Author name code: bruzek
ADS astronomy entries on 2022-09-14
author:"Bruzek, Anton" 
------------------------------------------------------------------------  

Title: Der Mond - Ein Atlas des Mondes, veröffentlicht in
    Zusammenarbeitmit der Royal Astronomical Society.
Authors: Moore, P.; Bruzek, A.
Bibcode: 1982demo.book.....M
Altcode:
  No abstract at ADS

Title: Landolt-Börnstein. Numerical data and functional
relationships in science and technology. New series. Group VI:
    Astronomy, astrophysics and space research. Volume_2. Astronomy and
astrophysics. Extension and supplement to Volume_1. Subvolume a:
    methods - constants - solar system.
Authors: Hellwege, K. -H.; Schaifers, K.; Voigt, H. H.; Wolf, R.;
   Durrant, C. J.; Behr, A.; West, R. M.; Solf, J.; Weigelt, G.; Schmahl,
   G.; Staubert, R.; Trümper, J.; Lemke, D.; Hachenberg, O.; Enslin, H.;
   Fricke, W.; Bruzek, A.; Gondolatsch, F.; Ip, W. -H.; Axford, W. I.;
   Schubart, J.; Jessberger, E. K.; Rahe, J.; Fechtig, H.; Leinert, C.;
   Grün, E.; Pilipp, W.; Scholer, M.; Palme, H.; Suess, H. E.; Zeh,
   H. D.; Kirsten, T.
Bibcode: 1981lndf.book.....H
Altcode:
  No abstract at ADS

Title: On a Peculiar Type of Filament Activation
Authors: Bruzek, A.
Bibcode: 1980IAUS...91..203B
Altcode:
  No abstract at ADS

Title: Post-flare Hα plage formation
Authors: Bruzek, A.
Bibcode: 1979SoPh...61...35B
Altcode:
  Observations on the permanent transformation during a flare of a fibril
  region into a stable plage region are presented and interpreted as
  flare-associated re-orientation of the chromospheric magnetic field.

Title: Small scale motions in the chromosphere and in the corona.
Authors: Bruzek, A.
Bibcode: 1979ssms.conf...79B
Altcode:
  No abstract at ADS

Title: Flares and Associated Phenomena
Authors: Dodson-Prince, H. W.; Bruzek, A.
Bibcode: 1977ASSL...69...81D
Altcode: 1977igss.conf...81D
  Solar Flare Thermal Flare Flare Area Flare Importance or Flare Class
  Comprehensive Flare Index (CFI) Flash Phase Flare Kernels Plage Flare
  Two-Ribbon Flare Filament-Associated Flares Homologous Flares Limb
  Flares Flare-Associated Phenomena Moreton Wave White-Light Flare X-Ray
  Flare Hard X-Ray Flare EUV Bursts Flare Gamma Ray Emission Particle
  Flare or Energetic Flare Flare Mechanisms

Title: Illustrated glossary for solar and solar terrestrial physics
Authors: Bruzek, A.; Durrant, C. J.
Bibcode: 1977ASSL...69.....B
Altcode: 1977igss.conf.....B; 1977assl...69.....B
  This book collects all terms of relevance to solar and solar-terrestrial
  physics that appear in current English-language literature. Each
  term or group of related terms is given a concise phenomenological
  and quantitative description, including the relationship to other
  phenomena and an interpretation in terms of physical processes. The
  major topics of the glossary encompass the solar interior, the solar
  cycle, solar rotation, large-scale circulation, nonspot magnetic
  fields, the quiet photosphere and chromosphere, the transition
  region, the solar corona, active regions, spots and faculae, flares
  and associated phenomena, prominences, solar radio emission, the
  solar wind and interplanetary medium, solar-terrestrial physics,
  and general theoretical terms. Specific terms defined include solar
  neutrinos, convective theory, the solar activity cycle, dynamos,
  the general solar magnetic field, the quiet sun, granulation and
  supergranulation, coronal holes, sunspot groups, solar activity
  indexes, the Evershed and Wilson effects, X-ray flares, EUV bursts,
  particle flares, prominence phenomenology, radio noise storms, solar
  radio bursts, macro/microturbulence, solar-wind models, geomagnetic
  indexes, geomagnetic storms, radiation belts, and aurorae.

