Author name code: goldberg
ADS astronomy entries on 2022-09-14
author:Goldberg, L.
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Title: A new estimate of galaxy mass-to-light ratios from flexion
    lensing statistics
Authors: Fabritius, Joseph M.; Goldberg, David M.
Bibcode: 2022MNRAS.515.6191F
Altcode: 2022MNRAS.tmp.2142F; 2021arXiv210805453F
  We perform a flexion-based weak gravitational analysis of the first two
  Hubble Frontier Field clusters: Abell 2744 and MACS 0416. A parametric
  method for using radially projected flexion signals as a probe of
  cluster member mass is described in detail. The normalization and slope
  of a L - θ<SUB>E</SUB> (as a proxy for L - σ) scaling relation in
  each cluster is determined using measured flexion signals. A parallel
  field analysis is undertaken concurrently to provide a baseline measure
  of method effectiveness. We find an agreement in the Faber-Jackson
  slope ℓ associated with galaxy age and morphology for both clusters,
  as well as a theoretical distinction in the cluster normalization mass.

Title: Shock Breakout in Three-dimensional Red Supergiant Envelopes
Authors: Goldberg, Jared A.; Jiang, Yan-Fei; Bildsten, Lars
Bibcode: 2022ApJ...933..164G
Altcode: 2022arXiv220604134G
  Using Athena++, we perform 3D radiation-hydrodynamic calculations of
  the radiative breakout of the shock wave in the outer envelope of a
  red supergiant (RSG) that has suffered core collapse and will become
  a Type IIP supernova. The intrinsically 3D structure of the fully
  convective RSG envelope yields key differences in the brightness
  and duration of the shock breakout (SBO) from that predicted in a 1D
  stellar model. First, the lower-density "halo" of material outside
  of the traditional photosphere in 3D models leads to a shock breakout
  at lower densities than 1D models. This would prolong the duration of
  the shock breakout flash at any given location on the surface to ≍1-2
  hr. However, we find that the even larger impact is the intrinsically 3D
  effect associated with large-scale fluctuations in density that cause
  the shock to break out at different radii at different times. This
  substantially prolongs the SBO duration to ≍3-6 hr and implies a
  diversity of radiative temperatures, as different patches across the
  stellar surface are at different stages of their radiative breakout
  and cooling at any given time. These predicted durations are in
  better agreement with existing observations of SBO. The longer
  durations lower the predicted luminosities by a factor of 3-10 (L
  <SUB>bol</SUB> ~ 10<SUP>44</SUP> erg s<SUP>-1</SUP>), and we derive
  the new scalings of brightness and duration with explosion energies
  and stellar properties. These intrinsically 3D properties eliminate
  the possibility of using observed rise times to measure the stellar
  radius via light-travel time effects.

Title: Numerical Simulations of Convective Three-dimensional Red
    Supergiant Envelopes
Authors: Goldberg, Jared A.; Jiang, Yan-Fei; Bildsten, Lars
Bibcode: 2022ApJ...929..156G
Altcode: 2021arXiv211003261G
  We explore the three-dimensional properties of convective, luminous (L
  ≍ 10<SUP>4.5</SUP>-10<SUP>5</SUP> L <SUB>⊙</SUB>), hydrogen-rich
  envelopes of red supergiants (RSGs) based on radiation hydrodynamic
  simulations in spherical geometry using Athena++. These computations
  comprise ≍30% of the stellar volume, include gas and radiation
  pressure, and self-consistently track the gravitational potential for
  the outer ≍3M <SUB>⊙</SUB> of the simulated M ≍ 15M <SUB>⊙</SUB>
  stars. This work reveals a radius, R <SUB>corr</SUB>, around which
  the nature of the convection changes. For r &gt; R <SUB>corr</SUB>,
  though still optically thick, diffusion of photons dominates the energy
  transport. Such a regime is well studied in less luminous stars, but
  in RSGs, the near- (or above-)Eddington luminosity (due to opacity
  enhancements at ionization transitions) leads to the unusual outcome
  of denser regions moving outward rather than inward. This region of the
  star also has a large amount of turbulent pressure, yielding a density
  structure much more extended than 1D stellar evolution predicts. This
  "halo" of material will impact predictions for both shock breakout and
  early lightcurves of Type IIP supernovae. Inside of R <SUB>corr</SUB>,
  we find a nearly flat entropy profile as expected in the efficient
  regime of mixing-length theory (MLT). Radiation pressure provides
  ≍1/3 of the support against gravity in this region. Our comparisons
  to MLT suggest a mixing length of α = 3-4, consistent with the sizes
  of convective plumes seen in the simulations. The temporal variability
  of these 3D models is mostly on the timescale of the convective plume
  lifetimes (≍300 days), with amplitudes consistent with those observed
  photometrically.

Title: Hydrogeochemical modelling of origin, evolution and mechanisms
    controlling water resources quality in the Pra Basin (Ghana)
Authors: Manu, Evans; Kühn, Michael; Kempka, Thomas; Goldberg,
   Tatiana; Vieth-Hillebrand, Andrea; Rach, Oliver
Bibcode: 2021EGUGA..23.7800M
Altcode:
  Understanding the geochemistry of water resources is a prerequisite
  in the development of sustainable water resource management
  strategies. The Pra Basin is one of the few basins in Ghana with
  economic importance. The Basin is constituted by three river systems
  (Birim, Offin and Pra) and covers a total land size of approximately
  2,300 km2. It traverses several towns and serves as the main water
  supply for communities and industry. Currently, the quality of water
  resources in the Pra Basin especially surfacewaters have been affected
  negatively as a result of activities such as illegal mining (e.g.,
  the use of mercury for the extraction of gold), indiscriminate waste
  disposal, and poor farm management practices (e.g., inappropriate
  application of fertilizers and pesticides). Specific contaminants
  include mercury (Hg), arsenic (As), lead (Pb), iron (Fe), manganese
  (Mn), cadmium (Cd), selenium (Se), and nitrate (NO3). The Pra Basin
  is underlain by three rock formations, the Birimian Supergroup, the
  Tarkwain Formation and the granitoids. The mineral composition of
  the Birimian Supergroup comprises argillitic/pellitic sediment (plus
  or minus kerogen), sericite schist, and quartz-sericite schist. The
  granitoids comprise biotite (hornblende, muscovite), biotite gneiss,
  biotite schist, amphibolite partly of contact metamorphism, K-feldspar
  rich granitoid, two-mica or muscovite granite and monzonite, serecite
  schist, quartz-serecite, and garnet. The Tarkwaian rocks mineralogy
  also includes basaltic flow/subvolcanic rock and minor interbedded
  volcaniclastics, detrital sediment mainly sandstone and conglomerate
  ultramafic and minor mafic igneous rock. Samples of groundwater were
  collected from shallow (mainly hand-dug wells of depths &lt; 10 m)
  and deep (mainly boreholes of depths &gt;30 m) aquifers across the Pra
  Basin. Surfacewaters were collected from rivers and stream networks. The
  samples were analysed for major ions, trace metals and stable isotopes
  (oxygen-18 and deuterium) using Inductively Coupled Plasma Optical
  Emission Spectrometry (ICP-OES), Ion Chromatography (IC), and Picarro
  L-2140i Ringdown Spectrometer at the GFZ laboratories. Multivariate
  statistical analysis and inverse geochemical modelling have been
  applied to around 100 water samples sourced from boreholes, hand-dug
  wells, and rivers of the Pra Basin to determine the chemical state
  of the waters. Specifically, the study seeks to (1) determine the
  origin and evolution of the geochemistry of both surfacewater and
  groundwater, (2) identify recharge and discharge areas, and (3)
  study sources and sinks of minerals including sulphates, carbonates,
  and silicates. The abundance of cations and anions are in the order
  of Na&gt;Ca&gt;K&gt;Mg and HCO3&gt;Cl&gt;SO4&gt;NO3 (surfacewater),
  Na&gt;Ca&gt;Mg&gt;K and HCO3&gt;Cl&gt;NO3&gt;SO4 (hand-dug well),
  and Na&gt;Ca&gt;Mg&gt;K, and HCO3&gt;Cl&gt;NO3&gt;SO4 (boreholes). Our
  research findings demonstrate that geochemistry of water resources in
  the Pra Basin is mainly controlled by rock-water interaction. With
  the application of hydrogeochemical modelling, including silicate
  mineral weathering and ion exchange, significant processes controlling
  the basin"s hydrochemistry variations are quantified. The presented
  results will support the development of sustainable water resources
  management strategies and contribute to mitigating future contamination.

Title: Evidence for α -cluster structure in <SUP>21</SUP>Ne in the
    first measurement of resonant <SUP>17</SUP>O+α elastic scattering
Authors: Nurmukhanbetova, A. K.; Goldberg, V. Z.; Nauruzbayev, D. K.;
   Golovkov, M. S.; Volya, A.
Bibcode: 2019PhRvC.100f2802N
Altcode:
  The first study of resonances in <SUP>17</SUP>O+α elastic scattering
  was carried out using the thick target inverse kinematics method. The
  data were analyzed in the framework of an R-matrix approach. Many α
  -cluster states were found in the <SUP>21</SUP>Ne excitation region
  of the 9-13 MeV excitation energy including the first observation of
  a broad l =0 state in an odd-even nucleus, which is likely the analog
  of the broad 0<SUP>+</SUP> at 8 MeV in <SUP>20</SUP>Ne. The observed
  structure in <SUP>21</SUP>Ne appeared to be strikingly similar
  to that populated in the resonant <SUP>16</SUP>O+α scattering in
  <SUP>20</SUP>Ne. The results are also useful for refinement of data
  on an <SUP>17</SUP>O(α ,n ) reaction important for astrophysics.

Title: LHC phenomenology and cosmology of string-inspired intersecting
    D-brane models
Authors: Anchordoqui, Luis A.; Antoniadis, Ignatios; Goldberg, Haim;
   Huang, Xing; Lüst, Dieter; Taylor, Tomasz R.; Vlcek, Brian
Bibcode: 2012PhRvD..86f6004A
Altcode: 2012arXiv1206.2537A
  We discuss the phenomenology and cosmology of a Standardlike Model
  inspired by string theory, in which the gauge fields are localized on
  D-branes wrapping certain compact cycles on an underlying geometry,
  whose intersection can give rise to chiral fermions. The energy
  scale associated with string physics is assumed to be near the
  Planck mass. To develop our program in the simplest way, we work
  within the construct of a minimal model with gauge-extended sector
  U(3)<SUB>B</SUB>×Sp(1)<SUB>L</SUB>×U(1)<SUB>I<SUB>R</SUB></SUB>×U(1)<SUB>L</SUB>.
  The resulting U(1) content gauges the baryon number B, the lepton number
  L, and a third additional Abelian charge I<SUB>R</SUB> which acts as
  the third isospin component of an SU(2)<SUB>R</SUB>. All mixing angles
  and gauge couplings are fixed by rotation of the U(1) gauge fields
  to a basis diagonal in hypercharge Y and in an anomaly-free linear
  combination of I<SUB>R</SUB> and B-L. The anomalous Z<SUP>'</SUP>
  gauge boson obtains a string scale Stückelberg mass via a 4D version
  of the Green-Schwarz mechanism. To keep the realization of the Higgs
  mechanism minimal, we add an extra SU(2) singlet complex scalar,
  which acquires a VEV and gives a TeV-scale mass to the nonanomalous
  gauge boson Z<SUP>''</SUP>. The model is fully predictive and can be
  confronted with dijet and dilepton data from LHC8 and, eventually,
  LHC14. We show that M<SUB>Z<SUP>''</SUP></SUB>≈3-4TeV saturates
  current limits from the CMS and ATLAS Collaborations. We also show
  that for M<SUB>Z<SUP>''</SUP></SUB>≲5TeV, LHC14 will reach discovery
  sensitivity ≳5σ. After that, we demonstrate in all generality that
  Z<SUP>''</SUP> milliweak interactions could play an important role
  in observational cosmology. Finally, we examine some phenomenological
  aspects of the supersymmetric extension of the D-brane construct.

Title: Neutrino Cosmology after WMAP 7-Year Data and LHC First
    Z<SUP>'</SUP> Bounds
Authors: Anchordoqui, Luis Alfredo; Goldberg, Haim
Bibcode: 2012PhRvL.108h1805A
Altcode: 2011arXiv1111.7264A
  The gauge-extended
  U(1)<SUB>C</SUB>×SU(2)<SUB>L</SUB>×U(1)<SUB>I<SUB>R</SUB></SUB>×U(1)<SUB>L</SUB>
  model elevates the global symmetries of the standard model (baryon
  number B and lepton number L) to local gauge symmetries. The
  U(1)<SUB>L</SUB> symmetry leads to three superweakly interacting
  right-handed neutrinos. This also renders a B-L symmetry
  nonanomalous. The superweak interactions of these Dirac states permit
  ν<SUB>R</SUB> decoupling just above the QCD phase transition:
  175≲T<SUB>ν<SUB>R</SUB></SUB><SUP>dec</SUP>/MeV≲250. In
  this transitional region, the residual temperature ratio between
  ν<SUB>L</SUB> and ν<SUB>R</SUB> generates extra relativistic degrees
  of freedom at BBN and at the CMB epochs. Consistency with both WMAP
  7-year data and recent estimates of the primordial He4 mass fraction
  is achieved for 3&lt;M<SUB>B-L</SUB>/TeV&lt;6. The model is fully
  predictive, and can be confronted with dijet and dilepton data from
  LHC7 and, eventually, LHC14.

Title: Supernova 2011dw in Pgc 58436 = Psn J16313945+4129229
Authors: Pelloni, A.; Newton, J.; Puckett, T.; Leonard, D. C.;
   Moustakas, J.; Swift, B. J.; McCarthy, D.; Bailey, V.; Carrico, E.;
   Carter, A.; Chui, E.; Douglas, E.; Eggeman, E.; Goldberg, R.; Grant,
   R.; Hartman, K.; Hellerstein, J.; Hooper, E.; Horlick-Cruz, C.; Hunter,
   L.; Jiles, T.; Johnson, E. D.; Kumar, K.; Lappe, L.; Lee, J.; Lee,
   W.; Marsh, F.; Mehta, G.; Miller, P.; Rampalli, R.; Reed, J.; Rice,
   K.; Saldivar, H.; Salgado-Flores, M.; Schlingman, A.; Scibelli, S.;
   Sinclair, K.; Steincamp, I.; Stock, N.; Todd, N.; Aizpuru Vargas,
   L. L.; Yamanaka, S.; Zachary, E.
Bibcode: 2011CBET.2756....1P
Altcode: 2011CBET.2756A...1P
  A. Pelloni, J. Newton, and T. Puckett report the discovery of
  an apparent supernova (mag 17.5) on an unfiltered CCD image
  (limiting mag 19.0) taken with a 0.35-m reflector at Portal, AZ,
  U.S.A., on June 24.3395 UT in the course of the Puckett Observatory
  Supernova Search. The new object, which was confirmed at mag 16.9
  on June 27.3391 by Puckett with the 40-cm reflector at Portal,
  is located at R.A. = 16h31m39.45 Decl. = +41o29'22".9 (equinox
  2000.0), which is 17".3 east and 14".0 south of the center of PGC
  58436. Nothing is visible at this position on images taken by Puckett
  on 2011 June 9 (limiting mag 19.1). The variable was designated PSN
  J16313945+4129229 when posted on the Central Bureau's TOCP webpage
  and is here designated SN 2011dw based on the spectroscopic report
  below. Puckett has posted a finder image for 2011dw at website URL
  http://possdata.com/PSNJ16313945+4129229.jpg. D. C. Leonard, San
  Diego State University; J. Moustakas, University of California at San
  Diego; B. J. Swift and D. McCarthy, University of Arizona; V. Bailey,
  E. Carrico, A. Carter, E. Chui, E. Douglas, E. Eggeman, R. Goldberg,
  R. Grant, K. Hartman, J. Hellerstein, E. Hooper, C. Horlick-Cruz,
  L. Hunter, T. Jiles, E. D. Johnson, K. Kumar, L. Lappe, J. Lee,
  W. Lee, F. Marsh, G. Mehta, P. Miller, R. Rampalli, J. Reed, K. Rice,
  H. Saldivar, M. Salgado-Flores, A. Schlingman, W. F. Schlingman,
  W. M. Schlingman, S. Scibelli, K. Sinclair, I. Steincamp, N. Stock,
  N. Todd, L. L. Aizpuru Vargas, S. Yamanaka, and E. Zachary, 2011
  Advanced Teen Astronomy Camp, report that a low-dispersion optical
  spectrum (range 370-690 nm) of PSN J16313945+4129229 = SN 2011dw,
  obtained with the 2.3-m Bok telescope (+ Boller &amp; Chivens
  spectrograph) at Steward Observatory on June 30 UT, displays a
  featureless, blue continuum. Identifying a faint, unresolved emission
  line in the spectrum at 675.8 nm with H-alpha indicates a redshift of
  0.03, in agreement with the recession velocity reported in the second
  Sloan Digital Sky Survey Data Release of the putative host galaxy,
  PGC 58436. The spectrum is reminiscent of a very young type-II/IIb
  supernova, although additional spectroscopy is required to confirm the
  nature of this event. Adopting the NASA/IPAC Extragalactic Database
  distance-modulus estimate of PGC 58436 of m-M = 35.5 magnitudes,
  that the apparent magnitude of PSN J16313945+4129229 (16.9 on June
  27.3391, as reported by the discoverers, above) indicates an absolute
  magnitude of -18.6, which is a somewhat-greater luminosity than typical
  type-II/IIb supernovae achieve.

