65 micron) showed the presence of statistically
  significant periodicity (160.009 +/- 2 min), with a confidence level
  of 2 to 4 sigma. This value is in excellent agreement with the period
  160.009 +/- 2 min found much earlier in Doppler shift measurements. The
  mean relative amplitude of total irradiance variations for this
  160.01-min period, as inferred from the data, is about 4 x 10 exp -6,
  and therefore does not contradict the upper limit of about 5 x 10 exp
  -6 established by the ACRIM-SMM bolometric measurements.

Title: Compact Extragalactic Objects - Search for 160-MIN Periodicity
    in X-Ray Data
Authors: Lyutyi, V. M.; Kotov, V. A.
Bibcode: 1990SvAL...16..331L
Altcode:
  No abstract at ADS

Title: Compact extragalactic objects : a search for 160-minute
    periodicity in the X-ray data.
Authors: Lyuty, V. M.; Kotov, V. A.
Bibcode: 1990PAZh...16..771L
Altcode: 1990PisAZ..16..771L
  Data on the X-ray variability of the Seyfert 1 galaxies NGC 4051 and
  4151 collected by the Ariel-5 and Exosat satellites are examined. It
  is revealed that a statistically significant 160.010 min period with
  a harmonic amplitude of 4-9 percent exists. It is predicted that
  the same periodicity exists for the nucleus of the third Seyfert,
  MCG-6-30-15. Results from this study support with earlier theories
  concerning the 'ubiquitous' status of the 160 min oscillations, based
  on observations of the sun and the nuclei of other Seyfert galaxies
  and the quasar 3C 273.

Title: Variation in the 160.010 m period of the solar relative
    difference brightness
Authors: Li, Ru-Feng; Kotov, V. A.; Didkovskii, L. V.
Bibcode: 1990SCSMP..33.1100L
Altcode:
  Two photoelectric diode arrays (16 x 16 and 32 x 32 pixels,
  respectively) were used to measure the difference brightness of the
  center of the sun with respect to the limb of the solar disk in 1986 at
  wavelengths of 0.7-0.8 micron. The results indicate a period of 160 m
  and an average amplitude of 0.00008 solar relative intensity unit. A
  refined value of the oscillation period of 160.0099 m is obtained
  from the periodic values of the difference brightness observed for 358
  days (1870 hr) over the period 1976-1986 at the Crimean Astrophysical
  Observatory. This is in good agreement with the IR observed value of
  160.0100 m (+ or - 6) and a value of 160.010 m (+ or - 1) obtained at
  the Doppler difference velocity.

Title: 160-MINUTE Solar Variations and the 22-YEAR Cycle
Authors: Kotov, V. A.; Tsap, T. T.
Bibcode: 1990SoPh..128..269K
Altcode: 1990IAUCo.121P.269K
  Systematic measurements of the differential Doppler velocity of the Sun
  have been performed in Crimea from 1974 through 1988 (total 987 days,
  6197 hours of observations). They confirm the presence of a long-term
  phase-coherent solar pulsation with a period of 160.010 min. On the
  other hand, the analysis of new data suggests that solar 160 min
  pulsation might, in frequency, have a multiplet fine structure. In
  particular, large changes of amplitude and phase of the pulsation over
  the years 1982-1986 may indicate that during the last few years we have
  been observing the solar 160 min oscillation of the `second portion'
  of the 22 year solar cycle.

Title: On short-term variations of the global magnetic field of
    the Sun.
Authors: Demidov, M. L.; Kotov, V. A.; Grigor'ev, V. M.
Bibcode: 1990IzKry..82..147D
Altcode:
  Measurements of the mean magnetic field of the Sun seen as a star
  made in 1975 - 1978 and 1987 at the Crimean, Mount Wilson and Sayan
  observatories show the presence of more or less persistent oscillations
  with periods near 47, 60, 85 and 160 minutes and average amplitudes
  ≡1 mkT. The new Sayan-1987 observations appear to confirm the
  previous conclusion [1976, 1985] about long-time coherency of the
  famous 160,0101-minute oscillation of the Sun.

Title: Short-period variations in the Sun's global magnetic field
Authors: Demidov, M. L.; Kotov, V. A.; Grigor'ev, V. M.
Bibcode: 1990BCrAO..82..135D
Altcode:
  No abstract at ADS

Title: A Problem with the 160-Minute Pulsation of the Sun
Authors: Kotov, V. A.
Bibcode: 1990LNP...367..235K
Altcode: 1990psss.conf..235K
  Differential measurements (1974-1988) of the solar velocity and
  photospheric brightness show the presence of long-term pulsation of the
  Sun with a period of P o=160.0101(±1) min. Its nature is poorly known
  since it seems hardly possible to explain the periodicity in terms
  of solar g-modes. But the most fascinating appears to be the recent
  discovery of the same 160-min periodicity in the light-flux variations
  of several AGN (active galactic nuclei). This finding strongly supports
  the hypothesis advanced much earlier about cosmological origin of
  the oscillation.

Title: Variation in the 160.010 m period of the solar relative
    difference brightness
Authors: Li, R. F.; Kotov, V. A.; Didkovskii, L. V.
Bibcode: 1990SSSMP..33.1100L
Altcode:
  No abstract at ADS

Title: Pulsation of the Sun: remarkable change due to the 22-year
    cycle of activity?
Authors: Kotov, V. A.; Tsap, T. T.; Didkovskii, L. V.
Bibcode: 1990IzKry..82..138K
Altcode:
  Systematic measurements of differential Doppler velocity performed
  at the Crimean Observatory from 1974 through 1987 (in all 902 days,
  5612 hours of observations) confirm the presence of the long-term
  phase-coherent solar pulsation with a period of 160.01 min. On the other
  hand, the analysis of new data suggests that 160-min pulsation on the
  Sun might have a multiplet (in frequency) fine structure. Particularly,
  great changes of amplitude and phase of the pulsation over 1983 - 1987
  years may indicate that since 1982 - 1983 years the authors observe
  indeed 160-min oscillation pattern inherent in the "second part" of
  the 22-year cycle of solar magnetic activity. Being verified, this
  unpredicted property of the pulsation can offer a novel possibility
  for probing the Sun's interior and perhaps for the study of the solar
  internal rotation and 11(22)-year cycle.

Title: Solar pulsations: effects due to the 22-year activity cycle?
Authors: Kotov, V. A.; Tsap, T. T.; Didkovskii, L. V.
Bibcode: 1990BCrAO..82..127K
Altcode:
  No abstract at ADS

Title: V1521 Cygni (Cygnus X-3)
Authors: Kotov, V.; Nesterov, N. S.
Bibcode: 1989IAUC.4826....2K
Altcode: 1989IAUC.4826....0K
  V. Kotov, Crimean Astrophysical Observatory, reports that the recent
  flare (cf. IAUC 4817) was independently detected by N. S. Nesterov,
  who found the 8.2-mm flux to increase from &lt; 0.5 Jy on July 19 to
  11.32 +/- 0.1 Jy on July 21.

Title: Five HERZ - a characteristic frequency of neutron stars ?
Authors: Kotov, V. A.; Fomin, V. P.
Bibcode: 1989Afz....30..362K
Altcode:
  No abstract at ADS

Title: Five hertz—A characteristic frequency of neutron stars?
Authors: Kotov, V. A.; Fomin, V. P.
Bibcode: 1989Ap.....30..221K
Altcode:
  No abstract at ADS

Title: 5-HZ - a Characteristic Frequency of Neutron Stars
Authors: Kotov, V. A.; Fomin, V. P.
Bibcode: 1989Afz....30..221K
Altcode:
  No abstract at ADS

Title: IPHIR: The helioseismology experiment on the PHOBOS mission.
Authors: Fröhlich, C.; Bonnet, R. M.; Bruns, A. V.; Delaboudinière,
   J. P.; Domingo, V.; Kotov, V. A.; Kollath, Z.; Rashkovsky, D. N.;
   Toutain, T.; Vial, J. C.; Wehrli, C.
Bibcode: 1988ESASP.286..359F
Altcode: 1988ssls.rept..359F
  IPHIR (InterPlanetary Helioseismology by IRradiance measurements) is
  a solar irradiance experiment on the USSR planetary mission PHOBOS to
  Mars and its satellite Phobos. The experiment is a cooperative effort
  of PMOD/WRC, LPSP, SSD/ESA, KrAO and CRIP. The sensor is a three channel
  sunphotometer (SPM) which measures the solar spectral irradiance at 335,
  500 and 865 nm with a precision of better than 1 ppm. A two axis solar
  sensor (TASS) is added to monitor the moderate solar pointing of the
  spacecraft. A microprocessor based data processing unit controls the
  sensor operation, acquires the data, and performs the data compression
  for the transmission at a mean rate of 1 bit/s. The two spacecrafts
  have been launched on July 7th and 12th, 1988. The experiment on
  PHOBOS I gathered data during 45 days before the S/C was lost, the
  one on PHOBOS II is still operating. The data recovery is excellent
  with virtually 100% coverage. Although the signal is disturbed by the
  pointing of the spacecraft the results of a preliminary analysis in
  the range of the 5-minutes oscillations demonstrate the improvement
  achievable due to the fact that the time series is truly continuous
  and the instrumental and sampling noise is very low.

Title: Book Review: The galaxy and the solar system. / U Arizona
    Press, 1986.
Authors: Kotov, V. A.; Kostik, R.; Shchukina, N.; Švestka, Zdeněk;
   Kotov, V. A.
Bibcode: 1988SoPh..115..203K
Altcode: 1988SoPh..115..203S
  No abstract at ADS

Title: A. B. Severny (1913-1987)
Authors: Kotov, V. A.; Mozzerin, V. M.
Bibcode: 1988SoPh..115....1K
Altcode: 1988SoPh..115....1.
  No abstract at ADS

Title: Observations of Solar Global Oscillations 1983-1985 and
    Potential Influence of Terrestrial Sources of Errors
Authors: Severny, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1988IAUS..123...33S
Altcode:
  The Earth atmospheric pressure fluctuations in the 5-min range of
  periods are analysed and their influence on observations of solar
  5-min oscillations are briefly discussed. New series of observations
  confirmed the oscillations of the Sun with period of 160.010 min.

Title: Five-minute oscillations of the solar brightness: observations
    with a photodiode array
Authors: Didkovskii, L. V.; Kotov, V. A.; Tarasova, T. N.
Bibcode: 1988BCrAO..79..174D
Altcode: 1990BCrAO..79..174D
  The authors present the results from six-days observations of
  5<SUP>m</SUP> oscillations of the solar brightness in 1984 totaling
  approximately 58 hours. With the aid of a photodiode array (16x16
  pixels), temporal variations of solar intensity in the central portion
  of the Sun's disk (≡0.2 D<SUB>sun</SUB>) were measured within spectral
  passband 0.82±0.13 μm with 1<SUP>m</SUP> integration time. Average
  power spectrum shows the presence of 5<SUP>m</SUP> oscillations with
  a discrete pattern of peaks and mean amplitudes ≡10<SUP>-4</SUP>
  in relative units. A typical frequency splitting, 69.6±0.8 μHz, is
  close to but yet significantly different from a well-known splitting
  67.7 μHz inferred from Doppler observations. The authors also noted
  that in 1984 observational season the mean power in 5<SUP>m</SUP>
  range of periods was decreased by a factor of 3 in comparison with
  analogous measurements made in 1983. It is supposed that these changes
  probably reflect real changes of solar brightness oscillations which,
  in turn, may be caused by the 11-year solar activity cycle.