Title: Spots and Faculae
Authors: Bruzek, A.
Bibcode: 1977ASSL...69...71B
Altcode: 1977igss.conf...71B
  Photospheric Faculae Facular Point Polar Faculae Magnetic Knots Moving
  Magnetic Features (MMF) Pore Sunspot Umbra Umbral Dots Umbral Flashes
  Umbral Oscillations Light Bridges Penumbra Penumbral Waves Evershed
  Effect Wilson Effect

Title: Active Regions
Authors: Martres, M. J.; Bruzek, A.
Bibcode: 1977ASSL...69...53M
Altcode: 1977igss.conf...53M
  (Solar) Activity Active Region Complexes of Activity Emerging Flux
  Regions Ephemeral Region Sunspot Group Proper Motion (of Sunspots)
  Evolving Magnetic Features (EMF) Parasites or Inclusions Magnetic
  Inversion Line Filament Channel or Plage Couloir Chromospheric Plage
  Fibrils Moustache (Ellerman Bomb) Magnetic Classification of Active
  Regions Mt. Wilson Spot Classification Solar Activity Indices Solar
  Activity Data

Title: Pre-Flare Energy Storage (title only)
Authors: Bruzek, A.
Bibcode: 1976SoPh...47..215B
Altcode:
  No abstract at ADS

Title: Book reviews
Authors: de Jager, C.; van Rensbergen, Walter; Kuperus, M.; Falthammar,
   Carl-Gunne; Mewe, R.; Reunen, G. C. M.; Bruzek, A.; Swanenburg,
   B. N.; Kleczek, J.; Millman, Peter M.; Vesseur, H. J. A.; Pacini,
   F.; Monfils, A.
Bibcode: 1976SSRv...18..541D
Altcode:
  No abstract at ADS

Title: Solar activity (Activité solaire).
Authors: Newkirk, G.; Dunn, R. B.; Mehltretter, P.; MacQueen, R.;
   Bonnet, R. M.; White, O. R.; Fokker, A. D.; Zwaan, C.; Bruzek, A.;
   Durrant, C.; Grossmann-Doerth, U.; Mehltretter, J. P.; Svestka, Z.;
   de Feiter, L. D.; Tandberg-Hanssen, E.; Howard, R.; Stix, M.; Pneuman,
   G. W.; Hundhausen, A. J.; Sawyer, C.; Simon, P.
Bibcode: 1976IAUTA..16b..13N
Altcode:
  No abstract at ADS

Title: Solar Active Regions and Periodicities in Solar Activity
Authors: Bruzek, A.
Bibcode: 1976IAUTA..16...27B
Altcode: 1976IAUT...16...27B
  No abstract at ADS

Title: K.-O. Kiepenheuer, 1910 November 10 - 1975 May 23.
Authors: Bruzek, A.
Bibcode: 1975SoPh...43....3B
Altcode:
  No abstract at ADS

Title: In memoriam
Authors: Bruzek, A.
Bibcode: 1975SoPh...43....2B
Altcode:
  No abstract at ADS

Title: Changes of the Hα Fibril Pattern during Solar Flares
Authors: Bruzek, A.
Bibcode: 1975SoPh...42..215B
Altcode:
  A pattern of parallel Hα fibrils inside a network cell changed into
  a pattern of vertical or radial flbriles after a flare had covered the
  region. This may be evidence for a change of the magnetic configuration
  during flare occurrence.

Title: K.-O. Kiepenheuer, 1910 November 10 - 1975 May 23.
Authors: Bruzek, A.
Bibcode: 1975S&W....14..352B
Altcode:
  No abstract at ADS

Title: The solar flare activity at the beginning of July 1974
Authors: Bruzek, A.
Bibcode: 1975KlBer..18..179B
Altcode:
  A survey of the unexpectedly high flare activity of July, 1974, is
  given. The flares occurred in a large spot group which developed and
  decayed quickly during its passage across the solar disk. Its magnetic
  configuration was rather complex with strong umbral magnetic fields and
  a high-gradient delta-configuration. The maximum optical importance of
  the flares was 2B while the associated X-ray bursts reached extremely
  high intensities, in one case 1 erg/sq cm-sec in the 1 - 8 A band. Two
  proton events with enhanced fluxes in the energy ranges below 30 MeV
  and below 60 MeV, respectively, were observed. The development of the
  presumable proton flare of July 3, 1974, is briefly discussed.