Title: Supernova 2011dv in NGC 6078 = Psn J16120400+1412330
Authors: Ciabattari, F.; Dimai, A.; Leonini, S.; Leonard, D. C.;
   Moustakas, J.; Swift, B. J.; McCarthy, D.; Bailey, V.; Carrico, E.;
   Carter, A.; Chui, E.; Douglas, E.; Eggeman, E.; Goldberg, R.; Grant,
   R.; Hartman, K.; Hellerstein, J.; Hooper, E.; Horlick-Cruz, C.; Hunter,
   L.; Jiles, T.; Johnson, E. D.; Kumar, K.; Lappe, L.; Lee, J.; Lee,
   W.; Marsh, F.; Mehta, G.; Miller, P.; Rampalli, R.; Reed, J.; Rice,
   K.; Saldivar, H.; Salgado-Flores, M.; Schlingman, A.; Schlingman,
   W. F.; Scibelli, S.; Sinclair, K.; Steincamp, I.; Stock, N.; Todd,
   N.; Aizpuru Vargas, L. L.; Yamanaka, S.; Zachary, E.; Balam, D. D.;
   Graham, M. L.; Hsiao, E. Y.; Green, D. W. E.
Bibcode: 2011CBET.2755....1C
Altcode: 2011CBET.2755A...1C
  F. Ciabattari, Borgo a Mozzano, Italy, reports the discovery of a point-
  like object (mag 16.2) on unfiltered CCD images (limiting magnitude
  19.2) obtained on June 28.86 UT with a 0.5-m Newtonian telescope in
  the course of the Italian Supernovae Search Project, the new object
  being located at R.A. = 16h12m04s.62, Decl. = +14d12'33".2 (equinox
  2000.0; astrometry with respect to UCAC-2 stars), which is 13" west
  of the center of the galaxy NGC 6078. The variable was designated
  PSN J16120400+1412330 when posted on the Central Bureau's TOCP
  webpage and is here designated SN 2011dv based on the spectroscopic
  confirmation reported below. Additional magnitudes for 2011dv as
  provided by Ciabattari: 1992 Apr. 30, [20.3 (Palomar Sky Survey, J
  plate); 1994 June 8, [20.3 (Palomar Sky Survey, F plate); 2010 June,
  [19.1 (images taken by Ciabattari); 2011 June 29.98 UT, 16.0 (A. Dimai,
  Cortina d'Ampezzo, Italy; and S. Leonini, Siena, Italy; remotely using
  the GRAS-7 PlaneWave 43-cm CDK telescope in Spain). D. C. Leonard, San
  Diego State University; J. Moustakas, University of California at San
  Diego; B. J. Swift and D. McCarthy, University of Arizona; V. Bailey,
  E. Carrico, A. Carter, E. Chui, E. Douglas, E. Eggeman, R. Goldberg,
  R. Grant, K. Hartman, J. Hellerstein, E. Hooper, C. Horlick-Cruz,
  L. Hunter, T. Jiles, E. D. Johnson, K. Kumar, L. Lappe, J. Lee,
  W. Lee, F. Marsh, G. Mehta, P. Miller, R. Rampalli, J. Reed, K. Rice,
  H. Saldivar, M. Salgado-Flores, A. Schlingman, W. F. Schlingman,
  W. M. Schlingman, S. Scibelli, K. Sinclair, I. Steincamp, N. Stock,
  N. Todd, L. L. Aizpuru Vargas, S. Yamanaka, and E. Zachary, 2011
  Advanced Teen Astronomy Camp, report that inspection of a low-dispersion
  optical spectrum (range 370-690 nm) of PSN J16120400+1412330 = SN
  2011dv, obtained with the 2.3-m Bok telescope (+ Boller &amp; Chivens
  spectrograph) at Steward Observatory on June 30 UT, shows it to be a
  normal type-Ia supernova near maximum light. Cross-correlation with
  a library of supernova spectra using the "Supernova Identification"
  code (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) finds good
  matches with near-maximum (2 +/- 6 days) template spectra of SN
  1992A and SN 2002bo. Adopting the NASA/IPAC Extragalactic Database
  recession velocity for NGC 6078 of 9378 km/s (Falco et al. 1999,
  PASP 111, 438), the maximum absorption in the Si II line (rest 635.5
  nm) is blueshifted by approximately 13600 km/s. D. D. Balam, Dominion
  Astrophysical Observatory, National Research Council of Canada (NRCC);
  M. L. Graham, Las Cumbres Observatory Global Telescope, University of
  California at Santa Barbara; E. Y. Hsiao, Lawrence Berkeley Laboratory;
  and D. W. E. Green, Harvard University, report that a spectrogram
  (range 389-725 nm., resolution 0.3 nm) of PSN J16120400+1412330 = SN
  2011dv, obtained on June 30.27 UT with the 1.82-m Plaskett Telescope
  of the NRCC, shows it to be a type-Ia supernova about five days past
  maximum light. Cross-correlation with a library of supernova spectra
  using the SNID code indicates that 2011dv is most similar to the
  type-Ia supernova 2006gz at five days past maximum light.

Title: Supernova 2011dn in UGC 11501 = Psn J19583553+0236163
Authors: Koff, R. A.; Leonard, D. C.; Moustakas, J.; Swift, B. J.;
   McCarthy, D.; Bailey, V.; Carrico, E.; Carter, A.; Chui, E.; Douglas,
   E.; Eggeman, E.; Goldberg, R.; Grant, R.; Hartman, K.; Hellerstein, J.;
   Hooper, E.; Horlick-Cruz, C.; Hunter, L.; Jiles, T.; Johnson, E. D.;
   Kumar, K.; Lappe, L.; Lee, J.; Lee, W.; Marsh, F.; Mehta, G.; Miller,
   P.; Rampalli, R.; Reed, J.; Rice, K.; Saldivar, H.; Salgado-Flores,
   M.; Schlingman, A.; Scibelli, S.; Sinclair, K.; Steincamp, I.; Stock,
   N.; Todd, N.; Aizpuru Vargas, L. L.; Yamanaka, S.; Zachary, E.
Bibcode: 2011CBET.2746....2K
Altcode:
  Additional unfiltered CCD magnitudes for SN 2011dn: June
  23.23-23.30 UT, 16.5 (R. A. Koff, Bennett, CO, U.S.A.; Celestron
  0.20-m f/10 reflector + SBIG ST-6 CCD camera; multiple co-added
  images); 23.354, 16.1 (Joseph Brimacombe, Cairns, Australia;
  three co-added 60-s images; position end figures 35s.56,
  11".3). Brimacombe's image is posted at the following website URL:
  http://www.flickr.com/photos/43846774@N02/5865118910/. D. C. Leonard,
  San Diego State University; J. Moustakas, University of California
  at San Diego; B. J. Swift and D. McCarthy, University of Arizona;
  V. Bailey, E. Carrico, A. Carter, E. Chui, E. Douglas, E. Eggeman,
  R. Goldberg, R. Grant, K. Hartman, J. Hellerstein, E. Hooper,
  C. Horlick-Cruz, L. Hunter, T. Jiles, E. D. Johnson, K. Kumar,
  L. Lappe, J. Lee, W. Lee, F. Marsh, G. Mehta, P. Miller, R. Rampalli,
  J. Reed, K. Rice, H. Saldivar, M. Salgado-Flores, A. Schlingman,
  W. F. Schlingman, W. M. Schlingman, S. Scibelli, K. Sinclair,
  I. Steincamp, N. Stock, N. Todd, L. L. Aizpuru Vargas, S. Yamanaka,
  and E. Zachary, 2011 Advanced Teen Astronomy Camp, report that
  inspection of a low-dispersion optical spectrum (range 370-690 nm)
  of PSN J19583553+0236163 = SN 2011dn, obtained with the 2.3-m Bok
  telescope (+ Boller &amp; Chivens spectrograph) at Steward Observatory
  on June 23 UT, shows it to be a type-Ia supernova of the SN-1991T-like
  sub-class, several days before maximum light. Cross-correlation with
  a library of supernova spectra using the "Supernova Identification"
  code (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) finds good matches
  with pre-maximum (-6.4 +/- 2.7 days) template spectra of SN 1991T, SN
  1997br, and SN 1999aa. Adopting the NASA/IPAC Extragalactic Database
  (NED) recession velocity for UGC 11501 of 7572 km/s (a 21-cm H I line
  measurement taken from Springob et al. 2005, Ap.J. Suppl. 160, 149),
  the maximum absorption in the (weak) Si II line (rest 635.5 nm) is
  blueshifted by approximately 10100 km/s.

Title: Waiting Points and Bottlenecks in Nova and X-ray Burst
    Nucleosynthesis
Authors: Goldberg, Leah
Bibcode: 2010APS..DNP.EA044G
Altcode:
  At Oak Ridge National Laboratory, we are investigating nucleosynthesis
  in nova explosions and X-ray bursts, specifically at ``waiting points''
  and ``bottlenecks'' -- unusual phenomenon in which nuclei interrupt
  the sequence of thermonuclear reactions that form heavier elements
  from lighter ones, significantly affecting the final abundances and
  the energy generation rate in stellar explosions. Nuclei identified
  as waiting points or bottlenecks seem to play a more important role in
  explosions and need to be singled out for further investigation. Such
  points are defined by a series of acceptance and rejection tests in
  a simulation, Computational Infrastructure for Nuclear Astrophysics
  (CINA), in which a suite of codes visualizes nucleosynthesis over a
  specified time interval and allows us, for each nucleus, to consider
  eight surrounding nuclei in the Z=N plane based on possible reaction
  paths in the rp-process. After considering abundance, lifetime and
  reaction flux, reaction rate, and reaction Q-value, we accept or reject
  accordingly, and can then better ascertain the relationship between
  waiting points and bottlenecks and nuclear flow.

Title: Experimental Evidence Leading to an Alternative Explanation
    of Why D-tyrosine Sometimes Crystallizes Faster than Its L-Enantiomer
Authors: Goldberg, Stanley I.
Bibcode: 2008OLEB...38..149G
Altcode: 2008OLEB..tmp....5G
  On the occasions when D-tyrosine is observed to crystallize faster than
  its L-enantiomer, it is the result of a diastereomeric interaction
  between an airborne, non-racemic, chiral influence—probably a
  fungal spore—and the tyrosine enantiomers, enhancing the degree of
  crystal nucleation of D-tyrosine over L-tyrosine. This explanation,
  supported by experimental evidence, is presented as a more plausible
  alternative to the Shinitzky Deamer hypothesis (Shinitzky et al.,
  Progress in biological chirality, Elsevier, Amsterdam, pp. 329 337,
  2004; Deamer et al., Chirality, 19:751 763, 2007) which relies on the
  parity violation energy difference between enantiomers, a femtojoule
  to picojoule per mole theoretical energy range.

Title: A Study of the ^14C(?,?) Reaction Rate Through the ANC
    Technique
Authors: Johnson, E. D.; Rogachev, G. V.; Mukhamedzhanov, A. M.;
   Aguilar, A.; Bender, P.; Devore, T.; Goldberg, G. V.; Kemper, K. W.;
   Lee, S.; Miller, L.; Mitchell, J.; Peplowski, P.; Perry, M.; Reynolds,
   R.; Rojas, A.
Bibcode: 2008APS..APRH15002J
Altcode:
  The astrophysical significance of the ^14C(?,?) reaction is due
  to its involvement in the NCO chain. The NCO chain is thought to
  trigger He flashes in white dwarf stars, and is also thought to be
  a neutron source for the s-process in low mass stars [L. Buchmann
  et al., The Astrophys. Journ. 324 (1988), M. Hashimoto et al., The
  Astrophys. Journ. 307 (1986)]. Recently the ANC of the 3^-, 6.4 MeV,
  near threshold state in ^18O was measured via a sub-Coulomb, inverse
  kinematics ?-transfer reaction at the Florida State University J.D. Fox
  Superconducting Accelerator Laboratory. The ^14C(?,?) reaction rate
  at stellar temperatures is highly dependent upon the structure of this
  3^- state. As shown in E.D. Johnson et al. PRL 97 (2006) the measured
  ANC can be used to calculate the ^14C(?,?) reaction rate without any
  dependence on nuclear models.

Title: Revised correlation between Odin/OSIRIS PMC properties and
    coincident TIMED/SABER mesospheric temperatures
Authors: Feofilov, A.; Petelina, S. V.; Kutepov, A. A.; Pesnell,
   W. D.; Goldberg, R. A.; Llewellyn, E. J.; Russell, J. M.
Bibcode: 2006AGUFMSA21A0243F
Altcode:
  The Optical Spectrograph and Infrared Imaging System (OSIRIS) instrument
  on board the Odin satellite detects Polar Mesospheric Clouds (PMCs)
  through the enhancement in the limb-scattered solar radiance. The
  Sounding of the Atmosphere using the Broadband Emission Radiometry
  (SABER) instrument on board the TIMED satellite is a limb scanning
  infrared radiometer that measures temperature and vertical profiles
  and energetic parameters for minor constituents in the mesosphere
  and lower thermosphere. The combination of OSIRIS and SABER data
  has been previously used to statistically derive thermal conditions
  for PMC existence [Petelina et al., 2005]. In this work, we employ
  the simultaneous common volume measurements of PMCs by OSIRIS and
  temperature profiles measured by SABER for the Northern Hemisphere
  summers of 2002--2005 and corrected in the polar region by accounting
  for the vibrational-vibrational energy exchange among the CO2 isotopes
  [Kutepov et al., 2006]. For each coincidence identified within ±1
  degree latitude, ±2 degrees longitude and ≤1 hour time the frost
  point temperatures were calculated using the corresponding SABER
  temperature profile and water vapor densities of 1, 3, and 10 ppmv. We
  found that the PMC presence and brightness correlated only with
  the temperature threshold that corresponds to the frost point. The
  absolute value of the temperature below the frost point, however,
  didn't play a significant role in the intensity of PMC signal for the
  majority of selected coincidences. The presence of several bright
  clouds at temperatures above the frost point is obviously related
  to the limitation of the limb geometry when some near- or far-field
  PMCs, actually located at higher (and colder) altitudes are detected
  at lower altitudes. S.V. Petelina, D.A. Degenstein, E.J. Llewellyn,
  N.D. Lloyd, C.J. Mertens, M.G. Mlynczak, and J.M. Russell III, "Thermal
  conditions for PMC existence derived from Odin/OSIRIS and TIMED/SABER
  data", Geophys. Res. Lett., 32, L17813, doi: 10.1029/2005GL023099,
  (2005) A.A. Kutepov, A.G. Feofilov, B.T. Marshall, L.L. Gordley,
  W. D. Pesnell, R.A. Goldberg, and J.M. Russell III, "SABER temperature
  observations in the summer polar mesosphere and lower thermosphere:
  importance of accounting for the CO2 ν_2 quanta V -V exchange",
  accepted for publication in Geophys. Res. Lett., (2006)

Title: Annual review of astronomy and astrophysics, Vol. 42.
Authors: Goldberg, Leo
Bibcode: 2004ARA&A..42.....G
Altcode:
  No abstract at ADS

Title: Annual review of astronomy and astrophysics, Vol. 41
Authors: Goldberg, Leo
Bibcode: 2003ARA&A..41.....G
Altcode:
  No abstract at ADS

Title: A Survey of Proper-Motion Stars. XV. Orbital Solutions for
    34 Double-lined Spectroscopic Binaries
Authors: Goldberg, Dorit; Mazeh, Tsevi; Latham, David W.; Stefanik,
   Robert P.; Carney, Bruce W.; Laird, John B.
Bibcode: 2002AJ....124.1132G
Altcode:
  We present orbital solutions for 34 double-lined spectroscopic binaries
  found in the Carney-Latham sample of 1464 stars selected for high
  proper motion. We use TODCOR, a two-dimensional correlation technique,
  to extract the velocities for the primary and secondary stars and their
  light ratio. For our single-order echelle spectra, obtained with the
  Center for Astrophysics Digital Speedometers, we find that we can reach
  secondaries that are as much as 2 mag fainter than their primaries. The
  ratio of the primary to secondary velocity residuals from the orbital
  fit equals approximately the secondary-to-primary light ratio, as
  would be expected for the photon-limited case. We use our mass and
  light ratios to evaluate the mass-luminosity relation for metal-poor
  main-sequence dwarfs in the mass range 0.55-0.8 M<SUB>solar</SUB>. We
  assume an L~M<SUP>β</SUP> relation and find that the exponent at around
  5200 Å is 7.4+/-0.6. We find this is in good agreement with the slope
  of the corresponding theoretical M<SUB>V</SUB>-M 14 Gyr isochrones
  from the VandenBerg &amp; Bell models for metal-poor stars. Some of
  the results presented here used observations made with the Multiple
  Mirror Telescope, a facility operated jointly by the University of
  Arizona and the Smithsonian Institution.

Title: Phenomenology of Randall-Sundrum black holes
Authors: Anchordoqui, Luis A.; Goldberg, Haim; Shapere, Alfred D.
Bibcode: 2002PhRvD..66b4033A
Altcode: 2002hep.ph....4228A
  We explore the phenomenology of microscopic black holes in the
  S<SUP>1</SUP>/Z<SUB>2</SUB> Randall-Sundrum (RS) model. We consider the
  canonical framework in which both gauge and matter fields are confined
  to the brane and only gravity spills into the extra dimension. The
  model is characterized by two parameters: the mass of the first
  massive graviton (m<SUB>1</SUB>), and the curvature 1/l of the RS
  anti-de Sitter space. We compute the sensitivities of present and
  future cosmic ray experiments to black hole mediated events, for a wide
  range of l and m<SUB>1</SUB>, and compare them with the sensitivities
  of Fermilab Tevatron runs I and II to higher-dimensional physics. As
  part of our phenomenological analysis, we examine constraints placed
  on l by AdS-CFT considerations.

Title: Variation of mesospheric ozone during the highly relativistic
    electron event in May 1992 as measured by the High Resolution Doppler
    Imager instrument on UARS
Authors: Pesnell, W. Dean; Goldberg, Richard A.; Jackman, Charles H.;
   Chenette, D. L.; Gaines, E. E.
Bibcode: 2000JGR...10522943P
Altcode:
  Highly relativistic electron precipitation events (HREs) include
  long-lived enhancements of the flux of electrons with E&gt;1MeV
  into the Earth's atmosphere. HREs also contain increased fluxes of
  electrons with energies above 100 keV that have been predicted to
  cause large depletions of mesospheric ozone. For some of the measured
  instantaneous values of the electron fluxes during the HRE of May
  1992, relative depletions greater than 22% were predicted to occur
  between altitudes of 55 and 80 km, where HO<SUB>x</SUB> reactions
  cause local minima in both the ozone number density and mixing ratio
  altitude profiles. These ozone depletions should follow the horizontal
  distribution of the electron precipitation, having a distinct boundary
  equatorward of the L=3 magnetic shell. To search for these effects,
  we have analyzed ozone data from the High Resolution Doppler Imager
  (HRDI) instrument on UARS. Owing to the multiple, off-track viewing
  angles of HRDI, observations in the region affected by the electrons
  are taken at similar local solar times before, during, and after the
  electron flux increase. Our analysis limits the relative ozone depletion
  to values &lt;10% during the very intense May 1992 HRE. We do observe
  decreases in the ozone mixing ratio at several points in the diurnal
  cycle that may be associated with the transport of water vapor into the
  mesosphere during May 1992. This masking of the precipitating electron
  effects by the seasonal variations in water vapor can complicate the
  detection of those effects.

Title: A Solution to the Problem of the Origin of Biochirality Based
    on Observational and Experimental Evidence
Authors: Goldberg, Stanley I.
Bibcode: 2000OLEB...30..212G
Altcode:
  The long standing problem of the origin of biochirality (homochirality)
  has resisted solution because enantiomers possess identical physical
  and chemical properties, so differences upon which to base possible
  separations cannot be evoked. <P />While homochirality is an
  indispensable factor in contemporary biochemical life, it also
  appears to have been required for the emergence of life as well
  for two compelling reasons. First, a homochiral prebiotic world
  would have neatly avoided the problem of an impossibly large number
  of configurational isomers resulting from stereochemically random
  assembly of D and L monomers into biopolymers such as peptides. Even
  the formation of a peptide of modest size, say one consisting of only
  twenty-five amino acid residues, would have meant the stereo-random
  formation of 2(exp 25) or 33,554,432 configurationally isomeric
  peptides; only one of which would have been the all L-peptide found in
  contemporary life. The second reason arises out a number of experimental
  and theoretical studies all consistent with the view that the presence
  of both enantiomers, even when one form is in low concentration relative
  to the other. will prevent or seriously inhibit development of vital
  biochemical processes (Bonner, 1995, and refs. therein). <P />Both
  difficulties are avoided if enantiopure chiral material were present
  on the primitive Earth, and this paper provides such a solution. It
  brings together and synthesizes recent observations on the delivery of
  nonracemic material to Earth (Cronin and Pizzarello, 1997) with older
  experimental work on phase relationships of enantiomers (Jacques et ai,
  1981) to reveal how global accumulations of enantiopure biologically
  relevant material could have formed on the early Earth.