Title: 160-minutes oscillations of the Sun: observations in 1974
    - 1986.
Authors: Kotov, V. A.; Severnyj, A. B.; Tsap, T. T.
Bibcode: 1988IzKry..79....3K
Altcode:
  Observations of global oscillations of the Sun were carried out at
  the Crimean Astrophysical Observatory during 711 days (4345 hours in
  total) in 1974 - 1986. These data confirm an existence and dominant
  character of solar low frequency oscillations with a period of
  160<SUP>m</SUP>0100(±6). The latter exhibits a remarkable long-time
  phase stability. Observations show that the amplitude of the 160-minute
  oscillation varies significantly during the observational season and
  also from year to year. The most interesting seems to be the progressive
  decrease of yearly-mean amplitude: from about 1.2 m/s in 1974 - 1975 to
  about 0.3 m/s in 1984 - 1986. It is suggested that this decrease might
  be connected with the 22-year cycle of solar activity and, therefore,
  may throw additional light on the nature of the 160-minute periodicity
  in the Sun.

Title: 160.01-Min oscillations of compact extragalactic objects and
    plausible cosmological consequences
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1988BCrAO..79..130K
Altcode: 1990BCrAO..79..130K
  The previous analysis of UBV-photometry of the quasar 3C 273 and the
  Seyfert galaxy NGC 4151 is extended to nuclei of other Seyferts in
  search of oscillations with a "ubiquitous" period P<SUB>0</SUB> =
  161.0101 (±1)<SUP>m</SUP>. Now the authors find the presence of the
  same period, within errors, for three more Seyferts: NGC 1275 (period
  160.0094 (±8)<SUP>m</SUP>), NGC 3516 (160.0100 (±9)<SUP>m</SUP>),
  and NGC 7469 (159.98 (±3)<SUP>m</SUP>) - with more or less random
  scattering of phases and total relative amplitudes (2-3%). It is argued
  that the periodic effect can be accounted for by neither observational
  biases nor some artifacts in the reduction procedure. For the NGC 4151
  the result is strongly supported by analysis of X-ray data obtained on
  board the Ariel-5 and EXOSAT satellites. It is pointed out that true
  nature of the solar 160<SUP>m</SUP> oscillation with its seemingly
  universal character is still an open question. It is hypothesized that
  the P<SUB>0</SUB> period may have a status of a preferred time-scale for
  the Universe. The hypothesis can possibly help to avoid a singularity
  present in the standard Big Bang cosmology.

Title: 160-Minute oscillations of the Sun: observations in 1974-1986
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1988BCrAO..79....1K
Altcode: 1990BCrAO..79....1K
  Observations of global oscillations of the Sun were carried out
  at the Crimean Astrophysical Observatory during 711 days (4345
  hours in total) in 1974 - 1986. These data confirm an existence and
  dominant character of solar low frequency oscillations with a period
  of 160.0100<SUP>m</SUP> (±6). The period exhibits a remarkable
  long-time phase stability which appears to be persistent for more
  than a decade. The period agrees perfectly well with the value
  160.0101<SUP>m</SUP> (±1) established earlier from analysis of
  onset times of solar flares observed on the Sun during 1947 - 1980
  interval. Observations show that amplitude of the 160-minute oscillation
  varies significantly during observational season and also from year to
  year. The most interesting feature seems to be a progressive decrease
  of yearly mean amplitude: from about 1.2 m/sec in 1974 - 1975 to about
  0.3 m/sec in 1984 - 1986. It is suggested that this decrease might
  be connected with the 22-year cycle of solar activity and, therefore,
  may throw additional light on the nature of 160-minute periodicity in
  the Sun.

Title: Space-time analysis of the Sun's brightness oscillations. I.
Authors: Didkovskii, L. V.; Kotov, V. A.
Bibcode: 1988BCrAO..80..114D
Altcode: 1990BCrAO..80..114D
  A 1024-cell 32x32 photodiode array was used to register the global
  oscillations of the Sun's brightness in a 0.73±0.10 μm spectral
  band. A simple procedure for processing of the observational data
  based on approximation of the "quiet Sun" brightness distribution by
  Chebyshev polynomials is described. A dinstinct concentration of power
  peaks in the range of periods around 5 minutes is seen in the power
  spectra of the "oscillating Sun minus quiet Sun" remainders.

Title: Photometry of the Seyfert galaxy NGC 4151 and the quasar 3C
273: the 160.010 minutes period.
Authors: Kotov, V. A.; Lyutyj, V. M.
Bibcode: 1988IzKry..78...89K
Altcode: 1988IKryO..78...89K
  A reanalysis of the U-photometric data (1968 - 1986) of the nucleus of
  the Seyfert galaxy NGC 4151 fully confirmed the previous conclusion
  about the presence of the period P<SUB>G</SUB> = 160.0098 (±5)
  min with a harmonic amplitude 0.014 mag. Similar analysis of
  the 18 year (1968 - 1986) photometry of the quasar 3C 273 also
  reveals an existence of the same period: P<SUB>Q</SUB> = 160.0105
  (±7) min (harmonic amplitude 0.015 mag.). Both periods coincide
  with the well-known period P<SUB>0</SUB> = 160.0106 (±6) min of
  global oscillations of the Sun. Such ubiquitous character of the
  160-min period may suggest its cosmological status and, perhaps,
  indicates that this period may be a new astrophysical parameter
  with intriguing inferences for cosmology. The authors propose a
  simple relation between the Hubble constant H<SUB>0</SUB> and the
  period P<SUB>0</SUB>:dP<SUB>0</SUB>/dt = H<SUB>0</SUB>P<SUB>0</SUB> =
  1.9×10<SUP>-14</SUP>. The resulting life-time of the 160-min period
  appears to be equal to ≡16×10<SUP>9</SUP>years, i.e. the age of
  the Universe.

Title: Spatially-temporal analysis of the solar brightness
    oscillations. I.
Authors: Didkovskij, L. V.; Kotov, V. A.
Bibcode: 1988IzKry..80..118D
Altcode:
  The 1024-channel (32×32) photodiode array is used for detection of the
  global solar brightness oscillations within 0.73±0.10 μm passband. A
  simple method of data reduction based on computation of the "quiet Sun",
  approximated by the system of Chebychev polynomials, is described. Power
  spectra of the residuals "oscillating Sun minus quiet Sun" clearly
  show a concentration of power in the 5-minute range of periods.

Title: The 160.01 minutes oscillations of compact extragalactic
    objects and plausible cosmological consequences.
Authors: Kotov, V. A.; Lyutyj, V. M.
Bibcode: 1988IzKry..79..139K
Altcode: 1988IKryO..79..139K
  UBV-photometry is extended to nuclei of Seyferts in
  search for oscillations with a «ubiquitous» period
  P<SUB>0</SUB> = 160.0101(±1)<SUP>m</SUP>: NGC 1275 (period
  160.0094(±8)<SUP>m</SUP>), NGC 3516 (160.0100(±9)<SUP>m</SUP>) and NGC
  7469 (159.98(±3)<SUP>m</SUP>) - with more or less random scattering
  of phases and total relative amplitudes (2 - 4)%. It is argued that
  the periodic effect can be accounted for by neither observational
  biases nor some artefacts in the reduction procedure. For NGC 4151 the
  results are strongly supported by analysis of X-ray data obtained on
  board the Ariel-5 and EXOSAT satellites. It is pointed out that the
  true nature of solar 160<SUP>m</SUP>-oscillations with its seemingly
  universal character is still an open question. It is hypothesized that
  the P<SUB>0</SUB>-period may have a status of a preferred time-scale
  for the Universe. The latter can possibly help us to avoid a singularity
  present in the standard big-bang cosmology.

Title: Periodic variations of solar brightness observed with the
    1024-channel photodiode array.
Authors: Didkovskij, L. V.; Kotov, V. A.
Bibcode: 1988IzKry..80..124D
Altcode:
  The observations of long-period brightness oscillations of the Sun
  were carried out by using a photodiode array (32×32 pixels) within
  the spectral passband 0.73±0.10 μm during 7 days in 1986. The spatial
  resolution was about 53 arc sec and accumulation time 38 sec. The data
  analysis showed that relative amplitudes of brightness variations
  increase toward the centre of the solar disk. It suggests a real
  (solar) origin of a significant part of the observed variations. For
  the central part of the disk (0.3 D<SUB>sun</SUB> in diameter) the
  data reveal 160-min oscillations with the average relative amplitude
  ≡5×10<SUP>-5</SUP>. The phase of 160-min oscillations nicely agrees
  with the one determined from earlier, 1976 - 1985, observations.

Title: Five-minute oscillations of the solar brightness: observations
    with a photodiode array.
Authors: Didkovskij, L. V.; Kotov, V. A.; Tarasova, T. N.
Bibcode: 1988IzKry..79..184D
Altcode:
  The authors present the results from 6-days observations of
  5<SUP>m</SUP>-oscillations of the solar brightness in 1984 totalling
  approximately 58 hours. Average power spectrum shows the presence of
  5<SUP>m</SUP>-oscillations with a discrete pattern of peaks and mean
  amplitudes ≡10<SUP>-4</SUP> in relative units. A typical frequency
  splitting, 69.5±0.8 mkHz, is close to but yet significantly
  different from a well-known splitting 67.7 mkHz inferred from
  Doppler observations. In 1984 observational season the mean power
  in 5<SUP>m</SUP>-range of periods is decreased by factor of 3 in
  comparison with analogous measurements made in 1983. It is supposed
  that these changes reflect probably real changes of solar oscillations
  seen in brightness which, in turn, may be caused by 11-year cycle of
  solar activity.

Title: Periodic variations of the brightness of the Sun: experience
    in observations with a 1024-channel array
Authors: Didkovskii, L. V.; Kotov, V. A.
Bibcode: 1988BCrAO..80..120D
Altcode: 1990BCrAO..80..120D
  Oscillations of the Sun's brightness at 0.73±0.10 μm were observed
  with a 32x32 photodiode array. The measurements were made on 7 days
  in 1986 with a spatial resolution of ≡53″and an accumulation
  time of 38 sec. The relative amplitude of the long-period brightness
  variations rises significantly toward the center of the disk. It is
  assumed that the variations are due in large part to oscillations of the
  Sun. For a central region of the disk 0.3 D<SUB><SUB>sun</SUB></SUB>
  in diameter, 160-minute oscillations are detected with a relative
  amplitude of ≡5·10<SUP>-5</SUP>. The phase of these variations for
  the 160.010-min period practically coincides with the mean phase of
  the differential-brightness oscillations from earlier (1976 - 1985)
  observations.