Title: Book reviews
Authors: de Jager, C.; Bruzek, A.
Bibcode: 1974SoPh...34..507D
Altcode:
  No abstract at ADS

Title: Optical Evidence for Plasma Ejections and Waves in the
    Solar Corona
Authors: Bruzek, A.
Bibcode: 1974IAUS...57..323B
Altcode:
  No abstract at ADS

Title: Über das Moustache-Phänomen
Authors: Bruzek, A.
Bibcode: 1973MitAG..32..187B
Altcode:
  No abstract at ADS

Title: Solar Activity
Authors: Bruzek, A.
Bibcode: 1973lsp2.conf...39B
Altcode:
  No abstract at ADS

Title: Lectures on Space Physics 1: Cosmic Rays and Space Biophysics
Authors: Bruzek, Anton; Pilkuhn, Hartmut
Bibcode: 1973lsp1.conf.....B
Altcode: 1973lsp1.book.....B
  No abstract at ADS

Title: Lectures on Space Physics 2: Sun and Interplanetary Medium,
    Relativistic Astrophysics
Authors: Bruzek, Anton; Pilkuhn, Hartmut
Bibcode: 1973lsp2.conf.....B
Altcode: 1973lsp2.book.....B
  No abstract at ADS

Title: Some Observational Results on Moustaches
Authors: Bruzek, Anton
Bibcode: 1972SoPh...26...94B
Altcode:
  The results of new observations of moustaches in Hα filtergrams and
  in Hα spectra are presented and their relations to photospheric and
  chromospheric phenomena are studied. The main findings and conclusions
  are: (1) previous results on basic data (size, brightness, lifetime,
  etc.) are essentially confirmed; (2) limb observations located the
  moustaches at the base of the structured Hα chromosphere, just
  above the level of the emission of Hα±1 Å. At the disk moustaches
  are, in general, covered by absorbing and slightly Doppler-shifted
  chromospheric elements which determine the Hα core in the moustache
  spectrum. However, absorption-free moustaches with an Hα emission core
  revealing a pure (true) moustache spectrum have also been found; (3)
  moustaches have been found to coincide with continuous facular granules;
  it is suggested that they are an extension of facular granules into
  the chromosphere rather than a low-level flare-like phenomenon.

Title: On the Relation between Filaments (Prominences) and Hα Loops
Authors: Bruzek, Anton
Bibcode: 1972SoPh...24..118B
Altcode:
  The relation between occurrence of Hα loops and filaments is discussed
  on the occasion of the observation of a new type of transient loops
  during a flare associated filament activation. Considering all known
  types of loop systems crossing neutral lines it is concluded that
  concurrent existence of stable filaments and Hα loops is incompatible.