Title: A search of UARS data for ozone depletions caused by the
    highly relativistic electron precipitation events of May 1992
Authors: Pesnell, W. Dean; Goldberg, Richard A.; Jackman, Charles H.;
   Chenette, D. L.; Gaines, E. E.
Bibcode: 1999JGR...104..165P
Altcode:
  Highly relativistic electron precipitation (HRE) events containing
  significant fluxes of electrons with E&gt;1MeV have been predicted
  by models to deplete mesospheric ozone. For the electron fluxes
  measured during the great HRE of May 1992, depletions were predicted
  to occur between altitudes of 55 and 80 km, where HO<SUB>x</SUB>
  reactions cause a local minimum in the ozone number density and mixing
  ratio. Measurements of the precipitating electron fluxes by the particle
  environment monitor (PEM) tend to underestimate their intensity; thus
  the predictions of ozone depletion should be considered an estimate
  of a lower limit. Since the horizontal distribution of the electron
  precipitation follows the terrestrial magnetic field, it would show
  a distinct boundary equatorward of the L=3 magnetic shell and be
  readily distinguished from material that was not affected by the HRE
  precipitation. To search for possible ozone depletion effects, we
  have analyzed data from the cryogenic limb array etalon spectrometer
  and microwave limb sounder instruments on UARS for the above HRE. A
  simplified diurnal model is proposed to understand the ozone data from
  UARS, also illustrating the limitations of the UARS instruments for
  seeing the ozone depletions caused by the HRE events. This diurnal
  analysis limits the relative ozone depletion at around 60 km altitude to
  values of &lt;10% during the very intense May 1992 event, consistent
  with our prediction using an improved Goddard Space Flight Center
  two-dimensional model.

Title: Galaxy candidates in the Zone of Avoidance
Authors: Lahav, Ofer; Brosch, Noah; Goldberg, Evgeny; Hau, George
   K. T.; Kraan-Korteweg, Renee C.; Loan, Andy J.
Bibcode: 1998MNRAS.299...24L
Altcode: 1997astro.ph..7345L
  Motivated by recent discoveries of nearby galaxies in the Zone of
  Avoidance (ZOA), we conducted a pilot study of galaxy candidates at
  low galactic latitude, near galactic longitude l~135 deg, where the
  Supergalactic plane is crossed by the Galactic plane. We observed with
  the 1-m Wise Observatory in the l band 17 of the `promising' candidates
  identified by visual examination of Palomar red plates by Hau et al. A
  few candidates were also observed in R or B bands, or had spectroscopic
  observations performed at the Isaac Newton Telescope and at the Wise
  Observatory. Our study suggests that there are probably 10 galaxies in
  this sample. We also identify a probable planetary nebula. The final
  confirmation of the nature of these sources must await the availability
  of full spectroscopic information. The success rate of ~50 per cent
  in identifying galaxies at galactic latitude |b|&lt;5 deg indicates
  that the ZOA is a promising region to discover new galaxies.

Title: Using Astrometry to Deblend Microlensing Events
Authors: Goldberg, David M.
Bibcode: 1998ApJ...498..156G
Altcode: 1997astro.ph..8172G
  We discuss the prospect of deblending microlensing events by observing
  astrometric shifts of the lensed stars. Since microlensing searches are
  generally performed in very crowded fields, it is expected that stars
  will be confusion limited rather than limited by photon statistics. By
  performing simulations of events in crowded fields, we find that if we
  assume a dark lens and that the lensed star obeys a power-law luminosity
  function, n(L) ~ L<SUP>-β</SUP>, over half the simulated events show a
  measurable astrometric shift. Our simulations included 20,000 stars in
  a 256 × 256 Nyquist-sampled CCD frame. For β = 2, we found that 58%
  of the events were significantly blended (F<SUB>*</SUB>/F<SUB>tot</SUB>
  &lt;= 0.9), and of those, 73% had a large astrometric shift (&gt;=0.5
  pixels). Likewise, for β = 3, we found that 85% of the events were
  significantly blended and that 85% of those had large shifts. Moreover,
  since the shift may be used to determine the true position of a
  source star with respect to the observed point-spread function, a
  high-resolution follow-up survey may be used to identify the source
  star and determine the blending fraction directly.

Title: Deblending Microlensing Events Using Astrometric Shifts
Authors: Goldberg, D. M.; Wozniak, P.; Paczynski, B.
Bibcode: 1997AAS...191.8307G
Altcode: 1997BAAS...29.1347G
  In this poster, we present the prospect that astrometric shifts
  can be used to identify blended microlensing events in crowded
  fields. Moreover, by measuring an astrometric shift, one can determine
  the position of the true lensed star with respect to the local field
  with very high precision. We first perform several simulations of
  microlensing searches in crowded fields and find that if we assume
  a dark lens, and that the lensed star obeys a power law luminosity
  function, n(L)~ L(-beta ) , over half the simulated events show a
  measurable astrometric shift. For simulations of 20000 stars on a 256x
  256 Nyquist sampled CCD frame, we found that with beta =2, 58% of the
  events were significantly blended (F_{*}/F<SUB>tot</SUB> &lt;= 0.9),
  and of those, 73% had a large astrometric shift (&gt;= 0.5 pixels). For
  beta =3, we found that 85% were significantly blended, and that 85%
  of those had a significant shift. Since we expect most blended events
  to show a significant shift, we look in the OGLE I database (Wozniak
  &amp; Szymanski 1997), and find measurable and systematic shifts
  in over half the candidate microlensing events, including OGLE # 5,
  which was considered to be blended from photometric data.

Title: Optical observations of Dwingeloo 1, a nearby barred spiral
    galaxy behind the Milky Way
Authors: Loan, A. J.; Maddox, S. J.; Lahav, O.; Balcells, M.;
   Kraan-Korteweg, R. C.; Assendorp, R.; Almoznino, E.; Brosch, N.;
   Goldberg, E.; Ofek, E. O.
Bibcode: 1996MNRAS.280..537L
Altcode:
  We present new optical observations of the nearby barred spiral
  galaxy Dwingeloo 1 (Dw1) obtained with the Isaac Newton, William
  Herschel and Wise telescopes. Dw1 lies at Galactic coordinates
  (l=138.˚52, b=-0.˚11) and it is heavily obscured by dust and gas in
  the Milky Way. We infer that Dw1 is of morphological type SBb or SBc
  (T=4), has an inclination i~=50 deg, a position angle PA~=110 deg,
  and a recession velocity relative to the Milky Way V_MW=256+/-9 km
  s^-1. The measured total apparent magnitudes of Dw1 are V=14.0+/-0.5,
  R=12.2+/-0.2 and I=10.7+/-0.2. The extinction estimate towards Dw1 is
  highly uncertain. The extinction in the B band, derived from Galactic
  HI column density measurements, is A_B~=5.8. Estimated from Galactic
  100-μm emission, the extinction is A_B~=4.3, while the reddened
  colours of Dw1 yield an estimate of A_B~=10.4. Assuming A_B=5.8,
  Tully-Fisher relations in the I and R bands lead to a distance estimate
  for Dw1 of D~=300 km s^-1. However, for the derived range of extinction
  estimates 4.3&lt;~A_B&lt;~10.4, the distance varies from 100 to 500 km
  s^-1. We also report the detection of numerous HII regions associated
  with Dw1, and present data from the Infrared Astronomical Satellite
  (IRAS) archive.

Title: Annual review of astronomy and astrophysics
Authors: Goldberg, Leo
Bibcode: 1996araa.book.....G
Altcode:
  No abstract at ADS

Title: Cataclysmic variables and related objects
Authors: Hack, Margherita; Ladous, Constanze; Jordan, Stuart D.;
   Thomas, Richard N.; Goldberg, Leo; Pecker, Jean-Claude
Bibcode: 1993NASSP.507.....H
Altcode: 1993cvro.nasa.....H; 1993QB835.H27......
  No abstract at ADS

Title: Rocket measurements of relativistic electrons: New features
    in fluxes, spectra and pitch angle distributions
Authors: Herrero, F. A.; Baker, D. N.; Goldberg, R. A.
Bibcode: 1991GeoRL..18.1481H
Altcode:
  We report new features of precipitating relativistic electron fluxes
  measured on a spinning sounding rocket payload at midday between
  altitudes of 70 and 130 km in the auroral region (Poker Flat, Alaska,
  65.1°N, 147.5°W, and L=5.5). The sounding rocket (NASA 33.059) was
  launched at 21:29 UT on May 13, 1990 during a relativistic electron
  enhancement event of modest intensity. Electron fluxes were measured
  for a total of about 210 seconds at energies from 0.1 to 3.8 MeV, while
  pitch angle was sampled from 0° to 90° every spin cycle. Flux levels
  during the initial 90 seconds were about 5 to 8 times higher than in
  the next 120 seconds, revealing a time scale of more than 100 seconds
  for large amplitude intensity variations. A shorter time scale appeared
  for downward electron bursts lasting 10 to 20 seconds. Electrons with
  energies below about 0.2 MeV showed isotropic pitch angle distributions
  during most of the first 90 seconds of data, while at higher energies
  the electrons had highest fluxes near the mirroring angle (90°) when
  they occurred, the noted downward bursts were seen at all energies. Data
  obtained during the second half of the flight showed little variation
  in the shape of the pitch angle distribution for energies greater than
  0.5 MeV; the flux at 90° was about 100 times the flux at 0°. We have
  compared the low altitude fluxes with those measured at geostationary
  orbit (L=6.6), and find that the low altitude fluxes are much higher
  than expected from a simple mapping of a pancake distribution at high
  altitudes (at the equator). Energy deposition of this modest event
  is estimated to increase rapidly above 45 km, already exceeding the
  cosmic ray background at 45 km.

Title: Radial Velocity Variations in Alpha Orionis, Alpha Scorpii,
    and Alpha Herculis
Authors: Smith, Myron A.; Patten, Brian M.; Goldberg, Leo
Bibcode: 1989AJ.....98.2233S
Altcode:
  Radial-velocity observations of Alpha Ori, Alpha Sco A, and Alpha Her A
  are used to study radial-velocity periodicities in M supergiants. The
  data refer to several metallic lines in the H-alpha region and to
  H-alpha itself. It is shown that Alpha Ori and Alpha Sco A have cycle
  lengths of about 1 yr and semiamplitudes of 2 km/s. It is suggested
  that many semiregular red supergiant varibles such as Alpha Ori may
  be heading toward chaos. All three stars show short-term stochastic
  flucutations with an amplitude of 1-2 km/s. It is found that the
  long-term variability of H-alpha velocities may be a consequence of
  intermittent failed ejections.

Title: Baryon-number violation in a quantum gas of W and Higgs bosons
Authors: Goldberg, Haim
Bibcode: 1989PhRvL..62.1952G
Altcode:
  Use of a coherent-state representation of the sphaleron allows a direct
  calculation of its production rate in a thermal gas of W and Higgs
  bosons Technical considerations permit a straightforward calculation
  only in the case λ/g<SUP>2</SUP>~=1 (M<SUB>H</SUB>~=3M<SUB>W</SUB>),
  where λ is the Higgs-boson quartic coupling, and g is the SU(2) gauge
  coupling. For this case it is found that the rate is unsuppressed
  for temperatures T&gt;=2.4M<SUB>W</SUB>(0), where M<SUB>W</SUB>(0)
  is the zero-temperature W mass. Thus anomalous B+L violation is also
  unsuppressed above this temperature.

Title: FGK stars and T Tauri stars
Authors: Cram, Lawrence E.; Kuhi, Leonard V.; Jordan, Stuart; Thomas,
   Richard; Goldberg, Leo; Pecker, Jean-Claude
Bibcode: 1989NASSP.502.....C
Altcode: 1989QB843.C6C73....; 1989fstt.book.....C
  The purpose of this book, FGK Stars and T Tauri Stars, like all other
  volumes of this series, is to exhibit and describe the best space
  data and ground based data currently available, and also to describe
  and critically evaluate the status of current theoretical models
  and physical mechanisms that have been proposed to interpret these
  data. The method for obtaining this book was to collect manuscripts
  from competent volunteer authors, and then to collate and edit these
  contributions to form a well structured book, which will be distributed
  to an international community of research astronomers by NASA and by
  the French CNRS.

Title: Atomic spectroscopy and astrophysics
Authors: Goldberg, Leo
Bibcode: 1988PhT....41h..38G
Altcode:
  The evolution of atomic spectroscopy as a central part of astrophysics
  is reviewed. The beginnings of laboratory astrophysics and the birth
  of theoretical astrophysics are examined. The way in which theoretical
  physics, including quantum theory, improved the accuracy of astronomical
  models, the acceptance of calculations of transition probabilities by
  astronomers, and laboratory astrophysics since the end of World War II
  are discussed. Several spectra are presented, noting their importance
  to astrophysics.

Title: O stars and Wolf-Rayet stars
Authors: Conti, Peter S.; Underhill, Anne B.; Jordan, Stuart; Thomas,
   Richard N.; Goldberg, Leo; Pecker, Jean-Claude; Baade, D.; Divan,
   L.; Garmany, C. D.; Henrichs, H. F.; Kudritzki, R. P.; Pauldrach,
   A.; Prévot-Burnichon, M. -L.; Puls, J.
Bibcode: 1988NASSP.497.....C
Altcode: 1988oswr.book.....C
  Basic information is given about O and Wolf-Rayet stars indicating
  how these stars are defined and what their chief observable properties
  are. Part 2 of the volume discussed four related themes pertaining to
  the hottest and most luminous stars. Presented are: an observational
  overview of the spectroscopic classification and extrinsic properties
  of O and Wolf-Rayet stars; the intrinsic parameters of luminosity,
  effective temperature, mass, and composition of the stars, and a
  discussion of their viability; stellar wind properties; and the
  related issues concerning the efforts of stellar radiation and
  wind on the immediate interstellar environment are presented. <P
  />Contents: Perspective (R. N. Thomas).Part I. Introduction (L. Divan,
  M.-L. Prévot-Burnichon).1. Introducing the O and Wolf-Rayet stars.Part
  II. One perspective on O, Of, and Wolf-Rayet stars emphasizing winds
  and mass loss, with remarks on environment and evolution:2. Overview of
  O, Of, and Wolf-Rayet populations (P. S. Conti). 3. Intrinsic stellar
  parameters (P. S. Conti, D. Baade). 4. Stellar winds: (a) Introduction
  (P. S. Conti). (b) Mass loss from O stars (C. D. Garmany). (c) Mass
  loss in Wolf-Rayetstars (P. S. Conti). (d) Radiation-driven winds
  of hot luminous stars (R. P. Kudritzki, A. Pauldrach, J. Puls). (e)
  Intrinsic variability in ultraviolet spectra of early-type stars: the
  discrete absorption lines (H. Henrichs). 5. Environments and evolution
  (P. S. Conti).Part III. Another perspective on O, Of, and Wolf-Rayet
  stars, emphasizing model atmospheres and possibilities for atmospheric
  heating (A. B. Underhill): 6. Understanding the O and Wolf-Rayet
  stars. 7. Model Atmospheres and the theory of spectra for O and
  Wolf-Rayet stars. 8. The physics of the mantles of hot stars. 9. Summary
  of processes influencing the spectra of O and Wolf-Rayet stars.

Title: Radial Velocity Variations of Alpha Orionis (Betelgeuse)
Authors: Patten, B. M.; Smith, M. A.; Goldberg, L.
Bibcode: 1987BAAS...19Q1028P
Altcode: 1987BAAS...19Z1028P
  No abstract at ADS

Title: Comments on Solar Wind 6 (edited by S. Drake)
Authors: Goldberg, L.
Bibcode: 1987sowi.conf..695G
Altcode:
  No abstract at ADS

Title: Diameter and Limb-darkening Measures for Alpha Orionis
Authors: Cheng, A. Y. S.; Hege, E. K.; Hubbard, E. N.; Goldberg, L.;
   Strittmatter, P. A.; Cocke, W. J.
Bibcode: 1986ApJ...309..737C
Altcode:
  Previously reported speckle interferometric measurements of the
  angular diameter of Alpha Ori are widely scattered and apparently
  inconsistent. Stellar atmosphere models predict a stellar disk to be
  limb-darkened differently for different spectral features, and that
  less limb-darkening will be observed at longer wavelengths. Upon
  careful analysis of calibrated speckle observations obtained at
  various wavelengths with the KPNO 4 m telescope, a single diameter
  parameter is found to be inadequate to explain all of the features of
  the measurements. There is evidence for a central stellar component
  of 42.1(+ or - 1.1) mas diameter with extended structure surrounding
  it. Limb-darkening effects are suggested by attempts to fit cosine
  model image profiles to the data. These fits have significant residuals
  at large radii suggesting a faint envelope extending from 1 to 5
  stellar radii.

Title: Secondary Condensational Instability
Authors: Goldberg, L. P.; Dahlburg, R. B.
Bibcode: 1986BAAS...18..991G
Altcode:
  No abstract at ADS

Title: Intermediate-coupling calculation of atomic spectra from
    hot plasma
Authors: Goldberg, A.; Rozsnyai, B. F.; Thompson, P.
Bibcode: 1986PhRvA..34..421G
Altcode:
  An algorithm is presented for the detailed computation of the spectral
  lines in hot, partially ionized plasmas in local thermodynamic
  equilibrium. The procedure uses the wave functions and state
  probabilities determined from the average atom model for microscopic
  configuration accounting. We use intermediate coupling to include the
  detailed structure of the bound-bound transition arrays. The model is
  applied to bromine plasma under such temperature and density conditions
  that partially filled L shells occur.

Title: Mass loss
Authors: Goldberg, Leo
Bibcode: 1986NASSP.492..245G
Altcode: 1986mts..book..245G
  Observational evidence for mass loss from cool stars is
  reviewed. Spectra line profiles are used for the derivation of mass-loss
  rates with the aid of the equation of continuity. This equation implies
  steady mass loss with spherical symmetry. Data from binary stars, Mira
  variables, and red giants in globular clusters are examined. Silicate
  emission is discussed as a useful indicator of mass loss in the middle
  infrared spectra. The use of thermal millimeter-wave radiation, Very
  Large Array (VLA) measurement of radio emission, and OH/IR masers are
  discussed as a tool for mass loss measurement. Evidence for nonsteady
  mass loss is also reviewed.

Title: The M-type stars
Authors: Johnson, Hollis Ralph; Querci, Francois R.; Jordan, Stuart;
   Thomas, Richard; Goldberg, Leo; Pecker, Jean-Claude
Bibcode: 1986NASSP.492.....J
Altcode: 1986mts..book.....J; 1986QB843.M16M89...
  No abstract at ADS

Title: Josif Shklovsky: A Personal Reflection
Authors: Goldberg, Leo
Bibcode: 1985S&T....70..109G
Altcode:
  No abstract at ADS

Title: Optical Spectroscopy of Red Giants (Review)
Authors: Goldberg, L.
Bibcode: 1985ASSL..117...21G
Altcode: 1985mlrg.proc...21G
  Accomplishments and problems in the study of mass loss from cool stars
  in the optical spectrum are reviewed. Accurate mass loss rates remain
  elusive principally because of inadequate knowledge of density, velocity
  and ionization structure in the circumstellar shells. Improved rates
  may be expected from binary star systems. Empirical rates derived for
  stars in globular clusters are found to be of doubtful validity. It
  is shown that optical observations can furnish important clues to the
  understanding of mass loss mechanisms.