Title: Photometry of the Seyfert galaxy NGC 4151 and the quasar 3C
273: the 160.010-minute period
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1988BCrAO..78..100K
Altcode: 1989BCrAO..78..100K
  A new analysis of photometric data on the nucleus of the Seyfert
  galaxy NGC 4151 (1968 - 1986, U filter) fully confirmed the conclusion
  indicating a period P<SUB>G</SUB> = 160.0098<SUP>m</SUP>(±5) with
  a harmonic amplitude of 0.014 magnitude. Analysis of 18 years of
  photometric observations of the quasar 3C 273 (1968 - 1986) also
  indicated that the same period is present here within the limits of
  error: P<SUB>Q</SUB> = 160.0105<SUP>m</SUP>(±7), amplitude 0.015
  magnitude. The two periods agreed with the known period P<SUB>0</SUB>
  = 160.0106<SUP>m</SUP>(±6) detected earlier in the power spectrum
  of the Sun's global oscillations. This "universal" nature of the
  160<SUP>m</SUP> period may indicate that it is of cosmologic origin,
  and the period itself appears to be a new astrophysical parameter
  with definite implications for cosmology. In particular, a simple
  relation is proposed to link Hubble's constant H<SUB>0</SUB> to the
  period P<SUB>0</SUB>:dP<SUB>0</SUB>/dt = H<SUB>0</SUB>P<SUB>0</SUB> =
  1.9.10<SUP>-14</SUP>. The corresponding lifetime of the 160<SUP>m</SUP>
  period is found to be ≡16.10<SUP>9</SUP>yr, i.e., equal to the age
  of the Universe.

Title: The 160-minute period, internal rotation, and 11-year solar
cycle: are they related?
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1987BCrAO..77...56K
Altcode: 1989BCrAO..77...56K
  No abstract at ADS

Title: Differential observations of the photospheric brightness
    oscillations of the Sun
Authors: Didkovskii, L. V.; Kotov, V. A.
Bibcode: 1987BCrAO..76..132D
Altcode: 1989BCrAO..76..132D
  No abstract at ADS

Title: Rotation of the Sun and rotation of its general magnetic field.
Authors: Kotov, V. A.
Bibcode: 1987IzKry..77...39K
Altcode:
  The author analysed the measurements of the solar mean magnetic
  field (SMMF, 1968 - 1984) and also the time series of polarity
  of the interplanetary magnetic field (IMF 1926 - 1983). Power
  spectra of both sets show the presence of two dominant
  periods of rotation: 26<SUP>d</SUP>.94±0<SUP>d</SUP>.02 and
  28<SUP>d</SUP>.20±0<SUP>d</SUP>.02 (synodic). The first period is
  interpreted as the most coherent period of rotation of the surface
  magnetic fields near equator. The other period corresponds to
  the highest peak in the IMF power spectrum and does not show any
  splittings due to differential rotation and 22-year cycle. It is
  conjectured that this 28<SUP>d</SUP>.20 period reflects rotation of
  a deeply rooted solar magnetic field which penetrates the radiative
  zone of the Sun. This tentative conclusion appears to be compatible
  with recent helioseismological observations. The author notes that the
  28<SUP>d</SUP>.20 period corresponds to rotation rate of the photosphere
  at heliolatitudes of about 28° where spots usually originate at the
  onset of each solar cycle.

Title: The rotation of the Sun and the rotation of its general
    magnetic field
Authors: Kotov, V. A.
Bibcode: 1987BCrAO..77...42K
Altcode: 1989BCrAO..77...42K
  No abstract at ADS

Title: On the possibility of rapid rotation of the solar core.
Authors: Kotov, V. A.; Kosovichev, A. G.
Bibcode: 1987IzKry..77...72K
Altcode:
  The authors discuss a conjecture that the central core of the Sun
  rotates plausibly with very short period near 160<SUP>m</SUP>. The
  rotational splitting of low degree p-modes oscillations was calculated
  for the standard solar model, but with the inner core of various size
  spinning with the 160<SUP>m</SUP> period. The results of calculations
  agree with the actual splitting of l = 1, 2 and 3 modes inferred by
  Duvall et al. (1984) from observations of 5<SUP>m</SUP>-oscillations,
  if one assumes that the radius of a rapidly spinning core is less than
  0.08 R_sun;. Such small core contains about 6% of the total solar
  mass. The resulting gravitational quadrupole moment J<SUB>2</SUB>
  of the Sun, ⪉4×10<SUP>-6</SUP>, does not contradict the results of
  observational data on solar oblateness.

Title: The frequency of 10 Hz in the distribution of radiopulsar
    periods
Authors: Kotov, V. A.; Vladimirskii, B. M.
Bibcode: 1987BCrAO..76..104K
Altcode: 1989BCrAO..76..104K
  No abstract at ADS

Title: The 160 minutes period, internal rotation and 11-year cycle
of the Sun: evidence for a relationship?
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1987IzKry..77...51K
Altcode:
  In order to specify an exact value of the 160<SUP>m</SUP> period of
  solar oscillations, the authors analyse a sample of about 19,000
  chromospheric flares on the Sun as observed by the world network
  of solar observatories in 1947 - 1980. For the dominant peak in the
  160<SUP>m</SUP> range studied the authors obtain the best period's
  value of 160<SUP>m</SUP>.01015±0<SUP>m</SUP>.00008, which is in
  excellent agreement with the result of Doppler observations. Some
  physical relation between fine structure of the 160<SUP>m</SUP>
  period and solar cycle might exist. The time sequence of flares
  reveals also a strong peak in the 80<SUP>m</SUP> range. Discrete
  frequencies of 160<SUP>m</SUP> oscillations (as seen in solar flares)
  may be dependent on detailed structure of the deep solar interior
  and therefore may be used to map out the interior rotation rate. It
  is also pointed out that the model with a rapidly spinning small core
  may reasonably explain the existence of a slower rotation zone inside
  the Sun, near 0.3 R_sun;, deduced recently by Duvall et al. (1984)
  from helioseismological observations.

Title: The oscillation period of Delta Scuti stars close to 160
    minutes
Authors: Kotov, V. A.
Bibcode: 1987BCrAO..76...10K
Altcode: 1989BCrAO..76...10K
  No abstract at ADS

Title: The frequency 10 Hz in the distribution of radiopulsar periods.
Authors: Kotov, V. A.; Vladimirskii, B. M.
Bibcode: 1987IzKry..76...93K
Altcode:
  A special statistical procedure, based on computation of the so-called
  "commensurability spectrum", being applied to the distribution of
  periods of 330 pulsars revealed the dominant frequency ν<SUB>0</SUB>
  = 10.05±0.07 Hz (period 0.0995±0.0007 s) of a quasiperiodic
  modulation of the distribution. This modulation means the presence of a
  statistically significant, at about 3.3 to 4.1-sigma confidence level,
  deficit of a number of PSR with frequencies ν ≈ ν<SUB>0</SUB>/n,
  where n is integer. The effect appears to be strongly pronounced for
  PSR with periods from 0.4 to about 1.6 s and can not be ascribed to
  some unknown observational selection effect.

Title: Differential observations of photospheric brightness
    oscillations of the Sun.
Authors: Didkovskii, L. V.; Kotov, V. A.
Bibcode: 1987IzKry..76..119D
Altcode:
  A photodiode array illuminated by the pin-hole image of the Sun is
  used to measure relative (center-to-limb) brightness variations of the
  photosphere at 0.82 μm, associated with global oscillations of the
  Sun. The observations performed in 1983 and 1984 during 86 days yielded
  about 448 hours of data on differential brightness oscillations. These
  data were analysed in the frequency range from 55 to 165 μHz (100 to
  300 min in period). The power spectra obtained vary significantly from
  season to season. The data show the existence of global oscillations
  with the well-known 160 min period. The mean brightness amplitude of
  the data for this 160-min mode is found to be ≡5×10<SUP>-5</SUP>
  in units of average solar brightness. It corresponds to ≡(0.2 -
  2.0)×10<SUP>-6</SUP> for a harmonic amplitude of the 160-min variations
  in the solar irradiance in the 0.82 μm spectral range.

Title: The oscillation period of Delta Scuti stars close to 160
    minutes.
Authors: Kotov, V. A.
Bibcode: 1987IzKry..76...10K
Altcode:
  The so-called {resonance power spectrum} (or {commensurability
  spectrum}) computed for 217 δ Sct stars shows that the dominant (the
  most commensurate) period for the total set of oscillation periods of
  these stars equals to 162.2±2.8 min. This value coincides fairly well,
  within the limits of error, with the famous 160-min period of global
  oscillations of the Sun. The finding appears to favour the nonlinear
  mechanism of resonant interaction between different modes of stellar
  oscillations, with the 160-min period being the most characteristic
  (resonant) one.

Title: The 160-minutes period in extragalactic objects: the LMC
    (RR Lyr stars) and NGC 4151.
Authors: Kotov, V. A.; Lyuty, V. M.
Bibcode: 1987IzKry..77..148K
Altcode: 1987IKryO..77..148K
  According to the finding that the most characteristic ("resonant"
  or commensurate) period for the orbital period distribution of close
  binaries of the Galaxy and also for RR Lyr variables in globular
  clusters is very near to 160 min, the authors computed a so-called
  "resonance power spectrum" for the sample of 72 RR Lyr stars observed
  in and around the two LMC globular clusters, NGC 2257 and 1786. It
  is found that the "resonant" period for these stars, 159.9±1.5 min,
  fairly agrees with the previous result. With the aim to extend the
  search for traces of this "ubiquitous" 160-min periodicity among
  various astrophysical objects, the authors analysed also the UBV
  photometric measurements of the nucleus of the Seyfert galaxy NGC
  4151, made in the 1968 - 1984 interval. Power spectrum of the data
  clearly showed the presence of a significant, at the 4.1-sigma
  confidence level, period 160.0099±0.0004 min with about ±2.5%
  amplitude. The authors estimate the lifetime of the 160-min period to be
  ≡15×10<SUP>9</SUP>years, which is nearly the age of the Universe. The
  product P<SUB>0</SUB>H<SUB>0</SUB>, where H<SUB>0</SUB> is the Hubble
  constant, appears to be a dimensionless parameter ≡2×10<SUP>-14</SUP>
  which might be of great interest for cosmology.