Title: Physics of Solar Prominences. Report on an International
    Colloquium Held at the German Solar Observatory, Anacapri, September
    29 to October 1, 1971
Authors: Bruzek, Anton; Kuperus, Max
Bibcode: 1972SoPh...24....3B
Altcode:
  This colloquium on solar prominences - the first ever held -
  has shown that a major part of activity in prominence research in
  recent years concentrated on both observation and computation of the
  magnetic conditions which were found to play a crucial role for the
  development and the maintainance of prominences. Remarkable progress
  was made in fine-scale measurements of photospheric magnetic fields
  around filaments and in internal field measurements in prominences. In
  addition, important information on the structure of the magnetic fields
  in the chromosphere adjacent to the filaments may be derived from high
  resolution photographs of the Hα fine structure around filaments
  which have become available recently; unfortunately, an unambiguous
  determination of the vector field in the chromosphere is not yet
  possible. <P />It is quite clear, now, that stable filaments extend
  along `neutral' lines which divide regions of opposite longitudinal
  magnetic fields. Different types of neutral lines are possible,
  depending on the history and relationship of the opposite field
  regions. There is convincing evidence that the magnetic field in the
  neighbouring chromosphere may run nearly parallel to the filament
  axis and that there are two field components in stable prominences:
  an axial field dominant in the lower parts and a transverse field
  dominant in the higher parts. <P />Methods for the computation of
  possible prominence field configurations from measured longitudinal
  photospheric fields were developed in recent years. In a number of
  cases (e.g. for loop prominences) the observed configuration could
  be perfectly represented by a force-free or even a potential field;
  poor agreement was found between computed and measured field strengths
  in quiescent prominences. In order to reconcile both of them it is
  necessary to assume electric currents. Unambiguous solutions will not
  be found until measurements of the vector field in the photosphere
  and in the prominences are available. <P />The two-dimensional
  Kippenhahn-Schlüter model is still considered a useful tool for the
  study of prominence support and stability. However, a more refined
  model taking into account both field components and considering also
  thermal stability conditions is available now. It was proposed that
  quiescent prominences may form in magnetically neutral sheets in
  the corona where fields of opposite directions meet. <P />As for
  the problem of the origin of the dense prominence material there
  are still two opposite processes under discussion. The injection of
  material from below, which was mainly applied to loop prominences, has
  recently been considered also a possible mechanism for the formation of
  quiescent prominences. On the other hand, the main objections against
  the condensation mechanism could be removed: it was shown that (1)
  sufficient material is available in the surrounding corona, and that
  (2) coronal matter can be condensed to prominence densities and cooled
  to prominence temperatures in a sufficiently short time. <P />The energy
  balance in prominences is largely dependent on their fine structure. It
  seems that a much better radiative loss function for optically thin
  matter is now available. The problem of the heat conduction can only
  be treated properly if the field configuration is known. Very little is
  known on the heating of the corona and the prominence in a complicated
  field configuration. For the optically thick prominences the energy
  balance becomes a complicated radiative transfer problem. <P />Still
  little is known on the first days of prominence development and on
  the mechanism of first formation which, both, are crucial for the
  unterstanding of the prominence phenomenon. As a first important step,
  it was shown in high resolution Hα photographs that the chromospheric
  fine structure becomes aligned along the direction of the `neutral'
  line already before first filament appearance. More Hα studies and
  magnetic field measurements are badly needed. <P />Recent studies
  have shown that even in stable prominences strong small-scale internal
  rotational or helical motions exist; they are not yet understood. On the
  other hand, no generally agreed interpretation of large-scale motions of
  prominences seems to exist. A first attempt to explain the ascendance
  of prominences, the `Disparitions Brusques', as the result of a kink
  instability was made recently. <P />New opportunities in prominence
  research are offered by the study of invisible radiations: X-rays and
  meterwaves provide important information, not available otherwise,
  on physical conditions in the coronal surroundings of prominences;
  EUV observations will provide data on the thin transition layer between
  the cool prominence and the hot coronal plasma.

Title: Properties of solar active regions.
Authors: Bruzek, A.
Bibcode: 1972sstp.conf...49B
Altcode:
  No abstract at ADS

Title: Properties of Solar Active Regions
Authors: Bruzek, A.
Bibcode: 1972ASSL...29...49B
Altcode: 1972sun..conf...49B
  No abstract at ADS

Title: Flare Associated Coronal Expansion Phenomena
Authors: Bruzek, Anton; Demastus, Howard L.
Bibcode: 1970SoPh...12..447B
Altcode:
  Two classes of coronal expansion phenomena have been studied
  in Sacramento Peak coronal movies: Slow, slightly decelerated
  expansion phenomena (v=∼10− =∼ 2 km/sec) and fast, accelerated,
  quasi-exploding arches (v =∼ 10 - &gt; 100 km/sec). The various
  phenomena were found to be associated with flares in different ways:
  The slow expansions were long lived post-flare phenomena initiated by
  the flare; the accelerated expanding arches were either (a) arches
  expanding prior to and apparently exploding at flare onset, or (b)
  arches apparently emerging from the flare (probably in its initial
  phase) and rapidly expanding and exploding, or (c) the expansion and
  disruption of (originally stable) coronal arches during occurrence of
  a distant flare. These expansions may be considered as evidence for
  corresponding flare associated changes in the coronal magnetic field.

Title: Motions in Arch Filament Systems
Authors: Bruzek, A.
Bibcode: 1969SoPh....8...29B
Altcode:
  A new analysis of Hα filtergrams and Hα spectra of arch filament
  systems (AFS) shows that material flows downwards in both branches
  of the arch filaments (v ≈ 50 km/sec) while the top of the arches
  ascends (v ≲ 10 km/sec). It is suggested that AFS are produced by
  the magnetic field which expands, between growing spots, into higher
  levels carrying material with it that subsequently slides down along
  the magnetic field following gravity.