Title: Reflections on the solar-stellar connection.
Authors: Goldberg, L.
Bibcode: 1985PASP...97..537G
Altcode:
  The achievements of optical astronomy in the investigation of the sun
  as a typical star in connection with the study of stellar evolution are
  reviewed, with emphasis given to the accomplishments of George Ellery
  Hale. Consideration is given to the discovery of magnetic fields on
  the sun; measurements of temperatures in the solar corona; and the
  early history of observational techniques for high dispersion solar
  spectroscopy. The development of satellite based astronomical devices
  such as the IUE, the Einstein Observatory, and the Space Telescope, is
  also considered. The construction of automatic photoelectric telescopes
  (APTs) for observations of variable stars is also discussed.

Title: Mass loss from cool stars.
Authors: Goldberg, L.
Bibcode: 1985fsgf.book..279G
Altcode: 1986fsgf.book..279G
  This review discusses (1) empirical determinations of mass loss rates
  for highly evolved cool stars, (2) some of the mechanisms that have been
  proposed to drive the flow, and (3) some aspects of stellar evolution,
  such as the formation of planetary nebulae.

Title: Interpreting Alpha Orionis Speckle Interferometry
Authors: Cheng, A.; Hege, K.; Strittmatter, P.; Goldberg, L.
Bibcode: 1984BAAS...16..939C
Altcode:
  No abstract at ADS

Title: Reflections on the solar-stellar connection.
Authors: Goldberg, L.
Bibcode: 1984BAAS...16..874G
Altcode:
  No abstract at ADS

Title: The variability of alpha Orionis.
Authors: Goldberg, L.
Bibcode: 1984PASP...96..366G
Altcode:
  A survey of variations in the radial-velocity and visual brightness
  of the star Betelgeuse (alpha-Orionis) over the last six decades is
  presented. On the basis of a comparison of the results of several
  observations, it is suggested that major disturbances in Betelgeuse's
  atmosphere are likely to occur in the year or two following the minimum
  in the six-year velocity curve. A coordinated observing program is
  proposed to take place during and after the next minimum, which is
  predicted to take place in early 1984. The desirable observations
  include multicolor photometry (particularly in the infrared),
  polarization measurements, and spectroscopy.

Title: Activity on Betelgeuse
Authors: Goldberg, L.
Bibcode: 1984Mercu..13...82G
Altcode:
  No abstract at ADS

Title: Introductory Remarks to the Session on Alpha Orionis and
    Related Topics
Authors: Goldberg, L.
Bibcode: 1984LNP...193..333G
Altcode: 1984csss....3..333G
  No abstract at ADS

Title: Founding of Kitt Peak
Authors: Goldberg, Leo
Bibcode: 1983S&T....65..228G
Altcode:
  No abstract at ADS

Title: Summary of the Colloquium
Authors: Goldberg, L.
Bibcode: 1983ASSL..102..653G
Altcode: 1983IAUCo..71..653G; 1983ards.proc..653G
  No abstract at ADS

Title: Remote Observing Origins
Authors: Goldberg, L.
Bibcode: 1983S&T....66..484G
Altcode:
  No abstract at ADS

Title: Possible origins for the 12 microns emission lines in the
    solar spectrum
Authors: Goldberg, L.
Bibcode: 1983ASSL..102..327G
Altcode: 1983IAUCo..71..327G; 1983ards.proc..327G
  The detection of about 40 unidentified emission lines near a
  wavelength of 12 microns in the solar spectrum has been reported
  by Braut and Noyes (1982, 1983). Braut and Noyes point out that
  these lines are a potentially powerful tool for magnetic field
  measurements in stars. It appears that the great widths of the
  absorption features in the strongest lines offer probably a strong
  clue to their identifications. The present investigation is concerned
  with two possible sources for the line broadening taking into account
  abundance broadening and autoionization.

Title: Prologue - Astronomy before the space age
Authors: Goldberg, L.
Bibcode: 1983ssst.book....1G
Altcode:
  Progress in astronomical and astrophysical knowledge since about 1900
  is traced, with a focus on the beginnings of space-based observations
  in the late 1950's. It is pointed out that observations were almost
  exclusively restricted to the visible spectrum unitl 1946. The unique
  possibilities offered by space observatories are listed, and the
  original plans for space-based studies of the earth, moon, planets,
  sun, and interplanetary space, as well as of phenomena beyond the solar
  system are reviewed. The direction of future space observations with
  the Space Telescope is indicated.

Title: An occultation angular diameter in Half light.
Authors: White, N. M.; Kreidl, T. J.; Goldberg, L.
Bibcode: 1982ApJ...254..670W
Altcode:
  The lunar occultation of 119 Tauri, spectral type M2 Ib, was observed
  in continuum light and in the light of the Ha absorption line. The
  restored strip-brightness distributions indicate that the Ha light
  comes from a region having at least twice the diameter of that producing
  the continuum light.

Title: Speckle interferometry of alpha Ori: preliminary results.
Authors: Goldberg, L.; Hege, E. K.; Hubbard, E. N.; Strittmatter,
   P. A.; Cocke, W. J.
Bibcode: 1982SAOSR.392B.131G
Altcode: 1982csss....2..131G
  No abstract at ADS

Title: Introductory Remarks at the Summary Session
Authors: Goldberg, L.
Bibcode: 1982obvf.conf..435G
Altcode:
  No abstract at ADS

Title: Reply to BOK - International Personal Contact as a Means for
    Enrichment of Science
Authors: Goldberg, L.; Gehrels, T.
Bibcode: 1982S&T....63..445G
Altcode:
  No abstract at ADS

Title: P CYG profiles in P Cyg.
Authors: Goldberg, L.
Bibcode: 1981A&A...104L...7G
Altcode:
  Attention is given to the proposal made by Underhill (1981) that
  two strong emission features near lambda 1306 and lambda 1309 in the
  spectrum of P Cygni are the result of dielectronic recombination through
  the autoionizing levels 3s3p3d 2F0 of Si II, giving rise to multiplet
  UV 13.04. It is found that the lines of this multiplet are closely
  blended with resonance lines of O I, Si II, and, to some extent,
  N I. It is shown that the observed spectrum may be accounted for by
  P Cygni profiles of the resonance lines and that, in the absence of
  corroborating qualitative calculations, the dielectronic recombination
  hypothesis is unjustified.

Title: Outflow of Matter in the Chromosphere of Alpha-Orionis
Authors: Goldberg, L.
Bibcode: 1981ASSL...89..111G
Altcode: 1981emls.proc..111G; 1981IAUCo..59..111G
  No abstract at ADS

Title: Book-Review - Beyond the Atmosphere
Authors: Newell, H. E.; Goldberg, L.
Bibcode: 1981S&T....62..474N
Altcode:
  No abstract at ADS

Title: Acceleration of mass flow in the chromosphere of Alpha Orionis
Authors: Goldberg, L.
Bibcode: 1981ASSL...88..301G
Altcode: 1981pprg.work..301G
  The spectrum of Alpha Orionis is composite and consists of four
  components arising from the photosphere, two distant shells expanding
  at constant velocities differing by 6-7 km/s, and a warm chromosphere
  in which the mass flow is being accelerated, perhaps to its terminal
  value in the inner shell. Calculations are presented on the feasibility
  of direct observational determinations of the heights and thicknesses
  of the chromospheric regions in bright giants and supergiants, using
  the technique of speckle interferometry and lunar occultations

Title: Solar physics
Authors: Goldberg, L.
Bibcode: 1981ssca.proc...14G
Altcode:
  The history of U.S. solar exploration is recounted. The state
  of knowledge concerning solar physics prior to World War II is
  discussed as a background, and the use of V-2 rockets after the war
  to penetrate the ozone layer and make observations is described. The
  use of Solar-scopes in the post-Sputnik, pre-NASA days, and the
  findings made with them, are discussed along with the efforts of the
  National Academy of Sciences. Finally, the NASA Orbiting Astronomical
  Observatory satellite program is reported on, both its history and
  its accomplishments in solar physics. The engineering involved in the
  missions is also discussed.

Title: Observations of the Outer Atmospheric Regions of Alpha-Orionis
Authors: Bernat, A. P.; Goldberg, L.
Bibcode: 1980LNP...114..278B
Altcode: 1980sttu.coll..278B; 1980IAUCo..51..278B
  No abstract at ADS

Title: Scientific Need for Space Astronomy
Authors: Goldberg, L.
Bibcode: 1980HiA.....5...63G
Altcode:
  No abstract at ADS

Title: Complementarity Between Space and Ground-Based Developments:
    Overview
Authors: Goldberg, L.
Bibcode: 1980oits.conf..129G
Altcode:
  No abstract at ADS

Title: Panel Discussion: Space VS. Ground-Competition or Collaboration
Authors: Goldberg, L.; Gursky, H.; O'dell, C.; Strittmatter, P.;
   Wampler, J.; Strom, S.
Bibcode: 1980oits.conf.1151G
Altcode:
  No abstract at ADS

Title: Motions in the Atmosphere of Alpha Orionis
Authors: Goldberg, L.; Testerman, L.; Willmarth, D.
Bibcode: 1979BAAS...11..682G
Altcode:
  No abstract at ADS

Title: Some problems connected with mass loss in late-type stars
Authors: Goldberg, L.
Bibcode: 1979QJRAS..20..361G
Altcode:
  Observational and theoretical evidence for mass loss from various
  types of stars are summarized, and mechanisms for its generation
  are described, including shock waves, thermally driven winds, and
  radiation-driven winds with laminar flow. In particular, spectroscopic
  observations of Alpha Orionis are reported, and the K I, Ca II, and H
  I lines show that its atmosphere is divided into at least three zones:
  a photosphere fluctuating in both brightness and radial velocity, an
  expanding chromosphere hot enough (temperature on the order of 1000 K)
  to emit strong Balmer-line radiation and uncoupled from motions in the
  photosphere, and a cold, distant circumstellar shell. Furthermore,
  the 5.781 yr period for the mean radial velocity variation of the
  photosphere is found to be correct to within about 0.5%, and the flow
  of matter away from the star appears to begin in the chromosphere,
  where it is accelerated to about 50% of its terminal value.

Title: Astronomy in China. A trip report of the American Astronomy
    Delegation
Authors: Goldberg, Leo; Edward, Lois
Bibcode: 1979actr.book.....G
Altcode:
  No abstract at ADS

Title: American Astronomers Visit China II
Authors: Goldberg, Leo
Bibcode: 1978S&T....56..383G
Altcode:
  No abstract at ADS

Title: American Astronomers Visit China I
Authors: Goldberg, Leo
Bibcode: 1978S&T....56..279G
Altcode:
  No abstract at ADS

Title: Kitt Peak National Observatory, Tucson, Arizona; Cerro Tololo
    Inter-American Observatory, La Serena, Chile. Reports.
Authors: Goldberg, L.; Blanco, V.
Bibcode: 1978BAAS...10..152G
Altcode:
  No abstract at ADS

Title: Observations of the mid-latitude lower ionosphere in winter
Authors: Aikin, A. C.; Goldberg, R. A.; Jones, W.; Kane, J. A.
Bibcode: 1977JGR....82.1869A
Altcode:
  Rocket observations of the lower ionosphere in the winter of 1971 at two
  locations show differences of electron density which are attributed to
  enhancements of nitric oxide and energetic electron fluxes precipitated
  into the mesosphere during the poststorm phase of a geomagnetic
  storm. Electron density distributions were observed above Wallops
  Island, Virginia, and Keweenaw, Michigan, larger values occurring
  at Keweenaw. Energetic electron fluxes were greater at Keweenaw (L =
  3.9) than at Wallops Island (L = 2.5). While particle ionization was
  the dominant factor in establishing the electron density during one
  measurement at Keweenaw, particles were not present 2 days earlier,
  even though the electron density distribution was significantly
  larger than that observed at Wallops Island on both occasions. An
  accompanying ion composition profile measured at Keweenaw during the
  earlier flight showed NO<SUP>+</SUP> to be the dominant ion to 76 km,
  where the concentration of hydrated ions, H<SUB>3</SUB>O<SUP>+</SUP>
  · (H<SUB>2</SUB>O)<SUB>n</SUB>, exceeded that of NO<SUP>+</SUP>. This
  lowering of the transition height from NO<SUP>+</SUP> to hydrated
  species is in agreement with independent observations of D region ion
  composition during anomalous winter conditions.

Title: Donald Howard Menzel
Authors: Goldberg, Leo
Bibcode: 1977S&T....53..244G
Altcode:
  No abstract at ADS

Title: Observations of K I Line Emission in the Circumstellar Shell
    of Alpha Orionis.
Authors: Lynds, C. R.; Harvey, J. W.; Goldberg, L.
Bibcode: 1977BAAS....9Q.345L
Altcode:
  No abstract at ADS

Title: Kitt Peak National Observatory, Tucson, Arizona; Cerro Tololo
    Inter-American Observatory, La Serena, Chile. Observatory reports.
Authors: Goldberg, L.
Bibcode: 1976BAAS....8..129G
Altcode:
  No abstract at ADS

Title: High-resolution profiles of sodium and potassium lines in
    Alpha Orionis.
Authors: Goldberg, L.; Ramsey, L.; Testerman, L.; Carbon, D.
Bibcode: 1975ApJ...199..427G
Altcode:
  Profiles of the K I resonance line at 7698.98 A and of the D1
  and D2 lines of Nai in the spectrum of a Ori have been recorded
  photoelectrically using the main beam of the McMath solar telescope
  at KPNO. The Na lines were observed in the fourth order of the
  spectrograph and the K iline in the third order, providing a resolving
  power of approximately 50 mA. The observed profiles are consistent with
  a model in which radiation from the stellar photo sphere is scattered
  and reemitted by an expanding envelope or envelopes of radius large
  compared with that of the photosphere. Each blueshifted absorption
  core appears to consist of two components of approximately the same
  intensity. The first has a heliocentric radial velocity of + 11-13 km ,
  which agrees very well with measurements of other resonance lines by
  other observers, whereas the second is in the range + 6 km 1 and appears
  not to have been detected previously. Subject headings: circumstellar
  shells - late-type stars - stellar winds - stars, individual

Title: High Resolution Profiles of Sodium and Potassium Lines in
    α Orionis.
Authors: Goldberg, L.; Ramsey, L.; Testerman, L.; Carbon, D.
Bibcode: 1975BAAS....7..233G
Altcode:
  No abstract at ADS

Title: Circumstellar shells around cool stars.
Authors: Goldberg, L.
Bibcode: 1975MSRSL...9..387G
Altcode: 1975assp.conf..387G; 1975apes.conf..387G
  The study of mass loss from red giants, as revealed by shells of
  gas and dust surrounding the stars, is aimed at establishing the
  mechanism by which red giants may evolve noncatastrophically to the
  white dwarf stage, while at the same time providing a source for the
  replenishment of interstellar gas used in star formation. The principal
  methods of deriving rates of mass loss from late-type stars, i.e.,
  by optical spectroscopy and by measurements of infrared radiation
  from circumstellar dust, are summarized and it is suggested that
  present estimates of the loss rates may be in error by factors of from
  2-10. Some new results, which have recently been obtained at the Kitt
  Peak and McDonald Observatories, illustrate the importance of achieving
  very high spectroscopic resolution as a basis for understanding the
  structure and dynamics of circumstellar shells. New observations of
  the profiles of the Na I and K I lines in Alpha Orionis will be shown
  as examples.

Title: Synchronous Mode-Locked Dye Lasers for Picosecond Spectroscopy
    and Nonlinear Mixing
Authors: Goldberg, L. S.; Moore, C. A.
Bibcode: 1975LNP....43..248G
Altcode: 1975lasp.conf..248G
  No abstract at ADS

Title: Research with Solar Satellites
Authors: Goldberg, Leo
Bibcode: 1974ApJ...191....1G
Altcode:
  Subject headings: chromospheres, solar - corona, solar - granules
  and supergranules, solar - hydromagnetics - magnetic fields, solar -
  solar activity - spectroheliograms - Sun - ultraviolet - X-rays

Title: The Harvard Experiment on OSO-6: Instrumentation, Calibration,
    Operation, and Description of Observations
Authors: Huber, Martin C. E.; Dupree, A. K.; Goldberg, Leo; Noyes,
   R. W.; Parkinson, W. H.; Reeves, E. M.; Withbroe, George L.
Bibcode: 1973ApJ...183..291H
Altcode:
  The Harvard experiment carried by OS 0-6 was an extreme-ultraviolet
  (EUV) spectrometerspectroheliometer with wavelength range 285-1385 A,
  spatial and spectral bandwidth 35 x 35 (arc sec)2 and 3 A, respectively;
  the instrumeflt acquired data that have been deposited with the National
  Space Science Data Center and World Data Center A at the Goddard Space
  Flight Center in Greenbelt, Maryland, and are now available in their
  entirety to the scientific community. This paper describes aspects
  of the experiment that are relevant to potential users of the data:
  instrument configuration and parameters, laboratory and inflight
  calibrations, as well as operational capabilities and procedures. We
  also report the observations obtained and, where relevant, list
  the nature, number, and dates of observations. Subject headings:
  atmospheres, solar - instruments - solar activity - spectra, solar -
  spectra, ultraviolet

Title: Kitt Peak National Observatory, Tucson, Arizona and Cerro
    Tololo Inter-American Observatory, La Serena, Chile. Observatory
    reports.
Authors: Goldberg, L.
Bibcode: 1973BAAS....5Q.142G
Altcode:
  No abstract at ADS

Title: Kitt Peak National Observatory, Tucson, Arizona; Cerro Tololo
    Inter-American Observatory, La Serena, Chile. Observatory reports.
Authors: Goldberg, L.
Bibcode: 1973BAAS....5R.142G
Altcode:
  No abstract at ADS

Title: Annual Review of Astronomy and Astrophysics, Vol._11.
Authors: Goldberg, L.; Layzer, D.; Phillips, J. G.
Bibcode: 1973ARA&A..11.....G
Altcode:
  No abstract at ADS

Title: HIGH-n Balmer Transitions in Gaseous Nebulae
Authors: Goad, L. E.; Goldberg, L.; Greenstein, Jesse L.
Bibcode: 1972ApJ...175..117G
Altcode:
  The intensities of the Balmer lines arising from levels with principal
  quantum number n &gt; 15, and the intensity of the apparent continuum
  formed by the overlapping of the Balmer lines, have been measured in
  the Orion Nebula (NGC 1976) and the planetary nebula NGC 7027. These
  observed intensities have been compared with the predictions of
  Brocklehurot's recombination theory in order to deduce the electron
  temperature and density of the nebulae. We find that % = 8600 +
  1500 K and logjo N, = 4.1 + 0.3 for NGC 1976 and that T, = 69000 +
  15000 K and logio AT, = 5.6 + 0.3 for NGC 7027.