Title: On the possibility of rapid rotation of the solar core
Authors: Kotov, V. A.; Kosovichev, A. G.
Bibcode: 1987BCrAO..77...80K
Altcode: 1989BCrAO..77...80K
  No abstract at ADS

Title: The 160-minute period in extragalactic objects: the LMC
    (RR Lyr stars) and NGC 4151
Authors: Kotov, V. A.; Lyutyi, V. M.
Bibcode: 1987BCrAO..77..166K
Altcode: 1989BCrAO..77..166K
  No abstract at ADS

Title: 160 min solar flare activity modulation.
Authors: Kotov, V. A.; Levitskij, L. S.
Bibcode: 1986BCrAO..75...54K
Altcode: 1987BCrAO..75...54K
  No abstract at ADS

Title: Solar oscillations and rotation of close binary systems in
the Galaxy: the 160 minute period.
Authors: Kotov, V. A.
Bibcode: 1986BCrAO..74...65K
Altcode: 1987BCrAO..74...65K
  No abstract at ADS

Title: The axial-rotation velocity distribution in the solar system
    and the sun's 160-min oscillations.
Authors: Kotov, V. A.
Bibcode: 1986BCrAO..75...83K
Altcode: 1987BCrAO..75...83K; 1986BuCri..75...83K
  No abstract at ADS

Title: Observations of 5-minute oscillations in the brightness of
    the solar photosphere.
Authors: Didkovskij, L. V.; Kotov, V. A.
Bibcode: 1986BCrAO..74..123D
Altcode: 1987BCrAO..74..123D
  No abstract at ADS

Title: The 160 min period in RR Lyr stars in globular clusters and
    highly evolved close binary systems.
Authors: Kotov, V. A.
Bibcode: 1986BCrAO..75..104K
Altcode: 1987BCrAO..75..104K
  No abstract at ADS

Title: Solar oscillations and the rotation of close binary systems
    in the Galaxy - The 160-min period
Authors: Kotov, V. A.
Bibcode: 1986IzKry..74...69K
Altcode:
  The previous conclusion that the 160<SUP>m</SUP> period of the global
  oscillations of the sun might be related to the external 160<SUP>m</SUP>
  gravitational wave from an unknown source is checked by statistical
  analysis of the period distribution of close binary stars. It is
  found that the observed distribution of about 4000 binaries shows a
  significant (3.5 σ confidence) lack of periods ≡2mzmP<SUB>0</SUB>
  and an excess (2.5 σ confidence) of periods ≡(2mz+1)mP<SUB>0</SUB>,
  where z is integer and P<SUB>0</SUB> = 160<SUP>m</SUP>. The overall
  significance of this 160<SUP>m</SUP> effect is about 4.1 σ. A
  precise determination of the characteristic period leads to the value
  160<SUP>m</SUP>.0±0<SUP>m</SUP>.1 which is in fair agreement with the
  solar oscillation period 160<SUP>m</SUP>.0101±0<SUP>m</SUP>.0007. A
  similar analysis of the distribution of 97 catalysmic binaries
  shows that the same frequency, P<SUB>0</SUB><SUP>-1</SUP>, is
  characteristic for these objects. It is conjectured that the frequency
  P<SUB>0</SUB><SUP>-1</SUP> = 104.160 μHz in the distribution of orbital
  rates of the galactic binaries is a consequence of the 160<SUP>m</SUP>
  gravitational radiation which might be cosmological (relict) by nature.

Title: Observations of 5-minute oscillations of solar photospheric
    brightness
Authors: Didkovskii, L. V.; Kotov, V. A.
Bibcode: 1986IzKry..74..132D
Altcode:
  The results of ground-based observations of temporal variations of
  the solar brightness at 0.82±0.13 μm are presented. The authors
  find a statistically significant enhancement of the spectral power for
  frequencies between 2.6 and 3.4 mHz. These variations are attributed to
  global p-mode for solar intensity oscillations because 5-minute peaks
  in the power spectrum reveal a discrete pattern with the well-known
  equidistant spacing of 68 microHz. The frequencies agree well with the
  values of 5-minute oscillations obtained from the total solar irradiance
  measurements made on board the SMM satellite. Five minute oscillations
  are seen in both "direct" (for the central area of the solar disk) and
  "differential" (center-to-limb) brightness signals and are thought to
  be associated with acoustic compression waves in the photosphere.

Title: The 160 min-period with regard to the frequency of occurrence
    of chromospheric flares.
Authors: Kotov, V. A.; Levitskij, L. S.
Bibcode: 1986psf..conf..112K
Altcode:
  No abstract at ADS

Title: Period of 160 minutes of RR Lyr variables in globular clusters
    and highly evolved close binary systems.
Authors: Kotov, V. A.
Bibcode: 1986IzKry..75..113K
Altcode:
  A statistical analysis based on computation of so-called
  "commensurability spectra" is applied to periods of 1211 RR Lyr
  variables in globular clusters and to a sample of highly evolved close
  binaries with orbital periods less than 4 days. It is shown that for
  the frequency range studied (from about 35 to 150 μHz) the period
  of 160 min appears to be the most characteristic one, with respect
  to commensurability, for both period distributions. The effect is
  found to be significant at about 3.8 and 3.2σ levels of confidence
  for RR Lyr variables and close binary systems correspondingly. It is
  suggested that this particular status of the 160-min period, at first
  discovered in the solar oscillations, then in galactic binary stars,
  and which seems to be of "universal" character, might reflect some
  unknown property of gravitational interaction.

Title: Modulation of the flare activity of the sun with a 160
    minute period.
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1986IzKry..75...59K
Altcode:
  The authors subjected to a statistical analysis the complete set
  of times of beginnings of chromospheric flares of importance B ≥
  1 observed on the sun during 1955 - 1980 (about 16200 flares in
  total). A high-resolution "power spectrum" of the time series was
  calculated for a range near the 160.0-min period using the superposed
  epoch technique and the χ<SUP>2</SUP>-criterion. It showed only
  two significant (⪆99.9% confidence) peaks corresponding to periods
  160.0056±2 and 160.0100±2 (min). It is supposed that the 160-min
  global oscillations of the sun trigger, statistically, occurrences of
  flares. A peak-to-peak amplitude of this 160-min effect is found to
  be about 12% with respect to the statistical mean value which would be
  expected in a random sample. It is noted that the spacing between the
  frequencies of those two dominant peaks corresponds fairly well to the
  11-year period. Nevertheless, some arguments are given in favour of a
  real (i.e. not arisen merely from 11-year modulation) nature of the
  duplicate structure of the 160-min period in solar flares. The same
  seems to be true for Doppler observations of solar oscillations. This,
  in turn, may lead to interesting conjectures on a possible physical
  association between 160-min oscillations and the solar 11-year cycle.

Title: Spin rates distribution in the solar system and 160 minute
    oscillations of the sun.
Authors: Kotov, V. A.
Bibcode: 1986IzKry..75...90K
Altcode:
  The previous analysis and results as regards the effect of a preferable
  commensurability of the spin rates (of planets and asteroids) with
  the 160-min period is now extended to a much more complete data set
  comprising 239 different bodies in the solar system: 223 asteroids
  with diameters D ≥ 30 km, 6 planets and 10 nuclei of short-period
  comets. It is found that for the frequency range studied (from about
  30 to 200 μHz) there is a unique period, 160 min, which shows the
  highest degree of overall commensurability with the entire sample of
  spin rates. The statistical significance of the result is estimated
  to be near 3.4σ to 5.8σ depending on one or another statistical
  hypothesis. A preliminary conclusion is made that the apparent
  "universal" behaviour of the 160-min periodicity can be classified,
  perhaps, as some property of the gravitational field.

Title: The 160-MINUTES Oscillations
Authors: Kotov, V. A.
Bibcode: 1985SoPh..100..101K
Altcode:
  We describe basic observational data regarding the 160-min oscillations
  of the Sun as well as the implications for helioseismology. The
  most acceptable theoretical interpretation seems to be a resonant
  interaction of gravity g-mode oscillations of the solar model with
  a slight modification to the equilibrium structure (with low heavy
  element abundance).

Title: On the problem of magnetic field asymmetry of the Sun:
    anomalous interplanetary magnetic field in 1970 - 1981.
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1985IzKry..71...32K
Altcode:
  Published data on solar magnetic asymmetry are reviewed, and it is
  shown that polar asymmetry is a characteristic feature of the solar
  magnetic field. Data on the daily AC-index of the IMF polarity
  (collected between 1926 and 1982) were studied by means of power
  spectrum analysis and the superposed epoch method. It is found that
  the annual variation in polarity shows a significant phase shift with
  respect to the change in the earth's heliolatitude in the course of a
  year. Contrary to the 1930-1969 time interval, when in each 10-year
  solar cycle the 1-year periodicity dominated the power spectra, the
  1970-1981 time interval was anomalous; in the most recent solar cycle,
  0.8- and 1.5-year periods dominated the power spectrum. This anomaly is
  believed to be caused by changes in solar magnetic asymmetry over time.

Title: On a possible relation of the law of planetary distances to
    the 160-minute pulsation of the sun.
Authors: Kotov, V. A.; Koutchmy, S.
Bibcode: 1985IzKry..72..199K
Altcode:
  The discovery of the global solar pulsation with the period of
  P<SUB>0</SUB> = 160<SUP>m</SUP> enables to introduce characteristic
  wavelength L = c×P<SUB>0</SUB> = 19.24 A.U. for the solar system,
  where c is the speed of light. A corresponding analysis of planetary
  distances reveals the existence of a statistically significant
  quasi-commensurability between L and 2πa<SUB>i</SUB> for inner planets
  and between 2a<SUB>i</SUB> and L for outer ones (a<SUB>i</SUB> being
  the major semi-axis of a planetary orbit). It is suggested that this
  L-commensurability can offer new approach to an explanation of the
  well-known Titius-Bode law for planetary distances. The physical
  mechanism enforcing the L-commensurability in the solar system is
  presumably related with 160<SUP>m</SUP>-gravitational waves from some
  external source of unknown nature.

Title: The 160-min period in the solar system: solar pulsation and
    the spin rates of planets and asteroids
Authors: Kotov, V. A.; Koutchmy, S.
Bibcode: 1985BCrAO..70...37K
Altcode: 1985BuCri..70...37K; 1987BCrAO..70...37K
  No abstract at ADS

Title: Solar oscillations with a 160-min period and other long period
solar oscillations: analysis of the power spectrum of nine-year
    observations and their interpretation
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1985BCrAO..71....1S
Altcode: 1985BCrAO..71....3S
  No abstract at ADS

Title: A possible relation between planetary distances and the
    160-minute solar pulsation.
Authors: Kotov, V. A.; Koutchmy, S.
Bibcode: 1985BCrAO..72..171K
Altcode: 1985BuCri..72..171K; 1987BCrAO..72..171K
  No abstract at ADS

Title: The search for a 160-min period in sequences of X-ray bursts
    and chromospheric flares of the sun
Authors: Kasinskii, V. V.; Kotov, V. A.; Levitskii, L. S.; Fomin, V. P.
Bibcode: 1985IzKry..73...43K
Altcode:
  Statistical analysis of 533 hard X-ray bursts of the sun, recorded by
  the Japanese satellite Hinotori in 1981 in the 17-40 keV range, reveals
  a 160-min modulation with a confidence level of 98 percent. This finding
  is confirmed by SMM satellite data where an analogous periodicity is
  found at a 93 percent confidence level. The superposed epoch method,
  applied to the time sequence of 16,000 solar flares with importance
  B greater than or equal to 1 also reveals a 160-min modulation
  with a 99 percent level of confidence. It is proposed that the
  chromospheric perturbation induced by the global 160-min oscillations
  can statistically trigger the occurrence of solar flares. However, this
  effect is nearly insignificant (85 percent confidence) in the case of
  strong (importance B greater than or equal to 2) flares, but highly
  significant (99.9 percent) in the case of weak (B = 1) flares. The
  peak amplitude of modulation of flare occurrences is about 7 percent.