Title: Flare associated optical phenomena
Authors: Bruzek, A.
Bibcode: 1969sfsr.conf...61B
Altcode:
  No abstract at ADS

Title: Koronale Expansionsphänomene
Authors: Bruzek, A.
Bibcode: 1969MitAG..27..211B
Altcode:
  No abstract at ADS

Title: Strukturen um Sonnenflecken.
Authors: Bruzek, A.
Bibcode: 1969Umsch..69..212B
Altcode:
  No abstract at ADS

Title: Solar flares
Authors: Bruzek, A.
Bibcode: 1969pia..conf...71B
Altcode:
  No abstract at ADS

Title: Flares in the active region during the proton flare period
    of July 1966.
Authors: Bruzek, A.
Bibcode: 1969AIQSY...3...82B
Altcode:
  No abstract at ADS

Title: Dynamik von Hα Feinstrukturen in aktiven Gebieten der Sonne
Authors: Bruzek, A.
Bibcode: 1968MitAG..25..189B
Altcode:
  No abstract at ADS

Title: Bright Points (moustaches) and Arch Filaments in Young
    Active Regions
Authors: Bruzek, A.
Bibcode: 1968IAUS...35..293B
Altcode:
  No abstract at ADS

Title: On small-scale mass motion associated with flares
Authors: Bruzek, A.
Bibcode: 1968mmsf.conf...67B
Altcode:
  No abstract at ADS

Title: On Arch-Filament Systems in Spotgroups
Authors: Bruzek, A.
Bibcode: 1967SoPh....2..451B
Altcode:
  Systems of arch-shaped filaments (AFS) occurring in the interspot region
  of young bipolar groups are studied. Their main characteristics are:
  Average length: 30000km, average width 20000km, width of individual
  filaments 1000-3000 km, height of arches 4-15000 km. A typical lifetime
  of the filaments 30 min; appreciable changes of the system occur
  within several hours; the lifetime of a system is about three days. -
  The arch-filament systems bridge the `neutral' line and connect the
  regions of the innermost spots of opposite polarity. Material moves
  along the filaments (v ∼ 25-50 km/sec) following the direction of the
  magnetic field, and sometimes arches are observed rising at a rate of
  ∼ 20 km/sec. They are very dark on the inner disk and appear either in
  emission or in absorption close to the solar limb. - The occurrence of
  `bright points' (moustaches) is found to be closely associated with AFS
  in young spotgroups. - The possible nature of AFS and their relation
  to other types of filamentary structures is discussed.

Title: Physics of Solar Flares: The Energy and Mass Problem
Authors: Bruzek, A.
Bibcode: 1967sp...conf..399B
Altcode:
  No abstract at ADS

Title: Das Flare-Phänomen auf der Sonne
Authors: Bruzek, A.
Bibcode: 1966MitAG..21....7B
Altcode:
  No abstract at ADS

Title: On the Association Between Loop Prominences and Flares.
Authors: Bruzek, A.
Bibcode: 1964ApJ...140..746B
Altcode:
  The evolution of loop prominence systems (LPS) and their relation to
  flares were studied using Ha observations from the solar limb and the
  solar disk. The limb observations show that a small LPS may start to
  develop from a flare knot several minutes after flare onset. The LPS's
  then grow discontinuously at a rate of the order of 10 km/sec by the
  formation of higher and higher loops which attain maximum heights
  of 40000 up to 150000 km (average valu , 83000 km); they have a
  characteristic lifetime of 12 hours. All LPS's so far detected on the
  disk (25 cases) were closely ?elated to major flares of the twostrand
  expanding type which produced strong SSWF effects (100 per cent), Type
  IV bursts (95 per cent), and PCA effects (85 per cent). Depending on
  their position the LPS's appeared on the disk in various shapes and with
  different delay times after flare onset; they were visible either in
  emission or in absorption. The observations strongiy suggest that the
  LPS's are part of a powerful flare event and are due to a propagation
  of the flare process into the solar corona. A model of the evolution
  bf the combined flare-loop system is derived from the observations.