Title: Harvard College Observatory, Cambridge,
    Massachusetts. Observatory report.
Authors: Goldberg, L.
Bibcode: 1972BAAS....4...40G
Altcode:
  No abstract at ADS

Title: Infrared and microwave emission from nebulae in the Galaxy.
Authors: Goldberg, L.
Bibcode: 1972saim.conf..315G
Altcode:
  No abstract at ADS

Title: Annual Review of Astronomy and Astrophysics, Vol._10.
Authors: Goldberg, L.; Layzer, D.; Phillips, J. G.
Bibcode: 1972ARA&A..10.....G
Altcode:
  No abstract at ADS

Title: Coronal Electron Density Maps for 7 March, 1970, Derived from
    Mgx λ625 Spectroheliograms (Papers presented at the Proceedings
    of the International Symposium on the 1970 Solar Eclipse, held in
    Seattle, U. S. A. , 18-21 June, 1971.)
Authors: Withbroe, G. L.; Dupree, A. K.; Goldberg, L.; Huber,
   M. C. E. .; Noyes, R. W.; Parkinson, W. H.; Reeves, E. M.
Bibcode: 1971SoPh...21..272W
Altcode:
  We have analyzed daily Mgx λ 625 spectroheliograms acquired by the
  Harvard College Observatory experiment on OSO-6 for a 28-day period
  centered on 7 March, 1970, the date of a well-observed total solar
  eclipse. These data are used to construct maps of the variation across
  the solar disk of the electron density at the base of the corona. The
  correspondence of high and low density regions with regions of enhanced
  and reduced emission in white light and Mgx pictures made during or
  near the time of the eclipse are described.

Title: Rocket Observations of the Ultraviolet Solar Spectrum during
    the Total Eclipse of 1970 March 7
Authors: Gabriel, A. H.; Garton, W. R. S.; Goldberg, L.; Jones,
   T. J. L.; Jordan, Carole; Morgan, F. J.; Nicholls, R. W.; Parkinson,
   W. J.; Paxton, H. J. B.; Reeves, E. M.; Shenton, C. B.; Speer, R. J.;
   Wilson, R.
Bibcode: 1971ApJ...169..595G
Altcode:
  A sequence of thirty-five ultraviolet photographic spectra of the
  Sun has been obtained in the wavelength region 850-2190 A, as a
  function of time during the eclipse. These cover the range from before
  second contact until midtotality, with a spatial resolution of the
  order 2 arc sec. A general description of the experiment and data is
  given. Twenty-five new coronal lines have been seen, the majority of
  which have been identified as new forbidden transitions. The La corona
  is observed out to over 1.5 R0, and a quantitative interpretation
  is presented. Analyses of other features-e.g., prominences,
  quiet-atmosphere structure, and coronal condensations-are continuing.

Title: Radio Recombination Lines
Authors: Goldberg, Leo
Bibcode: 1971spas.conf..169G
Altcode:
  No abstract at ADS

Title: Balmer line intensities near the series limit in gaseous
    nebulae.
Authors: Goad, L. E.; Goldberg, L.; Greenstein, J. L.
Bibcode: 1971BAAS....3..417G
Altcode:
  No abstract at ADS

Title: In Retrospect
Authors: Goldberg, Leo
Bibcode: 1971dngp.conf..147G
Altcode:
  No abstract at ADS

Title: Atoms, stars, and nebulae
Authors: Aller, Lawrence Hugh; Goldberg, Leo
Bibcode: 1971asn..book.....A
Altcode: 1971QB461.A568.....
  No abstract at ADS

Title: Harvard College Observatory, Cambridge, Massachusetts. Report
    1969-1970.
Authors: Goldberg, L.
Bibcode: 1971BAAS....3...78G
Altcode:
  No abstract at ADS

Title: The interpretation of XUV solar radiation.
Authors: Goldberg, L.
Bibcode: 1971adiu.conf..476G
Altcode:
  No abstract at ADS

Title: The Interpretation of XUV Solar Radiation
Authors: Goldberg, L.
Bibcode: 1971HiA.....2..476G
Altcode:
  No abstract at ADS

Title: Annual Review of Astronomy and Astrophysics, Vol.9.
Authors: Goldberg, L.; Layzer, D.; Phillips, J. G.
Bibcode: 1971ARA&A...9.....G
Altcode:
  No abstract at ADS

Title: Summary
Authors: Goldberg, L.
Bibcode: 1971ASSL...27..333G
Altcode: 1971psc..conf..333G
  No abstract at ADS

Title: Detection and Identification of Recombination Lines from an
    H i Region
Authors: Ball, J. A.; Cesarsky, D.; Dupree, A. K.; Goldberg, L.;
   Lilley, A. E.
Bibcode: 1970ApJ...162L..25B
Altcode:
  The H157a line arising from an H I region has been observed in the
  spectrum of NGC 2024 (Orion B). The measured frequency separation
  between this line and the anomalous line at 157a allows a firm
  identification of the anomalous emitter as carbon. The fraction of
  ionized hydrogen in this H I cloud is found to be (2.7 i 1.8) x 1O .

Title: The Analysis of Microwave Recombination Lines
Authors: Goldberg, L.; Cesarsky, D.
Bibcode: 1970ApL.....6...93G
Altcode:
  No abstract at ADS

Title: OSO-VI: Surges, Flares, and the Development of Active Regions
Authors: Reeves, E. M.; Dupree, A. K.; Goldberg, L.; Huber, M. C. E.;
   Noyes, R. W.; Parkinson, W. H.; Withbroe, G. L.
Bibcode: 1970BAAS....2R.215R
Altcode:
  No abstract at ADS

Title: OSO-VI: The EUV Spectrum of Solar-Active Regions
Authors: Dupree, A. K.; Goldberg, L.; Huber, M. C. E.; Noyes, R. W.;
   Parkinson, W. H.; Reeves, E. M.; Withbroe, G. L.
Bibcode: 1970BAAS....2..191D
Altcode:
  No abstract at ADS

Title: OSO-VI: The Harvard Experiment
Authors: Huber, M. C. E.; Dupree, A. K.; Goldberg, L.; Noyes, R. W.;
   Parkinson, W. H.; Reeves, E. M.; Withbroe, G. L.
Bibcode: 1970BAAS....2S.200H
Altcode:
  No abstract at ADS

Title: Harvard College Observatory, Cambridge, Massachusetts. Report
    1968-1969.
Authors: Goldberg, L.
Bibcode: 1970BAAS....2...43G
Altcode:
  No abstract at ADS

Title: Recombination Lines in NGC 7027
Authors: Goldberg, L.
Bibcode: 1970ApL.....5..151G
Altcode:
  No abstract at ADS

Title: Annual Review of Astronomy and Astrophysics.
Authors: Goldberg, L.; Layzer, D.; Phillips, J. G.
Bibcode: 1970ARA&A...8.....G
Altcode:
  No abstract at ADS

Title: Radiofrequency Recombination Lines
Authors: Dupree, A. K.; Goldberg, Leo
Bibcode: 1970ARA&A...8..231D
Altcode:
  No abstract at ADS

Title: Stimulated Emission of Recombination Lines in H i Regions
Authors: Dupree, A. K.; Goldberg, Leo
Bibcode: 1969ApJ...158L..49D
Altcode:
  Radio-frequency recombination lines arising from ionized atoms in
  H i regions can have intensities which are greatly strengthened
  over their equilibrium values as a result of stimulated emission
  due to a background continuum. It is suggested that the "anomalous"
  recombination line is formed in this way. In addition, hydrogen and
  helium recombination lines from H ii regions are expected to have
  components formed in H i clouds. Recombination lines may also be
  observable from H i clouds that are in the line of sight to nonthermal
  continuum sources. Such lines can be used to give a direct measure of
  the degree of ionization and abundances in the interstellar medium

Title: Absorption and Emission of Recombination Radiation by H
    I Regions
Authors: Dupree, A. K.; Goldberg, Leo
Bibcode: 1969BAAS....1..340D
Altcode:
  No abstract at ADS

Title: Ultraviolet Astronomy
Authors: Goldberg, Leo
Bibcode: 1969SciAm.220f..92G
Altcode: 1969SciAm.220...92G
  No abstract at ADS

Title: 28.The Infrared Emission of Planetary Nebulae
Authors: Goldberg, L.
Bibcode: 1969LIACo..15..283G
Altcode: 1969MSRSL..17..283G
  No abstract at ADS

Title: Harvard College Observatory, Cambridge, Massachusetts. Report
    1967-1968.
Authors: Goldberg, L.
Bibcode: 1969BAAS....1...20G
Altcode:
  No abstract at ADS

Title: Ultraviolet Solar Images from Space
Authors: Goldberg, Leo; Noyes, Robert W.; Parkinson, William H.;
   Reeves, Edmond M.; Withbroe, George L.
Bibcode: 1968Sci...162...95G
Altcode:
  No abstract at ADS

Title: Erratum: Stimulated Emission of Radio-Frequency Lines of
    Hydrogen
Authors: Goldberg, Leo
Bibcode: 1968ApJ...151..804G
Altcode:
  No abstract at ADS

Title: A Description of the Harvard Experiment on OSO-IV
Authors: Reeves, E. M.; Goldberg, L.; Parkinson, W. H.
Bibcode: 1968AJS....73S..74R
Altcode:
  The recent Orbiting Solar Observatory, OSO-I V, contained
  a photoelectric spectrometer-spectroheliometer in the pointed
  section. The instrument has recorded the solar spectrum from a region
  of 1 min of arc at the center of the solar disk over the wavelength
  region XX 300-1400. The spectrometer can select any single wavelength
  in the above range and, using the raster mode of the satellite,
  construct a spectroheliogram with a resolution of 1 min of arc. The
  optical system, calibration, and operation will be described with
  representative samples of data. A unique "quick-look" system has been
  used which allows the experimenter to receive an entire orbit's data
  in Cambridge within a few minutes and to respond with revised command
  sequences on an orbit-by-orbit basis for six consecutive satellite
  passes per day. The operational mode of the instrument can thus be
  adjusted to take full advantage of current activity on the solar disk.

Title: Buchbesprechungen über: Annual Review of Astronomy and
    Astrophysics. (Ed. L. GOLDBERG, D. LAYZER, and J. G. PHILLIPS)
    (Ref. A. UNSÖLD)
Authors: Goldberg, L.; Layzer, D.; Phillips, J. G.
Bibcode: 1968ZA.....68..167G
Altcode:
  No abstract at ADS

Title: Predicted Infrared Line Spectrum of NGC 7027.
Authors: Goldberg, Leo
Bibcode: 1968AJS....73R.178G
Altcode:
  The strong infrared emission observed in the spectra of NGC 7027 and
  other objects makes it important to investigate possible sources of
  line emission in the spectral region 1Oi3~lOi4 Hz. Delmer, Gould, and
  Ramsey (1967) have calculated the expected intensities of magnetic
  dipole transitions between fine-structure levels of the ground
  terms of p-electron configurations. In this paper we estimate the
  intensities both of similar transitions in d-electron configurations
  and of recombination lines of hydrogen. The strongest lines in the
  d-electron group are those of [Fe v~, [Fe YI~, and [Fe YIIJ, which
  also show lines in the visible spectrum.

Title: Observations Astronorniques au-dehors de 1'Atmosphère
    Terrestre (Astronomical Observations from outside the Terrestrial
    Atmosphere)
Authors: Goldberg, L.
Bibcode: 1968IAUTB..13..215G
Altcode:
  No abstract at ADS

Title: Buchbesprechungen über: Annual Review of Astronomy and
    Astrophysics. (Ed. L. GOLDBERG, D. LAYZER, and J. G. PHILLIPS)
    (Ref. A. UNSÖLD)
Authors: Goldberg, L.; Layzer, D.; Phillips, J. G.
Bibcode: 1968ZA.....69..385G
Altcode:
  No abstract at ADS

Title: The Infrared Emission of NGC 7027
Authors: Goldberg, L.
Bibcode: 1968ApL.....2..101G
Altcode:
  No abstract at ADS

Title: Theoretical intensities of recombination lines.
Authors: Goldberg, L.
Bibcode: 1968tirl.book.....G
Altcode:
  No abstract at ADS

Title: Preliminary EUV Spectroheliograms from OSO-IV
Authors: Noyes, R. W.; Goldberg, L.; Parkinson, W. H.; Reeves, E. M.;
   Withbroe, G. L.
Bibcode: 1968AJS....73R..73N
Altcode:
  The Harvard OSO-I V spectrometer-spectroheliometer has provided pictures
  of the sun over a wide range of wavelengths originating from different
  heights in the solar atmosphere, from the low chromosphere through the
  corona. Lines from H I through Si XII have been observed against the
  solar disk showing structure on the disk both in active regions and, in
  certain cases, well above the limb. The data allow a close comparison
  with simultaneous ground-based coronal observations. Representative
  spectroheliograms in lines of increasing ionization potentials are
  used to illustrate the size, structure, and development of active
  regions on the limb and on the disk at different heights in the solar
  atmosphere. Preliminary observations of limb brightening, instensity
  of active regions, and flare activity are presented.

Title: Theoretical Intensities of Recombination Lines
Authors: Goldberg, Leo
Bibcode: 1968iih..conf..373G
Altcode:
  No abstract at ADS

Title: Population of Atomic Levels by Dielectronic Recombination
Authors: Goldberg, Leo; Dupree, Andrea K.
Bibcode: 1967Natur.215...41G
Altcode:
  IN the preceding communication, Palmer et al. have reported the
  observation of an emission line close to the expected position of the
  recombination line 109α of C I in the radiofrequency spectra of the
  ionized hydrogen regions NGC 2024 and IC 1795. The total intensity of
  the newly observed line is about 3 per cent that of the neighbouring
  109α line of H I. Let us assume that the two lines originate from the
  same volume of space. If the upper levels of C I and H I were populated
  in thermodynamic equilibrium, the relative intensities of the two lines
  would be roughly in the ratio of the numbers of hydrogen and carbon
  ions in the emitting volume. This ratio would be equivalent to that
  of the cosmic abundances of hydrogen and carbon if both atoms were
  entirely in the singly ionized condition. In the Sun, the abundance
  of carbon is 5 × 10<SUP>-4</SUP> of that of hydrogen<SUP>1</SUP>,
  and there is no reason to suppose that the ratio is greatly different
  in H II regions. Thus, if the line found by Palmer et al. is indeed
  the 109α line of C I, its observed intensity relative to that of the
  same transition in hydrogen is at least sixty times greater than would
  be expected from the two assumptions of thermodynamic equilibrium and
  normal cosmic abundances. In this communication we point out that the
  apparently anomalous overpopulation of the n = 110 level of C I can be
  explained as a result of departures from thermodynamic equilibrium,
  which result in the preferential population of levels of high total
  quantum number by dielectronic recombination.

Title: Solar Abundance Determination from Ultraviolet Emission Lines
Authors: Dupree, Andrea K.; Goldberg, Leo
Bibcode: 1967SoPh....1..229D
Altcode:
  The intensities of far ultraviolet emission lines from the solar corona
  are analyzed to determine relative coronal abundances for oxygen,
  silicon, and iron. Dielectronic recombination is included in the
  formulation of ionization equilibrium. Observations of solar radio
  emission are used to obtain abundances relative to hydrogen. The
  absolute coronal abundances appear to be in agreement with their
  respective photospheric values. General properties of the structure of
  the chromosphere and corona are deduced from the analysis of observed
  emission in the ultraviolet and radio wavelength regions.

Title: Space Solar Physics
Authors: Goldberg, L.
Bibcode: 1967sp...conf..493G
Altcode:
  No abstract at ADS

Title: Ultraviolet and X Rays from the Sun
Authors: Goldberg, Leo
Bibcode: 1967ARA&A...5..279G
Altcode:
  No abstract at ADS

Title: Population of Atomic Levels by Dielectronic Recombination.
Authors: Goldberg, Leo; Dupree, Andrea K.
Bibcode: 1967AJ.....72Q.799G
Altcode:
  Under conditions found in H II regions, the populations of excited
  levels of atoms are determined primarily by the balance between
  electronic recombination and cascade into the levels and spontaneous
  transitions out of them. The bare nucleus of a hydrogenic ion can
  combine only by radiative capture but an ion that has one or more
  electrons can capture an electron by dielectronic recombination. This
  process may occur at a much faster rate and with a wholly different
  dependence on n and 1 than that of radiative capture. Illustrative
  calculations have been performed for Ca I in which the levels are
  assumed to be populated by dielectronic and three-body recombination
  and cascade, and to be depopulated by spontaneous downward transitions
  and collisional ionization. The results show that (1) the capture
  of electrons by dielectronic recombination can greatly increase the
  populations of highly excited levels as compared with their equilibrium
  values; (2) there will be a value of the total quantum number n for
  which bn, the ratio of the actual population to that in thermodynamic
  equilibrium, has a maximum value. This maximum occurs at n~50 to 100
  for Ne=104 cm-3 and at n~100 to 200 for Ne=102 cm-3 (3) recombination
  lines from complex atoms should be found in emission and, with the
  appropriate conditions, in absorption.

Title: On the Infrared Continuum of the Sun and Stars
Authors: Noyes, Robert W.; Gingerich, Owen; Goldberg, Leo
Bibcode: 1966ApJ...145..344N
Altcode:
  No abstract at ADS

Title: Stimulated Emission of Radio-Frequency Lines of Hydrogen
Authors: Goldberg, Leo
Bibcode: 1966ApJ...144.1225G
Altcode:
  No abstract at ADS

Title: Astrophysical Implications of Autoionization
Authors: Goldberg, Leo
Bibcode: 1966aatl.conf....1G
Altcode:
  No abstract at ADS

Title: The Sun and Solar Physics
Authors: Goldberg, Leo
Bibcode: 1966aes..conf....3G
Altcode:
  No abstract at ADS

Title: Buchbesprechungen über: Annual Review of Astronomy and
    Astrophysics. Vol. 3. (Ed. GOLDBERG, L. , A. J. DEUTSCH und D. LAYZER)
    (Ref. A. UNSÖLD)
Authors: Goldberg, L.; Deutsch, A. J.; Layzer, D.
Bibcode: 1966ZA.....64..370G
Altcode:
  No abstract at ADS

Title: Observations Astronomiques au-dehors de l'Atmosphère Terrestre
    (Astronomical Observations from outside the Terrestrial Atmosphere)
Authors: Goldberg, L.
Bibcode: 1966IAUTB..12..371G
Altcode:
  No abstract at ADS

Title: Observational Requirements for a Theory of Formation of H
    and K Lines
Authors: Goldberg, L.
Bibcode: 1965SAOSR.174..389G
Altcode:
  No abstract at ADS

Title: Carbon Monoxide in the Ultraviolet Solar Spectrum.
Authors: Goldberg, L.; Parkinson, W. H.; Reeves, E. M.
Bibcode: 1965ApJ...141.1293G
Altcode:
  No abstract at ADS

Title: Collisional excitation of autoionizing levels
Authors: Goldberg, L.; Dupree, A. K.; Allen, J. W.
Bibcode: 1965AnAp...28..589G
Altcode:
  No abstract at ADS

Title: A Study of Broad Absorption Features in the Solar Spectrum.
Authors: Goldberg, Leo; Newsom, Gerald; Parkinson, W. H.; Reeves, E. M.
Bibcode: 1965AJ.....70R.676G
Altcode:
  The broad depressions (2.6 A wide) in the solar spectrum at X
  6362 and 6343 have recently been identified (Mitchell and Mohler,
  Astrophys. J. 141, 1126, 1965) as the auto-ionizing transitions 3d4p
  3F0 -3d4d 3G in neutral calcium. A shock tube was used to determine the
  gf values of these lines and preliminary values have been derived. The
  McMath Solar Telescope at the Kift Peak National Observatory was used to
  observe these lines and to search for other broad absorptions. At the
  center of the disk, the depressions for the 6362 and 6343 A lines were
  4.3~0.1% and 2.8*0.2%, respectively, while near the limb (~=0.2) the
  percentage depression decreased by 17%. Spectra of cool, highluminosity
  stars, kindly loaned by Mount Wilson and Palomar Observatories, also
  showed these auto-ionizing lines. Several other broad depressions
  which have been observed in the sun are discussed.