Title: Period of 160 minutes in the solar system: solar pulsation
    and spin rates of planets and asteroids.
Authors: Kovtchmy, S.; Kotov, V. A.
Bibcode: 1985IzKry..70...38K
Altcode:
  It is proposed that the close correspondence between the period of
  solar global pulsation (160 min) and the 9th and 4th harmonics of
  the rotational periods of the earth and Saturn respectively cannot
  be fortuitous. To test this hypothesis, a commensurability function
  is examined, and the level of statistical certainty of the result is
  determined. An analysis of commensurability with the period of solar
  global pulsation was extended to all available data on the rotation of
  planets and asteroids, and it is shown that quasi-commensurability with
  this 160-min period is both dominant and statistically significant. The
  probability of randomly obtaining such a quasi-commensurability is
  equal to about 0.00001. On these grounds, it is proposed that there is
  (or was in the past) some gravitational coupling between those main
  bodies of the solar system having a 160-min period; this process could
  have resulted from a periodic variation of the gravitational field.

Title: A search for the 160-min period in sequences of solar X-ray
    bursts and chromospheric flares.
Authors: Kotov, V. A.; Kasinskij, V. V.; Levitskij, L. S.; Fomin, V. P.
Bibcode: 1985BCrAO..73...40K
Altcode: 1987BCrAO..73...40K
  No abstract at ADS

Title: Global solar oscillations observed from relative near-IR
    photosphericbrightness fluctuations.
Authors: Kotov, V. A.; Koutchmy, S.; Kononovich, Eh. V.; Ryzhikova,
   N. N.; Tsap, T. T.
Bibcode: 1985BCrAO..73...24K
Altcode: 1987BCrAO..73...24K
  No abstract at ADS

Title: Solar oscillations with a period of 160 min and other
    long-period oscillations - Analysis of the power spectrum during
    nine years of observations and interpretation
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1985IzKry..71....3S
Altcode:
  Doppler-velocity observations are used to investigate the power spectrum
  of solar oscillations in the 110-210-min periodicity range. In order
  to eliminate all power peaks of nonsolar origin, the present spectrum
  is compared with an analogous power spectrum computed on the basis
  of simultaneous telluric O2 6879-A line observations. This comparison
  reveals that 39 of the peaks may indeed have their origin in the sun;
  20 of these were compared with the theoretical periods of 'dirty' solar
  models (Christensen-Dalsgaard et al., 1979) whereby enrichment with
  heavy elements via accretion from interstellar space has occurred. Ten
  of the observed periods agree well with the periods of g-modes. One
  variation of the 'dirty' solar model (C) is characterized by a shallow
  convective zone and a low neutrino flux of 1.7 SNU.

Title: Unbalance in the Sun's general magnetic field: anomalies in
    the interplanetary magnetic field in 1970-1981
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1985BCrAO..71...31K
Altcode: 1985BuCri..71...31K
  No abstract at ADS

Title: Global oscillations of the sun according to observations of
    (relative) fluctuations of photospheric brightness in the near
    infrared
Authors: Koutchmy, S.; Kononovich, E. V.; Ryzhikova, N. N.; Kotov,
   V. A.; Tsap, T. T.
Bibcode: 1985IzKry..73...26K
Altcode:
  The instrument designed for monitoring of relative center-to-limb
  brightness fluctuations of the photosphere in near IR spectral range (λ
  = 1.65 μm) is described. Analysis of 67 days of observations carried
  out in 1981 - 1982 shows clearly the presence of 160-min variations of
  the differential, center-to-limb intensity with an average amplitude
  of about 3×10<SUP>-5</SUP> in units of the {average solar} brightness
  near 1.65 μm or 0.2K in terms of the temperature of the photosphere.

Title: Ten years observations of long-period oscillations of the Sun
Authors: Kotov, V. A.; Severny, A. B.; Tsap, T. T.
Bibcode: 1984ESASP.220..189K
Altcode: 1984ESPM....4..189K
  The measurements of Doppler shift of a Fraunhofer spectral line were
  performed over 10 yr. The power spectrum of the data shows a major peak
  at 160m period which is interpreted as multiple resonance of gravity
  modes of the Sun. This 160m oscillation reveals remarkable phase
  stability during the entire decade. It is noted that true pattern
  of the power spectrum can be seriously spoiled by Earth sources of
  noise. The importance of analysis of oscillations seen in a telluric
  line is emphasized.

Title: 160-minute and other long-period oscillations of the sun
    Analysis and interpretation of 9-year observations
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1984MmSAI..55..117K
Altcode:
  Besides the persistent 160-min oscillation Crimean observations show
  the presence of 10 or more other long-period oscillations interpreted
  as gravity g-modes.

Title: On Commensurability of the Axial Periods of Cometary Nuclei
    Rotation with the 160-MINUTE Period
Authors: Kotov, V. A.; Tarashchuk, V. P.
Bibcode: 1984ATsir1318....1K
Altcode:
  No abstract at ADS

Title: The 160-min pulsation period in the SMM solar hard X-ray
    burst data
Authors: Kasinskij, V. V.; Kotov, V. A.
Bibcode: 1984PAZh...10..235K
Altcode:
  Data on 2100 25-350-keV solar X-ray bursts obtained by the
  hard-X-ray-burst spectrometer of the SMM satellite (Wagner, 1982)
  over its entire period of operation in 1980-1981 and 400 1-min
  SMM observations of the 3.2-A line of Ca XIX on June 24-28, 1980,
  are analyzed statistically in terms of possible effects of the
  160.010-min solar pulsations reported by Severnyi et al. (1976) and
  Kotov et al. (1983). The power spectrum of the Ca XIX measurements
  is calculated and plotted, and the superposed-epochs technique is
  applied to the burst observations. Both sets of data are shown to
  found to exhibit intensity modulations with the 160-min period; the
  significance of the burst periodicity is determined as about 0.001.

Title: The 160-MINUTE Pulsation Period in the Solar Maximum Mission
    Solar Hard X-Ray Burst Data
Authors: Kasinski, V. V.; Kotov, V. A.
Bibcode: 1984SvAL...10...98K
Altcode:
  No abstract at ADS

Title: Periodic variations in the solar magnetic field?
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1984BCrAO..69...84K
Altcode: 1986BCrAO..69...84K
  No abstract at ADS

Title: Periodic variations of the solar magnetic field
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1984IzKry..69...90K
Altcode:
  Dominant recurrent periods - or rotation periods - of the mean
  solar magnetic field have been studied using the polarity of the
  interplanetary magnetic field (IMF, 1926 - 1981) as inferred from polar
  geomagnetic observations and direct measurements of the magnetic field
  of the sun seen as a star (1968 - 1981). The power spectra of these data
  reveal a set of discrete lines associated with 27 - 29 days (synodic)
  periods of the solar rotation. The most prominent peaks, in particular
  those at 26.95, 27.20, 27.38 and 28.21 days periods, exhibit remarkable
  phase-coherency over 56 years. It is suggested that these discrete lines
  (periods) belong to certain latitudinal zones on the sun where the
  magnetic field rotates coherently and almost independently (in regard
  to the phase) of the 11-years cycle and of the polar field reversals
  occurring near epochs of the solar activity maxima. In addition, the
  present analysis of 56 years of the IMF polarity shows the existence
  of a strong annual variation which appears to be, in the main part,
  a by-product of the well-known Rosenberg-Coleman's effect in the IMF
  predominant polarity.

Title: Power spectrum of long-period solar oscillations and 160-min
    pulsations during 1974-82
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1984Natur.307..247S
Altcode:
  We report here the results of solar oscillation observations carried
  out between 1974 and 1982 using the Crimean solar magnetograph. We
  have eliminated all peaks of telluric origin from the mean power
  spectrum; of the remaining 32 dominant (&gt;=2σ) peaks, 19 are
  of solar origin and 13 are partly blended with the atmospheric
  peaks. We found that 10 solar peaks are in very good agreement with
  the modes g<SUB>10</SUB>-g<SUB>20</SUB> of degree 1 = 4 calculated by
  Christensen-Dalsgaard et al.<SUP>1</SUP> for the solar model C with
  the envelope enriched in heavy elements by accretion. Deviations of the
  observed long-period oscillations from a linearity can be appreciable,
  leading to the appearance of combination frequencies. The dominant
  160-min peak seems to be excited by a strong `double' resonance
  of 2g<SUB>8</SUB> mode of model C with a combination frequency,
  and two other combination frequencies of modes 1g<SUB>1</SUB> and
  2f including the unstable mode l = 1. As model C is also in good
  agreement with the neutrino experiment, we suggest that this could
  be considered as the most appropriate model of the Sun. In contrast
  to previous detailed studies of solar pulsation with the particular
  160.01-min period<SUP>2,3</SUP>, the emphasis here is on the search for
  other possible long-period solar oscillations of low degree. These
  oscillations are thought to be bound to the regions beneath the
  convection zone and penetrate to the Sun's core which makes them
  a powerful tool for analysing the solar internal structure and the
  evolution of the Sun.

Title: A review of the present state of gravity modes oscillations
    of the sun
Authors: Severnyi, A. B.; Kotov, V. A.
Bibcode: 1984AdSpR...4h.129S
Altcode: 1984AdSpR...4..129S
  Short review of ground-based observations of the Sun and of solar
  gravity modes detection is presented with the emphasize on 160m
  oscillation as predominant, long-time phase-coherent oscillation. The
  limitations imposed by the influence of Earth's atmosphere and
  geoseismic waves on observations of solar oscillations are pointed out
  together with a necessity of the observations of solar oscillations
  with the aid of space-probes.

Title: Measurements of the solar 160 min oscillation at the Metsaehovi
    radio research station in 1980-1982 and comparison with the results
    at the Crimean Astrophysical Observatory
Authors: Urpo, S.; Teraesranta, H.; Holsti, N.; Tiuri, M.; Kotov,
   V.; Nesterov, N.
Bibcode: 1983STIN...8419268U
Altcode:
  The results of solar 160 min oscillation measurements at 8 mm and 13.5
  mm wavelengths are compared with optical and radio observations. Results
  confirm the existence of this oscillation also at radio frequencies.