Title: Optical Characteristics of Cosmic Ray and Proton Flares
Authors: Bruzek, Anton
Bibcode: 1964JGR....69.2386B
Altcode:
  In recent years several attempts have been made to find characteristic
  properties of the optical manifestations of flare events that produce
  the energetic protons which generate cosmic-ray increases at ground
  level (GLE) and polar-cap absorption effects (PCA). In a study1 of 9
  flares which were followed by a PCA effect Dodson and Hedeman [1962]
  recognized that in each of these cases part of the Ha flare covered
  the umbra of a large spot. Ellison et al. [1961] noticed that all
  cosmic-ray flares which had been well observed on the solar disk
  (7 cases) consisted of two roughly parallel bright strands which
  covered partly or completely the largest umbras of the associated spot
  group. Avignon et al. [1963] found a similar arrangement of the flare
  filaments in 13 out 15 PCA flares.

Title: Case Histories of Flares: The Large Flares of July 11, 12,
    18, and 20, 1961
Authors: Bruzek, A.
Bibcode: 1964NASSP..50..301B
Altcode: 1964psf..conf..301B
  No abstract at ADS

Title: The Influence of Flares on the Associated Permanent Coronal
    Condensation
Authors: Bruzek, A.
Bibcode: 1963IAUS...16..137B
Altcode:
  No abstract at ADS

Title: Über Fleckenprotuberanzen vor der Sonnenscheibe. Mit 4
    Textabbildungen
Authors: Bruzek, A.
Bibcode: 1962ZA.....54..225B
Altcode:
  No abstract at ADS

Title: Über die Umlaufgeschwindigkeit der polaren Filamente. Mit
    2 Textabbildungen
Authors: Bruzek, A.
Bibcode: 1961ZA.....51...75B
Altcode:
  No abstract at ADS

Title: Beobachtungen über die Beziehungen zwischen Eruptionen und
    Fleckenfeldern. Mit 4 Textabbildungen
Authors: Bruzek, A.
Bibcode: 1960ZA.....50..110B
Altcode:
  No abstract at ADS

Title: Über die Spiculen auf der Sonnenscheibe. Mit 2 Textabbildungen
Authors: Bruzek, A.
Bibcode: 1959ZA.....47..191B
Altcode:
  No abstract at ADS

Title: Die Filamente und Eruptionen eines Aktivitätszentrums. Mit
    6 Textabbildungen
Authors: Bruzek, A.
Bibcode: 1958ZA.....44..183B
Altcode:
  No abstract at ADS

Title: Über eruptionsartige Fackeln bei Filamentaufstiegen. Mit
    5 Textabbildungen
Authors: Bruzek, A.; Becker, U.
Bibcode: 1957ZA.....42...76B
Altcode:
  No abstract at ADS

Title: Die Korona-Emissionsgebiete und ihre Beziehungen zu
    Sonnenflecken und Fackeln. Mit 15 Textabbildungen.
Authors: Bruzek, A.
Bibcode: 1955ZA.....35..213B
Altcode:
  No abstract at ADS

Title: Die Mitte-Rand-Variation der H<SUB>α-</SUB>-Linienbreite,
    der H<SUB>α-</SUB> Zentralintensität und der Flächen der
    Eruptionen. Mit 4 Textabbildungen
Authors: Bruzek, A.
Bibcode: 1955ZA.....38....1B
Altcode:
  No abstract at ADS

Title: Beziehungen zwischen Protuberanzen und monochromatischer
    Korona. Mit 5 Textabbildungen
Authors: Bruzek, A.
Bibcode: 1955ZA.....35..265B
Altcode:
  No abstract at ADS

Title: Die hypothetische Neigung der Sonnenfleckenachsen. Mit 4
    Textabbildungen
Authors: Bruzek, A.
Bibcode: 1953ZA.....33..267B
Altcode:
  No abstract at ADS

Title: On a type of flare associated with ascendant dark filaments
Authors: Bruzek, A.
Bibcode: 1952Obs....72..154B
Altcode:
  No abstract at ADS

Title: Über die Ursache der ''Plötzlichen" Filamentauflösungen. Mit
    4 Textabbildungen
Authors: Bruzek, A.
Bibcode: 1952ZA.....31...99B
Altcode:
  No abstract at ADS

Title: Die Ausbreitung von "Euptionsstörungen". Mit 2 Textabbildungen
Authors: Bruzek, A.
Bibcode: 1952ZA.....31..111B
Altcode:
  No abstract at ADS

Title: Beobachtungen über das Verhalten von Filamenten während
    chromosphärischer Eruptionen. Mit 7 Textabbildungen
Authors: Bruzek, A.
Bibcode: 1951ZA.....28..277B
Altcode:
  No abstract at ADS