Title: Simultaneous Shock Tube Measurements of Fe and CR F values
    of Astronomical Interest.
Authors: Goldberg, Leo; Huber, Martin; Parkinson, W. H.; Reeves,
   E. M.; Tobey, F. L.
Bibcode: 1965AJ.....70Q.676G
Altcode:
  Measurements of relative f values of selected iron and chromium lines
  have been made in the wavelength range 3200 to 3800 A. Line strengths
  were measured photographically by absorption through the region
  behind a reflected shock in a pressure-driven shock tube with a wide
  spectrograph slit. Temperatures were determined from the brightness
  and emissivity of the shocked gas. Low concentrations of iron and
  chromium were introduced together as carbonyls, premixed with the
  argon test gas. This was done to ensure the equal processing of both
  atoms and to reduce systematic errors in the ratios of oscillator
  strengths of the two elements. Populations of the absorbing levels
  were determined from the Saha-Boltzmann equation, the hydrodynamic
  equations and the charge neutrality condition. The experimental
  uncertainties are 15% or better. The f value ratios obtained agree
  within a factor of 2 with ratios computed from literature f values
  adapted to a common scale (Corliss, C. H., and Bozmann, W. R.,
  Natl. Bur. Stds. Monograph 53, 1962, for Cr; Corliss, C. H., and
  Warner, B., Astrophys. J. Suppl. No. 83, 1964 for Fe). The technique
  of simultaneous measurements of relative f values yields consistent
  oscillator strengths for two elements and provides data for an accurate
  relative abundance determination.

Title: Collisional excitation of auto-ionizing levels
Authors: Goldberg, L.; Dupree, A. K.; Allen, J. W.
Bibcode: 1965IAUS...23..125G
Altcode:
  No abstract at ADS

Title: The Abundance of Iron in the Solar Photosphere.
Authors: Goldberg, Leo; Kopp, Roger A.; Dupree, Andrea K.
Bibcode: 1964ApJ...140..707G
Altcode:
  New laboratory measurements of the absolute f-values of Fe 1 lines by
  Corliss and Warner (1964) have made possible a new determination of
  the abundance of iron in the solar photosphere. Of the 628 lines used
  to obtain the curve of growth by the method of weighting functions,
  the majority fall on the linear branch of the curve and have lower
  excitation potentials in the range 3-5 eV. Since their mean optical
  depths of formation are as large as 0.6, it seems unlikely that the
  lines are significantly affected by departures from LTE. The resulting
  abundances appear to be independent of excitation potential, but seem
  to increase slightly with increasing wavelength. The average value
  of the derived abundance, log NF,/NH + 12 00 = 6.64, is in very good
  agreement with other modern determinations.

Title: The Origin of the Emission Reversals in the Fraunhofer h-
    and K-Lines
Authors: Goldberg, Leo
Bibcode: 1964ApJ...140..384G
Altcode:
  No abstract at ADS

Title: Origin of Emission Cores in Lines of Ionized Calcium and
    Magnesium.
Authors: Goldberg, Leo; Noyes, Robert W.
Bibcode: 1964AJ.....69R.542G
Altcode:
  Transitions between doubly excited 4pnl levels and singly excited 4snl
  levels of the Ca I atom are shown to be probable contributors to the
  emission cores of the Ca II H and K lines in the solar spectrum. The
  contribution to the source function from this process is calculated
  and found to reach a maximum at a height of approximately 300 km
  above the photosphere. Preliminary calculations of line profiles and
  center-to-limb variations for the H and K lines of both Ca II and Mg
  ii are presented and discussed.

Title: Preliminary Results from a Rocket Flight of the Harvard
    OSO-B Spectrometer.
Authors: Goldberg, Leo; Parkinson, W. H.; Reeves, E. M.; Noyes, R. W.
Bibcode: 1964AJ.....69Q.140G
Altcode:
  A model of the Harvard OSO-B spectrometer was flown in an Aerobee-Hi
  rocket from White Sands, New Mexico on 6 September 1963. During the
  course of the rocket flight, which attained a peak altitude of 221 km,
  three full scans and part of a fourth were obtained in the spectral
  region 1350-500 A. The dimensions of the entrance slit were 1.8 arc
  minutes wide by 9.0 arc minutes long. Examination of Ha and Ca K
  spectroheliograms shows that the entrance aperture was free of plage
  regions. The purpose of the flight was primarily to check the absolute
  calibration prior to launch of a similar instrument in OSO-B and also
  to obtain data on spectral intensities for the center of the quiet
  sun. Essentially all emission lines found by other experimenters were
  observed and good records were also obtained of the Lyman continuum. In
  general, the observed numbers of counts recorded for the emission lines
  are in satisfactory agreement with those predicted on the basis of
  published data on photon fluxes and the absolute laboratory calibration,
  but there are interesting differences which can be attributed at least
  in part to the fact that the present observations refer to the center of
  the quiet sun, whereas H interegger `s observations, for example, apply
  to the integrated flux from the whole sun, including active regions.

Title: The Abundance of He<SUP>3</SUP> in the Sun.
Authors: Goldberg, Leo
Bibcode: 1962ApJ...136.1154G
Altcode:
  No abstract at ADS

Title: Stellar and Interstellar Observations
Authors: Goldberg, Leo
Bibcode: 1962saa..conf..203G
Altcode:
  No abstract at ADS

Title: Means of Observation
Authors: Goldberg, Leo
Bibcode: 1962sgba.book...19G
Altcode:
  No abstract at ADS

Title: Scientific discussion
Authors: Goldberg, L.
Bibcode: 1962IAUTB..11..194G
Altcode:
  No abstract at ADS

Title: Project West Ford-Properties and Analyses: Introduction
Authors: Goldberg, Leo
Bibcode: 1961AJ.....66..105G
Altcode:
  No abstract at ADS

Title: The Sun
Authors: Goldberg, Leo; Dyer, E. R., Jr.
Bibcode: 1961sis..book..307G
Altcode:
  No abstract at ADS

Title: Galactic and Extragalactic Astronomy
Authors: Goldberg, Leo; Dyer, E. R., Jr.
Bibcode: 1961sis..book..341G
Altcode:
  No abstract at ADS

Title: Solar Experiements - U. S. Plans. Report
Authors: Goldberg, Leo
Bibcode: 1961LIACo..10...30G
Altcode: 1961LIACo..10...26G; 1961MSRSL...4...26G
  No abstract at ADS

Title: The Abundances of the Elements in the Solar Atmosphere.
Authors: Goldberg, Leo; Muller, Edith A.; Aller, Lawrence H.
Bibcode: 1960ApJS....5....1G
Altcode:
  The method of weighting functions has been utilized to derive the
  abundances of forty-two elements from faint and medium-strong lines
  in the solar spectrum. The model atmosphere adopted is that of Aller
  and Pierce as extended by Elste to both higher and deeper layers. The
  chief sources of equivalent widths were the measurements by Allen and by
  the Utrecht astronomers, but a substantial number of new measurements
  were included from McMath-Hulbert Observatory data. TheJ-values were
  taken from many different sources, but, whenever possible, experimental
  measurements were employed. When laboratory data were not available,
  they were replaced by theoretical values based on the assumption of LS
  coupling and making use of the f-sum rule or of the Bates and Damgaard
  tables for the absolute scale factor. A detailed description is given
  of the derivation of the abundance of each element, including the major
  sources of uncertainty, such as the errors in the measurement of weak
  lines throughout the spectrum and of all lines in the ultraviolet
  region, uncertainties in the solar model for ultraviolet lines, and
  the unreliable character of many of the f-values employed.

Title: The Measutement of the Local Doppler Shift of Fraunhofer Lines.
Authors: Goldberg, Leo; Mohler, Orren C.; Unno, Wasaburo; Brown,
   Jacqueline
Bibcode: 1960ApJ...132..184G
Altcode:
  Well-defined spectra showing the Doppler shift arising from
  small-scale motions in the solar atmosphere were obtained with the
  vacuum spectrograph of the McMath-Hulbert Observatory during August
  and September, 1955. These spectra have been measured, and the local
  Doppler shifts of several solar absorption lines have been determined
  at various positions on the disk of the sun. The average value of the
  random turbulent velocity is found to be 0.33 km/sec for elements with
  an average diameter of 5.5 seconds of arc (4000 km). However, the values
  of the random turbulent velocity, as well as other characteristics,
  show systematic differences between weak and strong lines. Metallic
  lines formed at average effective optical depths, r(SO0O) larger than
  0.2, show smaller velocities than the average. Their r.m.s. velocities
  monotonically increase toward the limb of the sun (1.0&gt; &gt;
  0.6). Stronger lines (roooo &lt;0.2) show systematically larger
  values of the r.m.s. velocities with no appreciable center-to-limb
  variation. Near the limb of the sun ( = 0.35) all the measured lines
  show smaller r.m.s. velocities than at j# = 0.58. This may be caused
  by the lack of resolution of small elements in the neighborhood of the
  solar limb. These results suggest that the large-scale motion in the
  upper photosphere decreases as the limb of the sun is approached. They
  also suggest that a rising element of the atmosphere is statistically
  followed by a falling element in the same region.

Title: Solar experiments
Authors: Goldberg, Leo
Bibcode: 1960AJ.....65..274G
Altcode:
  Owing to the well-known negative temperature gradient in the It is also
  hoped that some type of x-ray imaging device will be solar atmosphere,
  the solar chromosphere and corona emit strongly flown in the first
  vehicle. in the far-ultraviolet and x-ray regions of the spectrum,
  as has Plans are also being developed for the installation of a small
  already been revealed by observations from rockets. The highly solar
  observatory with a variety of instruments totaling about energetic
  events connected with solar flares also result in strong 600 or 700
  lb, exclusive of stabilization gear, power supply and emissions at
  very short wavelengths. Hence, solar experiments storage, etc. The
  instruments would include a high-dispersion from satellites will have
  high priority in the astronomy space spectrometer operating in the
  region from 3000 to 75 A, one or program. more spectroheliometers to
  register images of the sun in Lyman-a Design work has been begun on
  the development of solar in- and other monochromatic radiations, an
  x-ray telescope and strumentation to be flown in a series of vehicles
  with progressively spectrometer, and equipment for the observation
  of low-frequency larger payloads. The first experiment is being
  designed for a ve- radio emission from the sun. hicle that can carry
  instruments up to a weight of about 100 lb Finally, it is pointed out
  that a number of important problems and that will be stabilized with a
  pointing accuracy of a few min- in solar physics can be solved better by
  observations from balloons utes of arc. Two scanning spectrometers will
  be employed, one rather than from satellites. These include studies
  of the hydro- covering the spectral region from 1600 to 500 A and
  the other dynamic and magnetic properties of the solar photosphere,
  and from 600 to 75 A. The resolving power would be about 1 A, and
  observation of the infrared solar spectrum. the spectrometers would
  have a combined weight of about 45 lb.

Title: Astronomy from Satellites and Space Vehicles
Authors: Goldberg, Leo
Bibcode: 1960exsp.conf..119G
Altcode:
  No abstract at ADS

Title: Astronomy from Satellites and Space Vehicles
Authors: Goldberg, Leo
Bibcode: 1959JGR....64.1765G
Altcode:
  Space experiments of interest to astronomy fall naturally into
  three groups. First, the elimination of the earth's atmosphere as
  a barrier to observation exposes to view the entire electromagnetic
  spectrum of radiation from extraterrestrial sources. It also permits
  the investigation both of the faint outer extensions of the solar
  atmosphere, which are now obliterated by the bright daylight sky,
  and of the weak radiations from faint stars and nebulas which are
  masked by radiation from atoms and molecules in the earth's upper
  atmosphere. Second, the advent of satellites and space vehicles
  makes possible a whole series of experiments and observations which
  are absolutely unique and which can test the foundations of physical
  theories.

Title: The Photosphere of the Sun.
Authors: Goldberg, Leo; Pierce, A. Keith
Bibcode: 1959HDP....52....1G
Altcode:
  The continuous spectrum Solar constant Observed limb darkening Observed
  solar energy distribution Observational models of the photosphere The
  Fraunhofer spectrum Observational data The formation of Fraunhofer
  lines The analysis of Fraunhofer lines General references

Title: The Double Reversal in the Cores of the Fraunhofer H and
    K Lines.
Authors: Goldberg, Leo; Mohler, O. C.; Müller, Edith A.
Bibcode: 1959ApJ...129..119G
Altcode:
  Observations are presented of the profiles of the central doubly
  reversed cores of the H and K lines of Ca ii in the Fraunhofer
  spectrum. The profiles were obtained photoelectrically with the
  vacuum spectograph of the McMath-Hulbert Observatory at five different
  points on the solar disk from M = 1.0 to = 0.2. At the center of the
  disk the central intensities of H and K are 2.95 and 2.36 per cent,
  respectively, in terms of the neighboring continuous spectrum near
  X 4000. At = 0.2 the central intensities are 2.41 and 2.01 per cent
  for H and K, respectively, also with reference to the continuum at
  X 4000 at the center of the disk. The relative intensity ratio H:
  K is found to be constant in the inner absorption core and nearly
  the same for all values of . This suggests that the logarithm of
  the source function varies linearly with the logarithm of Nh, the
  number of Ca ii atoms per square centimeter above height, h, in the
  chromosphere. The Doppler widths were derived by two methods, namely,
  (1) by an intercomparison method which is independent of the source
  functiop and (2) by using the depth-dependence of the source function
  and the shapes of the profiles. The Doppler widths thus found increase
  from 0.063 A at = 1.0 to 0.110 A at = 0.2. The derived Doppler widths
  and source function are employed to calculate the profiles of the
  inner cores of H and K. Extremely good agreement is found between the
  calculated and the observed central cores at all five values of . The
  variation in the Doppler widths from center to limb is discussed,
  and it is concluded that the widening of the profiles to the limb
  is caused by an increase in turbulence with height, combined with
  anisotropy. The comparison of the Doppler widths derived for Ca ii with
  results previously obtained for the X 10830 line of He I supports the
  hypothesis that the chromosphere is heterogeneous and is composed of
  regions of quite different physical properties.

Title: On the Empirical Determination of Line-Absorption Coefficints.
Authors: Goldberg, Leo
Bibcode: 1958ApJ...127..308G
Altcode:
  A method is described for extracting the wave4ength dependence of the
  line-absorption coefficient from observed line profiles, similar in
  principle to those employed by de Jager and by Athay and Thomas for
  the derivation of the Doppler widths of the Balmer lines. The method
  requires the accurate observation of the profiles of pairs of lines
  of known relative strengths in multiplets but necessitates no prior
  knowledge of the atmospheric model. The method is applied to the
  determination of the Doppler widths of the X 6238 and X 6248 solar
  lines of Fe+ from the recent observations of Suemoto.

Title: The Profile of Hα during the Limb Flare of February 10, 1956.
Authors: Goldberg, Leo; Mohler, Orren C.; Muller, Edith A.
Bibcode: 1958ApJ...127..302G
Altcode:
  Profiles of the Ha line in a very bright loop prominence associated
  with the great limb flare of February 10, 1956, show pronounced violet
  asymmetries. Despite the fact that the centers of different profiles,
  made at several points in the line on two different exposures, exhibit
  relative Doppler displacements as high as 0.8 A, the shapes of all
  the profiles can be accounted for by the superposition on the main Ha
  profile of an additional component centered between 1.5 and 2.0 A to
  the violet. The possibility is discussed that the asymmetry may have
  been caused by the presence of abnormal amounts of deuterium, presumably
  generated by nuclear reactions during the flare event. It is concluded
  that, although the evidence for deuterium is not conclusive, it would be
  extremely important to observe other similar flareassociated prominences
  in the future, with modern high-dispersion spectrographs. Observations
  should also be made simultaneously on at least one additional line of
  an element other than hydrogen, in order to eliminate velocity effects.

Title: The observatories of the University of Michigan.
Authors: Goldberg, L.
Bibcode: 1958AJ.....63..366G
Altcode:
  No abstract at ADS

Title: The Photosphere of the Sun
Authors: Pierce, A. K.; Goldberg, L.
Bibcode: 1958HDA....52....1P
Altcode:
  No abstract at ADS

Title: Turbulent Velocities Inferred from the H and K Emission Lines
    in Stellar Spectra.
Authors: Goldberg, Leo
Bibcode: 1957ApJ...126..318G
Altcode:
  IL is shown that the turbulent velocities inferred by Wilson and Bappu
  (1957) from the widths of the H and K emission lines in stellar spectra,
  on the assumption of origin in an optically thin layer, can probably
  be reduced by a factor of 3 or 4 on the not unreasonable hypothesis
  that the lines are broadened by the Doppler effect in an optically
  thick atmosphere

Title: A Connexion Between the Granulation and the Structure of the
    Low Chromosphere
Authors: Goldberg, Leo; Mohler, Orren C.; Brown, Jacqueline D.
Bibcode: 1957Natur.179..369G
Altcode:
  PHOTOGRAPHS of the solar spectrum made with the vacuum spectrograph
  of the McMath-Hulbert Observatory have revealed a variety of
  interesting and complex features in the structures of the Fraunhofer
  lines<SUP>1</SUP>. The appearance of the hydrogen line cores suggests
  an underlying, diffuse component that evidently originates in the
  photosphere, upon which are superposed a series of streaks that must
  be of chromospheric origin. The weaker metallic lines (of Rowland
  intensity less than about 10) also fluctuate in width and intensity
  and have a characteristic zig-zag appearance caused by the Doppler
  shifts of ascending and descending gas columns which are associated
  with the granulation in the photosphere.