Title: Simultaneous registration of the 160-min pulsations of the
    sun with two radio telescopes.
Authors: Nesterov, N. S.; Urpo, S.; Kotov, V. A.
Bibcode: 1983PAZh....9..312N
Altcode:
  Observations of the center-limb differential solar brightness
  obtained at 13.5 mm (using the 22-m radio telescope at the Crimean
  Astrophysical Observatory) and at 8.15 mm (using the 13.7-m radio
  telescope at Helsinki University) on June 22, 1981, are presented
  and compared. An expression for determining the time evolution of
  the brightness temperature is derived and applied, and a plot of the
  processed data is shown. A 160-min variation is observed in both cases,
  with agreement to within 0.05 period. A fourfold difference in amplitude
  is attributed either to the wavelength difference or to an imperfect
  match of the areas of the sun observed.

Title: The 160-MINUTE Solar Pulsation Recorded Simultaneously by
    Two Radio Telescopes
Authors: Nesterov, N. S.; Urpo, S.; Kotov, V. A.
Bibcode: 1983SvAL....9..166N
Altcode:
  No abstract at ADS

Title: Observation of global 160-min infrared (differential) intensity
    variation of the Sun
Authors: Kotov, V. A.; Koutchmy, S.; Koutchmy, O.
Bibcode: 1983SoPh...82...21K
Altcode: 1983IAUCo..66...21K
  The method developed and the instrument designed for detecting
  variations of the solar limb darkening at the atmospheric transparency
  window of the solar opacity minimum region of λ 1.65 μ are
  described. This differential technique proved to be successful in
  rejecting undesirable low frequency noises due to the atmosphere
  and to the instrument. Analysis of observations made in 1977, 1978,
  and 1981 indicates the persistance of global fluctuations of the IR
  differential, center-to-limb intensity at the wellknown 160 min period
  with an average amplitude of about ± 2 × 10<SUP>-4</SUP> in units
  of the `average Sun' intensity near 1.65 μm.

Title: Dominating periods of rotation of the general magnetic field
    of the sun.
Authors: Kotov, V. A.; Levitskij, L. S.
Bibcode: 1983ppsf.conf...94K
Altcode:
  No abstract at ADS

Title: 160-Minute oscillations in the 13.5 mm circularly polarized
    radiation from the Sun
Authors: Efanov, V. A.; Kotov, V. A.; Moiseev, I. G.; Nesterov, N. S.;
   Severnyi, A. B.
Bibcode: 1983BCrAO..67...98E
Altcode: 1985BCrAO..67...98E
  No abstract at ADS

Title: The discreteness of the rotation periods of the solar and
    interplanetary magnetic fields
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1983IzKry..68...56K
Altcode:
  The rotation of solar magnetic fields during 1954-1980 has been
  investigated using data sets for the polarity of the interplanetary
  magnetic field (IMF) and measurements of the mean magnetic field
  of the sun for 1968-1980. Each data set used in the analysis was
  treated as a single time series. The power spectra of the fields
  show a set of discrete peaks near the solar rotation period of 27-28
  days. The most significant peaks were well reproduced in both the IMF
  and SMMF spectra. It is shown that neither sampling effects nor the
  interference of the 27-28-day variations in the long-term evolution
  of the IMF and SMMF can account for the concentration of power in the
  discrete lines. The solar magnetic fields at high latitudes (40-50 deg)
  appear to contribute significantly to the SMMF as measured by a solar
  magnetograph, and to the IMF observed at earth orbit.

Title: A study of the global oscillations of the sun. II - Results
    of observations in 1974-1980, their analysis and conclusions
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1983IzKry..66....3K
Altcode:
  A superposed-epoch analysis of the differential radial velocity of
  the sun covering a 7-year period (1974-1980), supported by a power
  spectrum analysis, shows the presence of oscillations with a period of
  160.01 m and an amplitude of about 0.5 m/s. Four other statistically
  significant oscillations (with periods of 134.5, 148.4, 171.1, and
  175.1 m) are shown to exist up to 1977. These, however, are thought
  to be transient phenomena, whereas the 160.01-m oscillations persist
  over the entire 7-year period, with the mean amplitude varying from
  year to year. In addition to sporadic fluctuations, the amplitude of
  the 160.01-m oscillations exhibits periodic variability with a sun
  rotation period of about 27.2 d. The factors supporting the solar
  origin of the 160.01-m oscillations are discussed.

Title: Long-term coherent periodicities in the mean magnetic field
    of the sun
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1983IAUS..102...23K
Altcode:
  The present investigation is concerned with periodic variations of the
  magnetic field of the sun as a star, taking into account mean field
  measurements in the Crimea, Mt. Wilson, and Stanford observatories. A
  total of 5783 daily values was available for the time interval from 1968
  to 1981. The data provide a unique possibility to study the sun as a
  variable magnetic star. In connection with the objective to combine the
  three data sets into a single time series, the original measurements of
  each observatory were corrected for the systematic calibration error,
  giving attention to the application of correction factors determined on
  the basis of an intercomparison of the three individual power spectra.

Title: A study of solar global oscillations. II. Results of
    observations in 1974-1980, their analysis, and some conclusions
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1983BCrAO..66....1K
Altcode: 1985BCrAO..66....1K
  No abstract at ADS

Title: Discrete solar rotation frequencies deduced from the solar
    and interplanetary magnetic fields
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1983BCrAO..68...50K
Altcode: 1985BCrAO..68...50K
  No abstract at ADS

Title: Variations of the interplanetary and solar magnetic fields
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1983IzKry..66..110K
Altcode: 1983IzKry..66Q.110K
  The authors determine time variations of the interplanetary magnetic
  field (IMF) observed near the earth and of the mean magnetic field of
  the sun seen as a star (SMMF) for 1968-1979. All the values of IMF and
  SMMF were 28-day averaged to eliminate the dependence on solar rotation;
  also the yearly means were calculated. It is shown that in contrast
  to the yearly average magnitude of the IMF which is almost constant
  throughout the solar cycle, that of the SMMF changes markedly from year
  to year (by 3-4 times). The analysis reinforces the previous conclusion
  (1981) on the presence of a significant annual variation in the SMMF
  with amplitude of about 0.1 Gs. It is suggested that some asymmetry
  of the global magnetic field of the sun in inertial (with respect to
  stars) space can be responsible for this annual effect as observed
  from the earth. The annual wave in the IMF magnitude is only marginally
  significant, ⪉3%, demonstrating once more quite different behaviour of
  the IMF and SMMF on a month-year time scale. The discrepancy is thought
  mainly to be the result of different averaging of two physical fields.

Title: The 160-min variation of circularly polarized solar radio
    emission at a wavelength of 13.5 MM
Authors: Efanov, V. A.; Kotov, V. A.; Moiseev, I. G.; Nesterov, N. S.;
   Severnyi, A. B.
Bibcode: 1983IzKry..67..111E
Altcode:
  Variations of the circularly polarized radio emission of the sun
  with period of 160 min and amplitude of about 2×10<SUP>-5</SUP> are
  detected at 13.5 mm wavelength. They exhibit phase-coherence (with
  about 34<SUP>m</SUP> delay-time) with the global 160-min oscillations
  of the sun seen in the velocity of the photosphere and might be related
  to synchronous changes of the solar general magnetic field.

Title: Manifestation of the 160-MIN Solar Oscillations in Velocity
    and Brightness - Optical and Radio Observations
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.; Moiseev, I. G.;
   Efanov, V. A.; Nesterov, N. S.
Bibcode: 1983SoPh...82....9K
Altcode: 1983IAUCo..66....9K
  All evidence of the solar origin of 160-min period oscillations is
  collected, and the present state of observations of this oscillation in
  optical and radio-ranges is considered. The main results are summarized:
  (a) the 160-min oscillation was observed in 1981 as well as before,
  (b) an attempt to find a nonradial component with l = 2 has failed,
  (c) the intensity and circular polarization of radioemission show with
  statistical significance the presence of this 160-min periodicity.

Title: Time variations of the interplanetary and solar magnetic fields
Authors: Kotov, V. A.; Levitskii, L. S.
Bibcode: 1983BCrAO..66..100K
Altcode: 1985BCrAO..66..100K
  No abstract at ADS

Title: Potential Models of the Unipolar Sunspot Magnetic Field
Authors: Denisenko, V. V.; Kotov, V. A.; Romanov, V. A.; Sokolov, V. S.
Bibcode: 1982SoPh...81..217D
Altcode:
  The potential models of the unipolar sunspot magnetic field are
  calculated on the basis of magnetographic measurements of the magnetic
  field made in the three spectral lines of different intensities, Hα,
  CaI λ6103 and FeI λ4808. The computed distributions of the magnetic
  field vector are compared with actual distributions observed at these
  three levels. It is shown that the electric current density in the
  spot reaches values up to 10<SUP>5</SUP> CGSE in the volume contained
  between formation depths of two pairs of lines, FeI λ4808-CaI λ6103
  and FeI λ4808 - Hα. Therefore, the magnetic field of the spot
  deviates strongly from a potential configuration. To the contrary, at
  higher levels, in the semi-infinite volume restricted at the bottom
  by the hydrogen Hα-line, the field appears to be quite close to a
  potential one.

Title: An investigation of the global oscillations of the sun:
    1. Methods and instruments
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1982BCrAO..65....1K
Altcode: 1982BuCri..65....1K; 1984BCrAO..65....1K
  No abstract at ADS

Title: Study of solar global oscillations. I - Method and instrument
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1982IzKry..65....3K
Altcode:
  The present investigation is concerned with a method for the
  measurement of the Doppler shift of the position of the spectral
  line Fe I lambda 5124 A, averaged over the central zone of the solar
  disk, with respect to the mean position of the same line for the limb
  region. The statistical accuracy of the measurement of the velocity
  is approximately + or - 0.2 m/sec. The historical background regarding
  the considered measurements is discussed along with the Crimean Solar
  Tower Telescope and the magnetograph employed in the measurements,
  the study of the sun in a parallel beam, and the method used to measure
  the solar global oscillations. Attention is given to questions regarding
  the accuracy of the method, errors related to the instrument, aspects of
  guidance and stability, possible errors due to the electronics system,
  and an evaluation of the effects of the errors on the accuracy of the
  results obtained with the aid of the considered method.

Title: Present State of the Study of 160-MINUTES Solar Oscillation
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1981SoPh...74...65S
Altcode:
  Global oscillation of the Sun with a period of 160 rain were first
  discovered in 1974 and since observed in Crimea during the last 6 years;
  they were confirmed, in 1976-1979, by Doppler measurements at Stanford
  (Scherrer et al., 1980) and quite recently by observations of Fossat
  and Grec at the south geographic pole. The average amplitude of the
  oscillation is about 0.5 m s<SUP>-1</SUP>. The phase shows remarkable
  stability at the period 160.010 min and good agreement between different
  sites on the Earth; therefore, this oscillation should now be recognized
  as definitely of solar origin. It is probably accompanied by synchronous
  fluctuations in the IR brightness and radio-emission of the Sun, and
  exhibits a dependence of the amplitude on the phase of solar rotation
  (with a peak of power at 27.2 days).