Title: The chemical composition of the solar atmosphere.
Authors: Goldberg, Leo; Muller, Edith A.; Aller, Lawrence H.
Bibcode: 1957AJ.....62R..15G
Altcode:
  The abundances of some 40 elements relative to hydrogen have been
  redetermined in a new investigation of the chemical composition of
  the solar atmosphere from the Fraunhofer spectrum. The measi~irements
  of equivalent widths by the Utrecht group and by Allen's have been
  supplemented by infrared data and by measurements of selected lines on
  vacuum spectrograph plates from the McMath-Hulbert Observatory. The
  method of analysis is that of weighting functions, as developed by
  Minnaert and Claas for weak lines and by Pecker for lines of medium
  strength. In this method, the equivalent width of each line is related
  to the abundance by an integral over the model atmosphere, in which
  the integrand is the product of the number of absorbing atoms, the
  weighting function at each point in the atmosphere, and a so-called
  saturation function which reduces to unity for weak lines. Special
  numerical techniques for the evaluation of these integrals have been
  devised by Elste and adapted by him for computation with the Michigan
  high-speed computers, MIDAC and the IBM 650. An extensive set of these
  integrals has been tabulated by Elste for both weak lines and those of
  medium strength covering the wave-length region XX4ooo to 22,000 and
  a wide range of excitation potentials. This tabulation has provided
  the basis for the present investigation of solar abundances. The
  model atmosphere employed was derived by Waddell and Pierce from the
  latter's recent observations of solar-limb darkening and spectral-
  energy distribution, but with the pressure distribution modified
  by Elste in accordance with the work of Weidemann. The results are
  generally in good agreement with those of other workers, but there
  are notable exceptions, especially for those abundances that depend
  on the analysis of lines of medium strength. The reason appears to be
  that the shape of the curve of growth in the transition region differs
  markedly for lines originating at different depths in the atmosphere. It
  is anticipated that the results quoted here can be further improved
  when new photoelectric observations of weak lines are secured with
  the vacuum spectrograph of the McMath-Hulbert Observatory. However,
  for a large number of elements, uncertainties in the f-values present
  the major obstacle to definitive abundance determinations. University
  of Michigan, Ann Arbor, Mich.

Title: The origin of the double reversal in the Fraunhofer H and
    K lines.
Authors: Goldberg, Leo; Muller, Edith A.
Bibcode: 1957AJ.....62R..92G
Altcode:
  The discovery by 0. C. Wilson of a correlation between the absolute
  magnitudes of the G, K and M stars and the widths of the emission
  reversals in their K-line cores emphasizes the importance of
  establishing the mechanism both for widening the H and K emission-line
  cores in the sun and for producing the central self-reversal. Evidence
  is presented that favors Doppler broadening on the one hand and
  abundance broadening on the other. It is shown that the apparently
  conflicting arguments for the two kinds of broadening can be resolved
  if the cores of the H and K lines are formed in an optically-thick
  chromosphere in which the excitation temperature decreases with
  height. Methods are developed for the derivation of the excitation
  temperature and Ca+ density distributions from the observed profiles and
  it is shown that the resulting model accounts satisfactorily for the
  main features of the observed profiles both at the center of the disk
  and at the limb. University of Michigan Observatory, Ann Arbor, Mich.

Title: A connection between the granulation and the structure of
    the low chromosphere.
Authors: Goldberg, Leo; Mohler, Orren C.; Brown, Jacqueline D.
Bibcode: 1957AJ.....62Q..92G
Altcode:
  Isophotometer tracings of a plate of the Fraunhofer spectrum in the
  region of H~ show an interesting connection between the structures of
  the H~ line and of the Fei line N4859.747 (Rowland intensity 4). The
  Hfl line is resolved into structures as small as 3" or less, and the
  detail in the neighboring metallic lines is equally good. Over an
  interval of about 6' on the disc, 41 features in the H~ line were
  measured for radial velocity with respect to the underlying photo-
  spheric component of the line core. Similarly, velocity shifts
  were measured in the neighboring Fei line at points in the line
  corresponding to the positions of the 41 H~ structures. The results
  obtained are as follows: i) There is a remarkable association of the H~
  structures with violet shifts in the Fei line. Of the 41 measured H~
  structures, 30 are associated with violet shifts in the Fei line,
  7 with red shifts, and 4 with zero shifts; 2) The H~ structures are
  themselves predominantly shifted to the violet. The statistics show
  26 violet shifts, I I red shifts, and 4 zero shifts; 3) The velocity
  spread in the Hfl line is about three times as great as that in the
  Fei line, the rms values being 0.64 and 0.24 km/sec, respectively. It
  is tentatively suggested that the violet- shifted structures observed
  in the hydrogen lines represent extensions of the granular columns
  into the low chromosphere. The inequality between the negative and
  positive shifts in the H~ line may be attributed to the fact that on
  the average the ascending columns are at a somewhat higher temperature
  than the descending columns. Since a difference of only a few hundred
  degrees in temperature causes an enormous difference in the population
  of the two-quantum level of hydrogen, the relative absence of structures
  with descending velocities could be due to vanishingly small optical
  depth in the cooler columns. Further clarification may be expected
  from studies now being carried on with lines covering a large range
  of optical depth and excitation characteristics, including Ha, the K
  line of Ca+, the D lines of sodium, and the Mg b lines. University of
  Michigan Observatory, Ann Arbor, Mich.

Title: Reports of observatories
Authors: Goldberg, L.
Bibcode: 1956AJ.....61..330G
Altcode:
  No abstract at ADS

Title: Preliminary Results with a Vacuum Solar Spectrograph.
Authors: McMath, Robert R.; Mohler, Orren C.; Pierce, A. Keith;
   Goldberg, Leo
Bibcode: 1956ApJ...124....1M
Altcode:
  New observations of the solar spectrum with a high-resolution vacuum
  spectrograph reveal a wealth of detail in the cores of all Fraunhofer
  lines observed both in the normal disk and in areas exhibiting
  various kinds of solar activity. The lines show fluctuations in width,
  intensity, and position over intervals as small as 2 seconds of arc. A
  representative collection of photographs is presented, together
  with tentative conclusions derived from inspection and preliminary
  measurement. Measurements of Doppler shifts have been carried out in
  considerable detail for the two lines Cr X 4626 and Ba+ X 5853. The
  random turbulent velocity at the center of the disk is 0 70 km/sec
  for the chromium line and O. km/sec for the ionized barium line. For
  both lines the random turbulent velocity appears to increase toward
  the limb. The velocity shifts observed for the Ha and sodium D lines
  are of the same order of magnitude as those of the weaker metallic
  lines. The disk observations of the Fraunhofer lines of hydrogen and
  ionized calcium seem to he consistent with a qualitative model of the
  low chromosphere, consisting of relatively hot clouds of gas and with
  cooler regions both above and between the hot regions. Both the K2
  emission in ionized calcium and the wide absorption features in Ha
  seem to originate in the hot regions; from the appearance of these
  line features near the limb it seems that the hot regions contribute
  a substantial fraction of the hydrogen and ionized calcium emission
  in the very low chromosphere. The profiles of Ha at the extreme limb
  and of the K line and other strong metallic lines on the disk favor
  the conclusion of Adams and Burwell that central self-reversal is a
  general characteristic of most strong chromospheric profiles. The
  similarity between the intensity and velocity fluctuations in the
  core of the strong magnesium line X 5167 and in those of neighboring
  weaker lines implies either a chromospheric origin for the centers of
  these weaker lines or the extension of the photospheric granules into
  the low chromosphere. The preliminary nature of the foregoing results
  is emphasized.

Title: The Width of the Infrared Helium Line in the Solar Spectrum.
Authors: Mohler, Orren C.; Goldberg, Leo
Bibcode: 1956ApJ...124...13M
Altcode:
  Measurements of intensity and half-width are reported for the Fraunhofer
  line He I 10830 After correction for instrumental broadening and
  blending, the width at half4ntensity, averaged over the center of the
  disk and the four limbs, is 0.91 A. Within the error of measurement,
  the line widths show no center-to4imb variation The line appears
  to be broadened entirely by the Doppler effect, with AND = 0.55
  A, corresponding to an r.m.s. velocity of about 15 km/sec. If the
  broadening is entirely thermal, the kinetic temperature is about 50000
  K. Although the line is probably formed in localized hot regions of the
  chromosphere, it is not yet clear whether or not the derived velocity
  contains a turbulent, as well as a thermal, component.

Title: Solar Physics
Authors: Goldberg, Leo; Menzel, Donald H.
Bibcode: 1956SCoA....1..103G
Altcode:
  No abstract at ADS

Title: The abundance of atmospheric carbon dioxide and its isotopes
Authors: Goldberg, Leo
Bibcode: 1956VA......2..855G
Altcode:
  No abstract at ADS

Title: Infrared Solar Spectrum
Authors: Goldberg, Leo
Bibcode: 1955AmJPh..23..203G
Altcode:
  An account is given of recent results obtained from the study of
  the infrared solar spectrum with modern grating spectrometers and
  detectors. The discussion is divided into three parts, namely, the
  sun's continuous spectrum, the solar absorption-line spectrum, and
  the telluric- or terrestrial-line spectrum.

Title: The Abundances of the Elements in the Sun
Authors: Goldberg, Leo; Aller, Lawrence H.; Müller, Edith A.
Bibcode: 1955stat.conf..141G
Altcode: 1954stat.conf..141G
  No abstract at ADS

Title: The Temperature of the Low Chromosphere.
Authors: Goldberg, Leo
Bibcode: 1954ApJ...120..185G
Altcode:
  No abstract at ADS

Title: The Width of Hα in Solar Flares.
Authors: Goldberg, Leo; Dodson, Helen W.; Müller, Edith A.
Bibcode: 1954ApJ...120...83G
Altcode:
  It is shown that the observed large widening, at or near maximum,
  of the Ha emission line in certain solar flares can be explained as a
  consequence of radiation damping and the high abundance of two- quantum
  H atoms in the line of sight. When the effective width `of the Ha line
  is calculated according to the theory of self-absorption, the assumption
  of radiation damping leads to agreement with the observed lines widths
  when the number of two-quantum H atoms lies in the approximate range per
  cm2 in the line of sight. If it is assumed that the lateral extension
  of a flare is large compared with its thick- ness, the theory predicts
  that the effective width of Ha should be proportional to the square
  root of sec 0, where 0 is the angular distance from the center of the
  solar disk. Study of the Ha line widths of 610 flares reported in the
  Quarterly Bulletin of the I.A.U. for the period January, 1949, through
  June, 1952, reveals that the average line width increases steadily
  with increasing central meridian distance of the flares. Furthermore,
  flares with exceptionally wide lines ( 4.0 A) are observed most often
  in flares 45 or more from the central meridian. The relation between
  effective line width and central intensity found by Ellison is explained
  as primarily a consequence of self-absorption. Finally, the existing
  observational evidence in favor of the Stark effect as an important
  cause of the line broadening is examined and found unconvincing.

Title: The Absorption Spectrum of the Atmosphere
Authors: Goldberg, Leo
Bibcode: 1954eap..book..434G
Altcode:
  No abstract at ADS

Title: Discussion of a Possible Cooperative Telescope
Authors: Goldberg, L.; Linnell, A. F.
Bibcode: 1954asph.conf..107G
Altcode:
  No abstract at ADS

Title: Carbon Monoxide in the Sun.
Authors: Goldberg, Leo; Müller, Edith A.
Bibcode: 1953ApJ...118..397G
Altcode:
  Nearly 300 llnes of carbon monoxide have been identified in the spectrum
  of the solar limb between 2.29 and 2.50 . The lines belong to the
  overtone bands 24), 31, 42, 33, , and 7-5. Analysis of the solar wave
  lengths has led to a new determination of the vibrational and rotational
  constants of the CO molecule. The measured absorption coefficients
  of Penner and Weber and the theoretical values of Scholz have been
  applied to the measured equivalent widths at the center of the disk. The
  resulting equivalent abundance of CO is 1.45 X t0' molecules per square
  centimeter above the photosphere, and the excitation temperature is
  4300 K. It is shown from model-atmosphere calculations that solar Co is
  concentrated near the top of the photosphere and hence that the derived
  excitation temperature is consistent since it agrees with the boundary
  temperature. At present, it is not known whether the dissociation
  energy of CO is 9.6 or 11.1 e.v. If the lower value is correct, the
  solar-line intensities suggest that the boundary temperature is less
  than 4500 K. The exact value of the temperature depends on the choice of
  atomic abundances for 0 and C. The low intensities of the fundamental
  band lines of CO in the 4.6 region are explained as a consequence of
  (1) the high opacity of the solar atmosphere at long wave lengths,
  (2) the importance of stimulated emissions in the infrared, and (3)
  the small collisional line widths in the sun's outer layers.

Title: Table of Infrared Solar Lines, 1.4-2.5 μ.
Authors: Mohler, Orren C.; Pierce, A. Keith; McMath, Robert R.;
   Goldberg, Leo
Bibcode: 1953ApJ...117...41M
Altcode:
  Accurate wave lengths and measurements of equivalent width are given
  for 888 solar lines in the spectral region 1. 2.5 . The number of
  solar lines has been more than doubled, as compared with previous
  preliminary studies in this spectral region. The wave lengths of
  the solar lines are referred to those of the Fraunhofer lines in the
  visible and very near infrared spectrum by the method of overlapping
  orders. The root-mean-square errors of the infrared standard wave
  lengths, as derived from repeated measurements of individual lines,
  are +0.13 A for the l.6 region and +0.17 A for the 2.3 region. The
  equivalent widths are preliminary. The estimated errors are between
  10 and 100 per cent, depending upon the degree of blending. About 470
  infrared solar lines have been tentatively identified with atoms of H,
  K, C, At, Na, Si, Mg, Ca, Ni, and Fe and with first overtone lines
  of CO. Comparisons between solar wave lengths and those measured in
  the laboratory or predicted from term values reveal somewhat closer
  agreement, on the average, between the solar and the predicted values
  than between the solar and the laboratory values.

Title: Introduction
Authors: Goldberg, Leo
Bibcode: 1953sun..book....1G
Altcode:
  No abstract at ADS

Title: The Abundance of CO in the Sun and in the Earth's Atmosphere
Authors: Goldberg, Leo; McMath, Robert R.; Mohler, Orren C.; Pierce,
   A. Keith
Bibcode: 1952PhRv...85..481G
Altcode:
  No abstract at ADS

Title: Identification of CO in the Solar Atmosphere
Authors: Pierce, A. K.; Goldberg, L.; McMath, R. R.; Mohler, O. C.
Bibcode: 1952PhRv...85..140P
Altcode:
  No abstract at ADS

Title: The Abundance of CO in the Sun and in the Earth's Atmosphere
Authors: Pierce, A. K.; Goldberg, L.; McMath, R. R.; Mohler, O. C.
Bibcode: 1952PhRv...85..418P
Altcode:
  No abstract at ADS

Title: H-alpha survey.
Authors: Goldberg, L.
Bibcode: 1951AJ.....56..160G
Altcode:
  No abstract at ADS

Title: The Abundance and Vertical Distribution of Methane in the
    Earth's Atmosphere.
Authors: Goldberg, Leo
Bibcode: 1951ApJ...113..567G
Altcode:
  Theoretical expressions are derived for the equivalent widths of
  CY4 lines formed in the earth's atmosphere which take into account
  the variation of pressure and temperature with altitude in the
  atmosphere. When allowance is made for the curvature of the earth;
  information on the vertical distribution of CII 4 can be obtained from
  low-sun observations. The theoretical formulae have been employed for
  the analysis of observations of the t, 5 , and to-it lines in the 2 P3
  band of CH4 at 1.666 in the solar spectrum. From observations made at
  Lake Angelus, Michigan, and Mount Wilson, California, the total numbers
  of CH4 molecules per square centimeter through the zenith are found to
  be 3.2 X t0 and 2.6 X 1019, respectively. The ratio of abundances is
  very nearly that which would be expected if the distribution of CH4 is
  world-wide and falls off exponentially with height at the same rate as
  the main body of the atmosphere. The observations are well represented
  by theoretical curves of growth for pure damping, with /4ir = 1.2 X
  t0 for Lake Angelus and /4ir = 1.0 X t0 for Mount Wilson. Within the
  experimental error the ratio of damping constants is equal to the ratio
  of ground-level pressures at the two stations, in agreement with theory.

Title: Reports: Lamont-Hussey Observatory, Bloemfontein, South Africa
Authors: Goldberg, Leo
Bibcode: 1950AJ.....55..194G
Altcode:
  No abstract at ADS

Title: Stellar and nebular spectroscopy. Atmospheres of B-type
    stars. Studies of A-type stars.
Authors: Goldberg, L.
Bibcode: 1950AJ.....55..192G
Altcode:
  No abstract at ADS

Title: Observations of Solar Limb Darkening Between 0.5 and
    10.2&amp;mu
Authors: Pierce, A. K.; McMath, R. R.; Goldberg, Leo; Mohler, O. C.
Bibcode: 1950ApJ...112..289P
Altcode:
  Measurements of solar limb darkening are tabulated for thirteen
  wave lengths between 0.5 and 10.2 . Observations in the wave-length
  region 0.5-2.2 were carried out with the McGregor Tower telescope and
  spectrometer for the interval cos 0 = 1.0 to cos 0 = 0.16. Measurements
  at three longer wave lengths were made with a Perkin-Elmer spectrometer
  attached to the 24inch reflector and covered the interval cos 0 = 1.0
  to cos 0 = 0.2. At certain wave lengths the near infrared measurements
  agree with those of Abbot's to within 0.1 per cent; at other wave
  lengths the systematic differences are as large as 1 per cent. It is
  found that the degree of limb darkening decreases in the infrared
  from 3.5 to 10.2 . This result is qualitatively consistent with a
  systematic increase of the solar continuous opacity toward longer wave
  lengths in the infrared, as predicted by theoretical calculations of
  the absorption coefficient of the negative hydrogen ion.

Title: Position of the Portage Lake Observatory
Authors: Goldberg, Leo
Bibcode: 1950AJ.....55..160G
Altcode:
  No abstract at ADS

Title: New Solar Lines in the Spectral Region 1.97-2.49 μ.
Authors: Goldberg, Leo; Mohler, Orren C.; Pierce, A. Keith; McMath,
   Robert R.
Bibcode: 1950ApJ...111..565G
Altcode:
  Measurements of wave length and of percentage central absorption are
  given for 109 solar lines in the region 1.97-2.49 of the infrared
  solar spectrum. The lines were found on tracings obtained with
  the high-dispersion spectrometers and Cashman PbS cells of the
  McMath-Hulbert Observatory at Lake Angelus and at the Mount Wilson
  Observatory. Forty-seven lines have been identified as arising from
  neutral atoms of H, Na, Si, Mg, Al, Ca, and Fe. The relative scarcity
  of solar lines in the 2.2 IL region is discussed, and a qualitative
  explanation is given in terms of the variation with wave length of
  the continuous absorption coefficient of H- combined with the solar
  temperature gradient.