Title: Annual variation of the mean magnetic field of the sun
Authors: Kotov, V. A.; Levitskii, L. S.; Stepanyan, N. N.
Bibcode: 1981BCrAO..63....1K
Altcode: 1981BuCri..63....1K
  No abstract at ADS

Title: Annual variation of the solar mean magnetic field.
Authors: Kotov, V. A.; Levitskii, L. S.; Stepanian, N. N.
Bibcode: 1981IzKry..63....3K
Altcode:
  The paper examines observations of the solar mean magnetic field
  (SMMF) made during 1968-1978 at the Crimean, Mt. Wilson, and Stanford
  observatories. An analysis of the data clearly shows an annual variation
  of the SMMF with an amplitude of about 0.1 G, and it is argued that
  this periodicity can be attributed neither to instrumental nor to
  seasonal causes. It is noted that the heliolatitude effect cannot
  be used to explain this periodicity, and that there are unexplained
  phase differences between annual variations of the SMMF and the sun's
  polar field. The nature of the annual variation of the SMMF is left
  unresolved.

Title: Global Oscillations of the Sun
Authors: Severny, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1981IGAFS..56...11S
Altcode:
  No abstract at ADS

Title: Detection of 160 min solar intensity variations: sampling
    effects.
Authors: Koutchmy, S.; Koutchmy, O.; Kotov, V. A.
Bibcode: 1980A&A....90..372K
Altcode:
  The theory that the 2 h 40 min period in the Crimean and Stanford
  global solar velocity oscillation measurements may have resulted
  partly by 1-day sampling is verified using the IR center-limb
  intensity variations measurements. It was shown that (1) the power
  spectrum of these data has a peak near the 2 h 40 min period, and (2)
  the power spectra of the series with the observing windows 'filled'
  with a constant do not manifest a significant peak at the 9th harmonic
  of the day. It was concluded that the analysis of the really observed
  data is not biased by the influence of data windows and 1-day sampling
  regularity of observations.

Title: Detection of 160-min solar oscillations and atmospheric
    extinction
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1980A&A....88..317S
Altcode:
  The influence of the earth's atmosphere on the search for global solar
  oscillations with a period of 160m is studied. It is shown that neither
  the amplitude nor the phase behavior of the oscillations persisting
  during the last five years (1974-1978) can be explained in terms of
  the terrestrial atmospheric influences or by the statistical method
  of treatment. The observational evidence strongly suggests that the
  160m periodicity is of solar origin.

Title: Further evidence of solar oscillations with a period of
    160 minutes
Authors: Scherrer, P. H.; Wilcox, J. M.; Severnyi, A. B.; Kotov,
   V. A.; Tsap, T. T.
Bibcode: 1980ApJ...237L..97S
Altcode:
  Observations made at the Crimean Astrophysical Observatory and the
  Stanford Solar Observatory during 1979 provide evidence of the existence
  of oscillations of the sun with a period near 160 minutes. The new
  observations showed the same period with a phase of maximum expansion
  as predicted from earlier data; for 1979 the time of maximum expansion
  of the center of the solar disk was found to be 01:55 UT for the Crimean
  observatories and 01:58 UT for Stanford with a phase uncertainty of plus
  or minus 15 minutes. In addition, a new regression line can be found
  which yields a period of 160.01 minutes or a drift in phase of 31.5
  minutes per year in an analysis at exactly 160 minutes. The continued
  agreement in phase (and amplitude) between the two observatories
  for four years, as well as the fact that the period of oscillations
  determined differs from exactly one-ninth of a day, supports the
  interpretation that solar oscillations are indeed being observed.

Title: The Effect of the Equation of Time on the 160-MINUTE Solar
    0SCILLATION
Authors: Kotov, V. A.; Koutchmy, S.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1980SvAL....6..233K
Altcode:
  No abstract at ADS

Title: Certain characterisitics of the large-scale magnetic fields
    of the Sun
Authors: Kotov, V. A.; Stepanyan, N. N.
Bibcode: 1980BCrAO..62...96K
Altcode: 1980BuCri..62...96K
  No abstract at ADS

Title: Solar pulsations.
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1980HiA.....5..453S
Altcode:
  Observations of solar oscillations with a period of approximately 160
  min are discussed. The oscillations were detected independently in 1974,
  1976, 1978 and 1979, with a high phase coherence between observation
  times. The amplitude of the oscillations is found to depend on the
  phase of solar rotation, and a slow drift of the phase of maximum
  is observed, leading to an estimate of a period of 160.010 min. The
  period may be interpreted by a variety of pulsation modes while the
  spherical harmonic l is not known, however the observed dependence of
  oscillation amplitude on solar rotation phase can be accounted for by
  the rotational splitting of the S1(m) mode at l = 2. The oscillations
  have also been observed to disappear and reappear with nearly the same
  phase, and may offer the possibility of a means of energy transport
  other than radiative.

Title: Certain characteristics of large-scale magnetic fields on
    the sun
Authors: Kotov, V. A.; Stepanian, N. N.
Bibcode: 1980IzKry..62..117K
Altcode:
  The characteristics are obtained by comparing the sun's general
  magnetic field, measured with a magnetograph, with the background field,
  determined on the basis of H-alpha maps. The average intensity of the
  magnetic field in the photosphere is found to be approximately 2.2
  gauss. The intensity in the regions occupied by the S field is somewhat
  greater than in the regions of the N field. During the years 1973-1976,
  the primary period for the rotation of the large-scale fields was
  approximately 27.04-27.15 d; in 1976-1978, two period were observed,
  26.75 d and 29.30 d. This is seen as the result of a shift toward the
  equator of the large-scale structures of the magnetic field of the
  old 11-year cycle and the formation of the high-latitude structures
  of a new cycle. It is also found that the background field in the N
  hemisphere, on the average, is positive (approximately +0.14 gauss),
  whereas in the S hemisphere it is negative (approximately -0.14
  gauss). In the southern hemisphere, the magnetic structures are found
  to rotate somewhat faster than in the northern hemisphere. It is noted
  that this would be the case if the structures in the S hemisphere were
  closer to the equator than in the N hemisphere.

Title: The magnetic field of the Sun as a star, 1969-1976
Authors: Kotov, V. A.; Demidov, M. L.
Bibcode: 1980BCrAO..61....1K
Altcode:
  No abstract at ADS

Title: Shaking Down the Sun's Long-Period Vibes
Authors: Kotov, V. A.; Severny, A. B.; Tsap, T. T.; Scherrer, P. H.;
   Wilcox, J. M.; Fossat, E.; Grec, G.; Pomerantz, M.
Bibcode: 1980SciN..118..100K
Altcode:
  No abstract at ADS

Title: The magnetic field of the sun as a star, 1969-1976
Authors: Kotov, V. A.; Demidov, M. L.
Bibcode: 1980IzKry..61....3K
Altcode:
  A superposed epoch analysis of the mean solar magnetic field measured in
  the Crimea during 1969-1976 was performed using approximately 215 sector
  boundaries of the interplanetary magnetic field. The mean field displays
  a sector structure, with a typical field strength within a sector of
  0.4-0.3 G. The average magnitude of the mean field decreased from 0.5
  G in 1969-1970 to 0.15 G in 1975-1976. The principal recurrence period
  in the data is 27.04 d + or - 0.06 d. The resulting curve reflects
  the asymmetry between magnetic fields of opposite sign (the duration
  of S polarity is 3-4 days greater than that of the N polarity).

Title: Solar oscillations and the problem of the internal structure
    of the sun
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1979SvA....23..641S
Altcode: 1980SvA....23..641S
  No abstract at ADS

Title: Solar oscillations and the problem of the internal structure
    of the sun
Authors: Severny, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1979AZh....56.1137S
Altcode:
  Observations of solar oscillations made over a period of five years
  are reviewed, and implications of the observations for the physics
  of the solar interior are indicated. An analysis of over 1000 hours
  of solar observations from 1974 to 1978 is presented which shows the
  observed oscillations of the solar radius to be real, with a period of
  160.010 + or - 0.004 min and a Doppler shift amplitude of 1 m/sec. The
  slow drift of the phase of the velocity maximum has been observed,
  together with the dependence of the amplitude on the phase of the
  solar rotation period. Synchronous oscillations of the solar magnetic
  field and radio emission have also been found to be synchronous to
  the brightness oscillations, and the oscillations have been seen to
  disappear occasionally, possibly due to the passage of a supergranule
  across the solar disk. It is suggested that the oscillations represent
  gravitational quadrupole oscillations, and could serve as a means for
  nonradiative heat transfer from within the sun and thus alleviate the
  problem of low neutrino flux.

Title: Solar radio pulsations of 160-min period observed at 1.9-3.5 CM
Authors: Eryushev, N. N.; Kotov, V. A.; Severnyij, A. B.; Tsvetkov,
   L. I.
Bibcode: 1979PAZh....5..546E
Altcode:
  Centimeter-wavelength measurements of solar radio emission with
  the 22-m Crimean radio telescope during 1977-1978 have revealed
  fluctuations in the relative (center/limb) radio brightness with a
  160-min period and an amplitude of approximately 0.001. They correspond
  to brightness-temperature variations of plus or minus approximately
  10 K and are synchronized with the 160-min global pulsations of the
  solar surface.

Title: Solar Radio Pulsations of 160-MIN Period Observed at 1.9-CM
    and 3.5-CM
Authors: Eryushev, N. N.; Kotov, V. A.; Severnyi, A. B.; Tsvetkov,
   L. I.
Bibcode: 1979SvAL....5..292E
Altcode:
  No abstract at ADS

Title: Observations of solar oscillations with periods of 160 minutes
Authors: Scherrer, P. H.; Wilcox, J. M.; Kotov, V. A.; Severny, A. B.;
   Tsap, T. T.
Bibcode: 1979Natur.277..635S
Altcode:
  Severny et al. (1976) have reported oscillations of the sun with
  a period near 160 min. A description is presented of observations
  made at the Stanford Solar Observatory during the time from 1975 to
  the present which seem to support the reports by Severny et al. At
  Stanford the relative velocity between a central circular area of
  radius 0.5 solar radius on the solar disk and most of the remaining
  area of the solar disk is measured. A superposed epoch analysis of
  the observations using a period of 160 min is discussed. An apparent
  agreement in phase between the obtained observational data and those
  reported by Severny et al. tends to support the interpretation that
  solar oscillations are being observed.