Title: Recent advances in infra-red solar spectroscopy
Authors: Goldberg, L.
Bibcode: 1950RPPh...13...24G
Altcode:
  No abstract at ADS

Title: The 3n3 Band of Telluric CO<SUB>2</SUB> in the Solar Spectrum
Authors: Pierce, A. K.; Goldberg, L.; Mohler, O. C.; McMath, R. R.
Bibcode: 1950PhRv...78...74P
Altcode:
  No abstract at ADS

Title: N<SUB>2</SUB>O Bands in the Solar Spectrum
Authors: Pierce, A. K.; McMath, R. R.; Mohler, O. C.; Goldberg, L.;
   Donovan, R. A.
Bibcode: 1950PhRv...78...65P
Altcode:
  No abstract at ADS

Title: Telluric Bands of CH_{4} in the Solar Spectrum.
Authors: McMath, Robert R.; Mohler, Orren C.; Goldberg, Leo
Bibcode: 1949ApJ...109...17M
Altcode:
  An all-reflecting telescope and spectrometer have been employed in
  conjunction with a Cashman PbS cell to secure a direct-intensity map
  of the solar spectrum in the region of 0.8-2.5 ~i with a resolution
  of about 50,000. Four molecular-band systems at 1.66, 2.20, 2.32,
  and 2.37 ~ have been identified as the P1 + V4~ V3 + P4 and ~2 + P3
  transitions of CH4 in the earth's atmosphere. A preliminary analysis
  of the wave numbers of the 2P3 rotational components indicates
  second-order deviations from theory. The average half-spacing B0 is
  found to be 5.163, as compared with the value B0 = 5.252 obtained by
  Childs. A comparison of the 2P3 telluric line intensities with those
  produced by a measured quantity of methane at room temperature leads
  to a calculated methane abundance in the earth's atmosphere of 1.2
  parts in a million by mass, and a temperature of -37° C

Title: New Solar Lines in the Spectral Region 1.52-1.75 μ.
Authors: Goldberg, Leo; Mohler, Orren C.; McMath, Robert R.
Bibcode: 1949ApJ...109...28G
Altcode:
  Accurate wave lengths and measurements of percentage central absorption
  are given for nearly three hundred new solar lines discovered in the
  region 1.52-1.75 ~ of the infrared solar spectrum. The lines were found
  on high-resolution, direct-intensity tracings of the spectrum obtained
  at the McMath- Hulbert Observatory with the McGregor spectrometer
  and a Cashman cell. Ninety-three of the lines have been identified as
  belonging to neutral atoms of C, Mg, Al, Si, Fe, Mn, and Ni, mainly
  on the basis of wave lengths computed from term values. In addition,
  the third, seventh, and eighth members of the Brackett series of
  hydrogen have been identified, together with the Na I 4s-4p doublet
  at XX 22,054 and 22,081. INTRODUCTIO

Title: Note on Methane in the Infra-Red Solar Spectrum
Authors: Pierce, A. K.; McMath, R. R.; Mohler, O. C.; Goldberg, L.
Bibcode: 1949PhRv...76.1533P
Altcode:
  No abstract at ADS

Title: Carbon Dioxide in the Infra-Red Solar Spectrum
Authors: Pierce, A. K.; Goldberg, L.; Mohler, O. C.; McMath, R. R.
Bibcode: 1949PhRv...76.1848P
Altcode:
  No abstract at ADS

Title: The solar curve of growth and the kinetic temperature of the
    solar reversing layer.
Authors: Pierce, A. Keith; Goldberg, Leo
Bibcode: 1948AJ.....53..202P
Altcode:
  An observational solar curve of growth for iron, titanium, and
  vanadium was constructed from the gf values of the Kings and the
  equivalent widths of Allen. Corrections for the variable continuous
  opacity and limb darkening coefficient were applied to each line
  before grouping according to excitation potential. For iron and
  titanium the displacement of the groups gave a temperature of 46800
  K, while for vanadium no proper temperature could be found because
  of the non-linear relation between excitation potential and the
  displacements. The observed curve of growth was fitted to a theoretical
  curve based on the Milne-Eddington model. The "best" fit corresponds to
  a most probable Doppler velocity of 2.5 km/sec and values AND/AXN = a
  (as defined by Mitchell and Zemansky, Resonance Radiation and Excited
  Atoms, Cambridge, 1934) equalling 0.01 for the weaker iron lines
  and 0.05 for the stronger. The velocity parameter may be interpreted
  in terms of either a kinetic temperature of 57000 plus a turbulent
  velocity of 2.0 km/sec or a straight kinetic temperature of 19,5000
  K. In an attempt to distinguish between the alternatives of thermal
  or turbulent broadening, the half-widths of faint lines of several
  elements of different atomic weight, ranging from carbon to nickel,
  were determined from the Utrecht Atlas. The widths of these lines,
  after correction for instrumental broadening, show a dependence on
  atomic weight that accords well with the assumption of thermal widening
  at a temperature of 16,0000 K. Observatory, University of Michigan,
  Ann Arbor, Mich.

Title: Recent developments in infra-red solar spectroscopy.
Authors: McMath, R. R.; Mohler, O. C.; Goldberg, L.
Bibcode: 1948AJ.....54Q..44M
Altcode:
  Since the late fall of 1947, the ~cGregor tower of the McMath-Hulbert
  Observatory has been used for study of the infra-red solar spectrum
  beyond the photographic limit. A specially designed, all-mirror optical
  system and Pfund-type grating spectrometer, with monochromator,
  have been used in conjunction with a Cashman leadsulphide cell to
  obtain direct-intensity tracings of the solar spectrum over the
  entire region between 8ooo and 25000 A. The spectrum is re corded on
  a scale of about five millimeters per angstrom. In the 15000 X region,
  lines with separation of 0.3 angstroms are just resolved. Water vapor
  absorption almost completely obliterates the spectrum in the regions I
  .3-1.5 microns and 1.75-1.95 microns. The intervening portions of the
  spectrum, however, are relatively clear and contain a wealth of solar
  atomic lines, as well as telluric molecular lines and bands. Progress in
  identification has been slow, largely because of the complete absence
  of high-resolution laboratory studies in this region of the infra-red
  spectrum. Approximately 200 solar atomic lines have been identified
  in the infra-red spectrum on the basis of wave lengths computed from
  known atomic energy levels. The elements for which lines have been
  found include Fe, Si, Na, AIg, Al, C, Ca, as well as the third and
  seventh members of the Brackett series of hydrogen. The vast majority
  of these lines have excitation potentials higher than five volts. Band
  systems of molecules originating in the earth's atmosphere constitute
  some of the most interesting features of the infra-red spectrum. Among
  these are four CO1 bands in the 1.6 micron region, which have been
  resolved for the first time, and three strong bands of CO1 at 2.1
  microns. Among the identified molecular bands, those of ammonia and
  methane are particularly noteworthy. The evidence for ammonia as
  a constituent of the earth's atmosphere is very strong, while the
  evidence for methane is conclusive. Mc Math- Hulbert Observatory,
  Pontiac, Mich. and University of Michigan Observatory, Ann Arbor, Mich.

Title: The Solar Corona and Ultraviolet Radiation
Authors: Goldberg, Leo; Menzel, Donald H.
Bibcode: 1948HarMo...7..279G
Altcode: 1948cent.symp..279G
  No abstract at ADS

Title: Evidence for coronal absorption on the solar disk.
Authors: McMath, Robert R.; Goldberg, Leo; Mohler, Orren C.
Bibcode: 1947AJ.....52R.156M
Altcode:
  A broad, diffuse absorption line at 637A.45 I.A. + 0.01 has been found
  in the spectrum of the solar disk on plates obtained with the McGregor
  sbectrograph and the 70-ft. tower telescope of the McMath-Hulbert
  Observatory. Its width has been estimated at 0.3 to 0.4 A. The line
  is seen very faintly at the center of the disk, becoming strongly
  accentuated at the limb. It appears equally intense all around the
  limb and no significant variations in intensity or in wave length
  have been found. The appearance of the line and the closeness of its
  position to that of the red coronal line (given by Lyot as X6374.5I +
  0.03) suggest the possibility that the absorption line arises from
  atoms of Fe x. The evidence for or against the identification as Fe
  x is discussed, the results at present being inconclusive. If the
  line is due to Fe x, its intensity and distribution around the limb
  are such that a considerable abundance of Fe x must be present in the
  chromosphere. In this connection attention is called to the observation
  by H. D. and H. W. Babcock' of a similar diffuse absorption line
  at X6374.40 in the flash spectrum outside of eclipse. The Babcocks
  reported that the line was flanked by emission components on either
  side. A predicted line of Fe I (ziC2o - e702) occurs at X6374.43. No
  other members of this multiplet have been observed with certainty in
  the solar spectrum, however, and the width of the observed absorption
  line makes its identification as predicted Fe I unlikely, unless it
  is closely blended with another faint line. A search has been made
  for a similar absorption line at the position of the green coronal
  line 5302.86, identified by Edlen as arising from Fe xiv. No such
  absorption line has been found. It is pointed out that excitation
  conditions in the chromosphere favorable for the presence of Fe
  x would not necessarily produce Fe xiv. I.Pub. A. S. P. 46, 132,
  1934. McMath-Hulbert Observatory, Lake Angelus, Pontiac, Mich.

Title: Statistical equilibrium of helium atoms in gaseous nebulae
Authors: Goldberg, Leo
Bibcode: 1946PAAS...10R..13G
Altcode:
  No abstract at ADS

Title: Continuous absorption coefficients for complex atoms
Authors: Goldberg, Leo; Aller, L. H.
Bibcode: 1946PAAS...10R.162G
Altcode:
  No abstract at ADS

Title: Atomos, estrellas Y nebulosas
Authors: Goldberg, Leo; Aller, Lawrence Hugh
Bibcode: 1944aeyn.book.....G
Altcode: 1944QB461.G617.....
  No abstract at ADS

Title: Book reviews: Atoms, Stars, and Nebulae
Authors: Goldberg, Leo; Aller, Lawrence H.
Bibcode: 1943PA.....51..289G
Altcode:
  No abstract at ADS

Title: Atoms, stars and nebulae
Authors: Goldberg, Leo; Aller, Lawrence Hugh
Bibcode: 1943asn..book.....G
Altcode: 1943QB461.G6.......
  No abstract at ADS

Title: Physical Processes in Gaseous Nebulae. XV.
Authors: Goldberg, Leo
Bibcode: 1941ApJ....93..244G
Altcode:
  The statistical equilibrium of an assembly of neutral helium atoms
  has been investigated with refer- ence to the problem of gaseous
  nebulae. The helium atom was assumed to contain an infinite number of
  energy levels, but a single equation of equilibrium was written down
  for all triplet levels above 2 3po and, similarly, for all singlets
  above 2 ipo Mean values are thus obtained for the popiilations of the
  high singlets and the high triplets. The population is given in terms
  of a quantity b~, the ratio between the true population and the value
  for thermodynamic equilibrium at a temperature T~. The temperature T~
  refers to an assumed Maxweffian distribution of the free electrons. The
  nebular atoms are assumed to be opaque to the stellar radiation field
  oniy in the frequencies cor- responding to absorptions from levels i
  IS, 2 Is, and 2 ~S. Numerical solutions of the equations are tabu-
  lated for stellar temperatures, T1, of 50,000° and 100,000° and
  electron temperatures of 5000° 10,000°, 20,0000, 40,000°, and
  80,0000, and also for the special case T1 = T6 = 20,0000

Title: An Investigation of the Rowland Intensity Scale.
Authors: Menzel, Donald H.; Goldberg, Leo; Cook, Edward M.
Bibcode: 1940ApJ....91..320M
Altcode: 1940HarRe.195....1M
  A new calibration of Rowland's scale of solar intensities has been
  derived with the aid of the theoretical strengths of multiplets in
  transition arrays. The calibration takes the form of a double-entry
  table giving average values of log X0, where X0 is the optical depth at
  the center of an absorption line, for each Rowland intensity from -3 to
  +8 at intervals of 400 A from X 2800 to X 68oo. A total of 37 transition
  arrays, representing 13 metaffic elements and 1119 lines in all, was
  employed in the analysis. The present calibration is considerably less
  steep than the earlier one of Russell, Adams, and Moore

Title: Transition Probabilities for he I.
Authors: Goldberg, Leo
Bibcode: 1939ApJ....90..414G
Altcode: 1939HarRe.182....1G
  Simple, screening-type wave functions have been utilized to derive
  general expres- sions for the line strengths in the 2s-np and
  2p-nd series of He i. The resulting strengths calculated for these
  series compare favorably with those computed by 11yi- leraas for the
  transitions up to n = 6. A computation of the radiational damping con-
  stants shows that the He I triplet damping factors are of the order
  of one hundred times smaller than the singlet values, a result that
  arises from the metastability of the lowest triplet level and from
  the short wave length of the fundamental singlet line. The expressions
  for the discrete f-values have been extended to the continuum by the
  device of letting n -~ ~K, where K is a continuous quantum number,
  according to the method outlined by Menzel and Pekeris. The resulting
  expressions provide for the determination of the absorption coefficients
  for bound-free transitions from the 2S and 2~ levels. Thef-sum rule
  of Kuhn and Thomas-Reiche predicts that the sum of thef-values of all
  transitions from a singly excited level of He I should equal unity. The
  rule appears to be satisfactorily obeyed for all but the 2 ~S level,
  for which the sum is 0.849

Title: Scientific Books: The Distribution of the Stars in Space
Authors: Goldberg, Leo
Bibcode: 1939Sci....90..110G
Altcode: 1939Sci....90..110B
  No abstract at ADS

Title: A Study of the Equivalent Width of Helium Lines in Early-Type
    Stars.
Authors: Goldberg, Leo
Bibcode: 1939ApJ....89..623G
Altcode: 1939HarRe.167....1G
  The theoretical strengths of the He i lines in the diffuse 2p-nd
  series have been employed, together with E. G. Wiffiams' measures of
  equivalent widths, to construct curves of growth for the helium lines
  in fifty-seven 0- and B-type stars. Comparisons of these curves with a
  theoretical curve for helium atoms at a temperature of 20,0000 per- mits
  a determination of the quantifies V and ~. V is defined by the relatio

Title: The Temperature of the Solar Chromosphere.
Authors: Goldberg, Leo
Bibcode: 1939ApJ....89..673G
Altcode:
  The theoretical strengths of the diffuse triplet lines of He r have
  been employed in connection with Menzel and Cillié's measures of
  1932 chromospheric lines in an attempt to determine the excitation
  temperature of the solar chromosphere. The temperature appears to
  increase with the height, ranging from 4300° for the chromospheric
  slab 670 km above the solar limb to 6700° for a height of 2330 km. The
  diffuse singlet lines of He i appear to be anomalously faint relative
  to the dif- fuse triplets. The suggestion is made that, in a rarefied
  chromosphere, the combination of the metastabffity of the 2~S level
  and a possible excess of ultraviolet radiation in the region at 500
  A may account for the relative faintness of the singlets

Title: Equivalent widths and the reversing-layer temperature
Authors: Menzel, Donald H.; Goldberg, Leo; Baker, James G.
Bibcode: 1939PAAS....9R..51M
Altcode:
  No abstract at ADS

Title: A study of the equivalent widths of helium lines in early-type
    stars
Authors: Goldberg, Leo
Bibcode: 1939PAAS....9S.220G
Altcode:
  No abstract at ADS

Title: Temperature of the solar chromosphere
Authors: Goldberg, Leo
Bibcode: 1939PAAS....9R.220G
Altcode:
  No abstract at ADS

Title: Equivalent Widths and the Temperature of the Solar Reversing
    Layer
Authors: Menzel, Donald H.; Baker, James G.; Goldberg, Leo
Bibcode: 1938ApJ....87...81M
Altcode: 1938HarRe.145....1M
  Allen's extensive determinations of equivalent widths of Fraunhofer
  lines provide important observational material for an analysis of the
  physical state of the solar atmos- phere. A comparison of the observed
  intensities of absorption lines, as read from an em- pirical curve of
  growth, with the theoretical strengths of lines in a transition array
  makes it possible to calculate the effective excitation temperature of
  the reversing layer. Tem- peratures of 4350° ± 200° and 41500 ±
  50° are computed from the lines of Ti i and Fe I, respectively. A
  qualitative discussion of the errors inherent in the theoretical
  calculation of mul- tiplet strengths is given, and a method for
  calculating the reversing-layer temperature by means of the f-file sum
  rule is described. The application of this method to the lines of Ti i
  yields a temperature of 4400° ± ba0. Since the sum rule is independent
  of the coupling in an atom, and is therefore free of the assumptions
  involved in the calculation of multiplet strengths, the value 4400° is
  adopted, for purposes of discussion, as the mean excitation temperature
  of the solar reversing layer. If the opacity of the solar atmosphere
  varies with wave length, we should expect to find the numbers of atoms,
  as derived from equivalent widths, depending upon wave length as well
  as upon the temperature and excitation potential. The data for Fe in-
  dicate an opacity law almost independent of wave length. These results,
  however, are not definitive. Since the mean lower excitation potentials
  increase systematically with wave length, opacity and temperature
  effects are correlated. The data for Ti, where no systematic correlation
  exists, are not inconsistent with an opacity varying as X~, whereas
  theory predicts a law varying approximately as X3e-hc/XkT. An attempt
  is made to rec- oncile the observations and the theoretical values

Title: The Intensities of Helium Lines.
Authors: Goldberg, Leo
Bibcode: 1938PhDT.........1G
Altcode:
  No abstract at ADS

Title: Note on Relative ƒ-VALUES for Lines of fe I
Authors: Menzel, Donald H.; Goldberg, Leo
Bibcode: 1937ApJ....85...40M
Altcode: 1937HarRe.131....1M
  In connection with R. B. and A. S. King's recent intensity measurements
  of Fe i absorption lines in furnace spectra, the omission of a weight
  factor in reducing equiva- lent widths to relative f-values is noted. In
  order to yield true f-values, the values as published must be divided
  by the statistical weight of the lower level

Title: Multiplet Strengths for Transitions Involving Equivalent
    Electrons
Authors: Menzel, Donald H.; Goldberg, Leo
Bibcode: 1936ApJ....84....1M
Altcode: 1936HarRe.126....1M
  Bacher and Goudsmit have shown that the parentage of a term arising from
  a shell of equivalent electrons is expressible as a linear combination
  of all the terms of the ion. When two or more terms of a kind occur in
  the same configuration, however, the method gives only the sum of the
  parentages of the terms involved. The resulting parentages may be used
  with the well-known Kronig formulae to calculate multiplet strengths
  in transition arrays where the jumping electron is equivalent to others
  in oniy one of the two configurations. At the present time, the method
  is applicable to all arrays involving equivalent s- and p-electrons,
  and to arrays involving not more than three equivalent d-electrons. For
  convenience of calculation a table containing the parentages of terms
  arising from equivalent electron shells is given. The table also
  lists the configurations of astro- physical interest to which these
  parentages may be applied in the calculation of multi- plet strengths

Title: Note on Absolute Multiplet Strengths
Authors: Goldberg, Leo
Bibcode: 1936ApJ....84...11G
Altcode:
  A table of factors is given by means of which the relative multiplet
  strengths tabu- lated by the writer in an earlier paper may be converted
  to absolute strengths in terms of c2, the square of the one-electron
  matrix component. ~ is a constant for any given tran- sition array

Title: Relative Multiplet Strengths in LS Coupling
Authors: Goldberg, Leo
Bibcode: 1935ApJ....82....1G
Altcode: 1935HarRe.112....1G
  The relative strengths of different multiplets in LS coupling have
  been calculated and tabulated for sixty-five transition arrays of
  astrophysical interest. In arrays where the jumping electron belongs to
  a shell of three or more equivalent electrons, the method of Condon and
  IJiford was employed; all other cases were dealt with by the extension
  of Kronig's formulae to relative multiplet strengths, according to
  the methods outlined by Shortley. A description of the Condon-TJfford
  method is given, together with an illus- tration of its application
  to the transition array p3 -p2s. It is shown, also, that in apply-
  ing this method, it is necessary to write down the zero-order states
  of only one configura- tion, that involving the smallest number of terms