Title: Observations of oscillations of the Sun.
Authors: Kotov, V. A.; Severnyi, A. B.; Tsap, T. T.
Bibcode: 1978MNRAS.183...61K
Altcode:
  Evidence is presented which shows that a previously observed 160-min
  oscillation in the solar surface and certain other periodic oscillations
  that have persisted for three years are of intrinsic solar origin and
  cannot be ascribed to any possible sources of error in observations or
  measurements. A method is described which involves measurement of the
  relative Doppler shift between a spectral line from the whole central
  portion of the solar disk and the same line produced by the whole outer
  rim of the disk. Results are discussed for applications of this method
  to the magnetically insensitive line of Fe I at 5123.7 A. Various
  analyses of the data obtained are performed, possible sources of
  systematic error are eliminated, and it is demonstrated that significant
  periods of solar oscillation exist, the most significant being 160
  min. Attempts made to detect oscillations in mean solar magnetic fields
  and brightness as well as in the brightness of Uranus are noted.

Title: Further Progress in Observations of Solar Oscillations
Authors: Severny, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1978pfsl.conf..123S
Altcode: 1978ESPM....2..123S
  No abstract at ADS

Title: Measurements of the solar limb-darkening in the 1 - 4 µm
    range.
Authors: Koutchmy, S.; Koutchmy, O.; Kotov, V.
Bibcode: 1977A&A....59..189K
Altcode:
  Radial scans in selected spectral regions near the opacity minimum,
  in both equatorial and polar directions, have been performed for the
  purpose of obtaining improved values for the limb darkening of the very
  undisturbed quiet solar atmosphere. Equipment and correction procedures
  are described. The new data are compared with earlier values, and the
  HSRA model is found to be inadequate for predicting values near the
  opacity minimum. The data are more in accord with the new model M of
  Vernazza et al. (1976) and also with the BCA model. No pole-equator
  difference of limb darkening due to the presence of faint faculae
  was found.

Title: The mean magnetic field of the sun: method of observation
    and relation to the interplanetary magnetic field.
Authors: Scherrer, P. H.; Wilcox, J. M.; Kotov, V.; Severnyi, A. B.;
   Howard, R.
Bibcode: 1977SoPh...52....3S
Altcode:
  The mean solar magnetic field as measured in integrated light has
  been observed since 1968. Since 1970 it has been observed both at
  Hale Observatories and at the Crimean Astrophysical Observatory. The
  observing procedures at both observatories and their implications for
  mean field measurements are discussed. A comparison of the two sets
  of daily observations shows that similar results are obtained at both
  observatories. A comparison of the mean field with the interplanetary
  magnetic polarity shows that the IMF sector structure has the same
  pattern as the mean field polarity.

Title: Polarization of light appearing on mirrors of a tower solar
    telescope.
Authors: Kotov, V. A.
Bibcode: 1977IzKry..56..150K
Altcode:
  No abstract at ADS

Title: Contribution of the background magnetic field and fields of
    active regions and spots to the general magnetic field of the sun.
Authors: Kotov, V. A.; Stepanian, N. N.; Shcherbakova, Z. A.
Bibcode: 1977IzKry..56...75K
Altcode:
  No abstract at ADS

Title: Observations of solar pulsations
Authors: Severnyi, A. B.; Kotov, V. A.; Tsap, T. T.
Bibcode: 1976Natur.259...87S
Altcode:
  We have modified our solar magnetograph to measure velocities at the
  solar surface, rather than magnetic fields. Using this apparatus, we
  have observed fluctuations of period 2 h 40 min, which are remarkably
  stable. The interpretation of this phenomenon seems to cause much
  theoretical difficulty.

Title: The rotation of matter in a sunspot.
Authors: Kotov, V. A.
Bibcode: 1976IzKry..54..184K
Altcode:
  Radial velocities in a sunspot are derived from magnetographic
  measurements of the Fe I lines at 4808 and 5250 A, the Ca I line at
  6103 A, and the H-alpha line. It is found that the gas in the sunspot
  rotates in a cyclonic sense at a mean velocity of about 0.25 km/s in
  the photosphere and in an anticyclonic sense at a mean velocity of about
  -1.3 km/s in the chromosphere, which agrees with the behavior expected
  for a sunspot in the southern hemisphere. Measurements of three lines
  with different intensities are reported which might indicate a slight
  increase in tangential velocity with depth, and the vortex structure
  of mass-flow lines and magnetic lines of force is discussed. It is
  suggested that the observation of gas rotation in opposite directions
  in the photosphere and chromosphere should be taken into account in
  a proposed model for the transformation of rotational kinetic energy
  into electromagnetic energy of the current system.

Title: Observations of Oscillations of the Entire Sun
Authors: Kotov, V. A.; Severny, A.; Tsap, T.
Bibcode: 1976IAUTB..16..244K
Altcode: 1976IAUT...16B.244K
  No abstract at ADS

Title: Enhancement of magnetic fields, radio brightness at
    mm-wavelengths and Halpha -activity at the polar regions of the sun.
Authors: Babin, A. N.; Gopasiuk, S. I.; Efanov, V. A.; Kotov, V. A.;
   Moiseev, I. G.; Nesterov, N. S.; Tsap, T. T.
Bibcode: 1976IzKry..55....3B
Altcode:
  No abstract at ADS

Title: Measurements of the magnetic field from different spectral
    lines.
Authors: Gopasyuk, S. I.; Kotov, V. A.; Severnyj, A. B.; Tsap, T. T.
Bibcode: 1975IzKry..53..247G
Altcode:
  No abstract at ADS

Title: The interpretation of the total magnetic vector measurements
    in sun spots
Authors: Kotov, V. A.
Bibcode: 1974STIN...7527993K
Altcode:
  A large change in the magnetic field with depth in the spot was
  found on the basis of the total vector (H) measurements at two levels
  corresponding to the depths of the line formations lambda 5250 A Fe
  and lambda 6103 A Ca. The spiralling of the horizontal field and its
  rotation with depth were observed where the vertical field increases
  with height. The densities of the vertical and horizontal electric
  currents in the spot are equal to approximately 5000 and approximately
  100,000 CGSE respectively. The discrepancy between the height gradients
  of the vertical field inside the spot was obtained from the measured
  vertical field at two levels and from the use of the equation div H =
  O. This discrepancy may be attributed to the difference between the very
  high resolution at depth and the low resolution on the sun's surface.

Title: An investigation of the transversal magnetic field in sunspots.
Authors: Kotov, V. A.
Bibcode: 1974IzKry..51...39K
Altcode:
  The effect of transverse magnetic field rotation with depth is examined
  with the aid of sunspot magnetograms obtained in the 4808-A and 5250-A
  Fe I lines, the 6103-A Ca I line, and the H-alpha line. The results
  show a significant change (45 to 90 deg) in the orientation of the
  transverse magnetic field in different sunspot regions. Stronger
  rotation was observed in umbrae, but more detailed measurements are
  needed to confirm this. The depth behavior of the transverse magnetic
  field is analyzed, and it is found that rotation is more pronounced
  in the deeply formed 4808-A line than in the others. The 5250-A line
  is apparently formed in the uppermost sunspot layers. Observations of
  rotation in northern and southern hemispheric sunspots are found not
  to contradict the dependence of rotation direction on magnetic field
  polarity, which follows from the Zeeman-effect theory with allowance
  for anomalous dispersion.

Title: The Comparison of the Magnetographic Magnetic Field Measured
    in Different Spectral Lines
Authors: Gopasyuk, S. I.; Kotov, V. A.; Severny, A. B.; Tsap, T. T.
Bibcode: 1973SoPh...31..307G
Altcode:
  The discrepancies in the values of longitudinal magnetic field
  obtained from magnetographic records in different spectral lines
  are considered. On the basis of extensive data including 60 pairs of
  magnetographic maps for 11 spectral lines, obtained simultaneously
  for one of these lines and λ6103 with the aid of the Crimean double
  channel magnetograph, the following conclusions have been reached. The
  relative field strength (6103) depends partly on the distance from the
  center of the disk (Figure 4) and mainly on the magnetic sensitivity
  of the line gλ<SUP>2</SUP> (Figure 3), pointing to the primary role
  of saturation effect. The possible influence of line asymmetry on
  these discrepancies is also suggested.

Title: On the influence of instrumental polarization on magnetic
    field measurements.
Authors: Kotov, V. A.
Bibcode: 1973IzKry..48...78K
Altcode:
  No abstract at ADS

Title: On the calibration of photoelectric measurements of a
    magnetic field.
Authors: Kotov, V. A.
Bibcode: 1973IzKry..47...14K
Altcode:
  No abstract at ADS

Title: Measurements of the Transverse Magnetic Field in the
    Chromosphere above a Sunspot.
Authors: Kotov, V. A.
Bibcode: 1972SvA....15..687K
Altcode:
  No abstract at ADS

Title: On the interpretation of total magnetic vector measurements
    in sunspots.
Authors: Kotov, V. A.
Bibcode: 1972IzKry..46..115K
Altcode:
  No abstract at ADS

Title: The systematic errors of the total vector H of magnetic field
    measurements with the Crimean Astrophysical Observatory magnetograph.
Authors: Kotov, V. A.
Bibcode: 1972IzKry..44...77K
Altcode:
  No abstract at ADS

Title: Measurements of the Transverse Magnetic Field in the
    Chromosphere above a Sunspot.
Authors: Kotov, V. A.
Bibcode: 1971AZh....48..869K
Altcode:
  No abstract at ADS

Title: Systematic Errors of the Crimean Vector Magnetograph (presented
    by a. Severny)
Authors: Kotov, V. A.
Bibcode: 1971IAUS...43...71K
Altcode:
  No abstract at ADS

Title: On the Structure of Magnetic Field and Electric Currents of
    a Unipolar Sunspot (presented by a. Severny)
Authors: Kotov, V. A.
Bibcode: 1971IAUS...43..212K
Altcode:
  No abstract at ADS

Title: A Comparison of Simultaneous Measurements of the Polar Magnetic
    Fields Made at the Crimea and Mount Wilson
Authors: Kotov, V. A.; Stenflo, J. O.
Bibcode: 1970SoPh...15..265K
Altcode:
  Measurements of the polar magnetic fields of the sun made in August
  1968 with the Crimean and Mt Wilson magnetographs are compared. The
  agreement between the results obtained at the two observatories is
  rather satisfactory. The correlation coefficient between the Crimean
  and Mt Wilson values of the observed average field strength at different
  latitudes is 0.7 for the north and 0.5 for the south polar region. The
  earlier conclusion based on the Mt Wilson material that a polarity
  reversal of the field occurred at latitudes +70° and -55° in the north
  and south hemispheres (Stenflo, 1970) is confirmed by the Crimean data.

Title: Magnetic field and electric currents of a unipolar sunspot.
Authors: Kotov, V. A.
Bibcode: 1970IzKry..41...67K
Altcode:
  No abstract at ADS

Title: The magnetic field of a solar prominence.
Authors: Kotov, V. A.
Bibcode: 1969IzKry..39..276K
Altcode:
  No abstract at ADS

