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Author name code: sauval
ADS astronomy entries on 2022-09-14
author:"Sauval, A. Jacques" 

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Title: The elemental composition of the Sun. III. The heavy elements
    Cu to Th
Authors: Grevesse, Nicolas; Scott, Pat; Asplund, Martin; Sauval,
   A. Jacques
2015A&A...573A..27G    Altcode: 2014arXiv1405.0288G
  We re-evaluate the abundances of the elements in the Sun from copper
  (Z = 29) to thorium (Z = 90). Our results are mostly based on
  neutral and singly-ionised lines in the solar spectrum. We use the
  latest 3D hydrodynamic solar model atmosphere, and in a few cases
  also correct for departures from local thermodynamic equilibrium
  (LTE) using non-LTE (NLTE) calculations performed in 1D. In order
  to minimise statistical and systematic uncertainties, we make
  stringent line selections, employ the highest-quality observational
  data and carefully assess oscillator strengths, hyperfine constants
  and isotopic separations available in the literature, for every line
  included in our analysis. Our results are typically in good agreement
  with the abundances in the most pristine meteorites, but there are
  some interesting exceptions. This analysis constitutes both a full
  exposition and a slight update of the relevant parts of the preliminary
  results we presented in Asplund et al. (2009, ARA&A, 47, 481),
  including full line lists and details of all input data that we have
  employed. <P />Tables 1-3 are available in electronic form at <A
  href="http://www.aanda.org/10.1051/0004-6361/201424111/olm">http://www.aanda.org</A>

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Title: The elemental composition of the Sun. II. The iron group
    elements Sc to Ni
Authors: Scott, Pat; Asplund, Martin; Grevesse, Nicolas; Bergemann,
   Maria; Sauval, A. Jacques
2015A&A...573A..26S    Altcode: 2014arXiv1405.0287S
  We redetermine the abundances of all iron group nuclei in the Sun,
  based on neutral and singly-ionised lines of Sc, Ti, V, Mn, Fe, Co and
  Ni in the solar spectrum. We employ a realistic 3D hydrodynamic model
  solar atmosphere, corrections for departures from local thermodynamic
  equilibrium (NLTE), stringent line selection procedures and high
  quality observational data. We have scoured the literature for
  the best quality oscillator strengths, hyperfine constants and
  isotopic separations available for our chosen lines. We find log
  ɛ<SUB>Sc</SUB> = 3.16 ± 0.04, log ɛ<SUB>Ti</SUB> = 4.93 ± 0.04,
  log ɛ<SUB>V</SUB> = 3.89 ± 0.08, log ɛ<SUB>Cr</SUB> = 5.62 ± 0.04,
  log ɛ<SUB>Mn</SUB> = 5.42 ± 0.04, log ɛ<SUB>Fe</SUB> = 7.47 ± 0.04,
  log ɛ<SUB>Co</SUB> = 4.93 ± 0.05 and log ɛ<SUB>Ni</SUB> = 6.20 ±
  0.04. Our uncertainties factor in both statistical and systematic errors
  (the latter estimated for possible errors in the model atmospheres and
  NLTE line formation). The new abundances are generally in good agreement
  with the CI meteoritic abundances but with some notable exceptions. This
  analysis constitutes both a full exposition and a slight update of the
  preliminary results we presented in Asplund et al. (2009, ARA&amp;A,
  47, 481), including full line lists and details of all input data
  we employed. <P />Tables 1-3 are available in electronic form at <A
  href="http://www.aanda.org/10.1051/0004-6361/201424110/olm">http://www.aanda.org</A>

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Title: The elemental composition of the Sun. I. The intermediate
    mass elements Na to Ca
Authors: Scott, Pat; Grevesse, Nicolas; Asplund, Martin; Sauval,
   A. Jacques; Lind, Karin; Takeda, Yoichi; Collet, Remo; Trampedach,
   Regner; Hayek, Wolfgang
2015A&A...573A..25S    Altcode: 2014arXiv1405.0279S
  The chemical composition of the Sun is an essential piece of reference
  data for astronomy, cosmology, astroparticle, space and geo-physics:
  elemental abundances of essentially all astronomical objects are
  referenced to the solar composition, and basically every process
  involving the Sun depends on its composition. This article, dealing
  with the intermediate-mass elements Na to Ca, is the first in a
  series describing the comprehensive re-determination of the solar
  composition. In this series we severely scrutinise all ingredients
  of the analysis across all elements, to obtain the most accurate,
  homogeneous and reliable results possible. We employ a highly
  realistic 3D hydrodynamic model of the solar photosphere, which has
  successfully passed an arsenal of observational diagnostics. For
  comparison, and to quantify remaining systematic errors, we repeat
  the analysis using three different 1D hydrostatic model atmospheres
  (marcs, miss and Holweger &amp; Müller 1974, Sol. Phys., 39, 19) and
  a horizontally and temporally-averaged version of the 3D model (⟨ 3D
  ⟩). We account for departures from local thermodynamic equilibrium
  (LTE) wherever possible. We have scoured the literature for the best
  possible input data, carefully assessing transition probabilities,
  hyperfine splitting, partition functions and other data for inclusion
  in the analysis. We have put the lines we use through a very stringent
  quality check in terms of their observed profiles and atomic data, and
  discarded all that we suspect to be blended. Our final recommended
  3D+NLTE abundances are: log ɛ<SUB>Na</SUB> = 6.21 ± 0.04, log
  ɛ<SUB>Mg</SUB> = 7.59 ± 0.04, log ɛ<SUB>Al</SUB> = 6.43 ± 0.04,
  log ɛ<SUB>Si</SUB> = 7.51 ± 0.03, log ɛ<SUB>P</SUB> = 5.41 ± 0.03,
  log ɛ<SUB>S</SUB> = 7.13 ± 0.03, log ɛ<SUB>K</SUB> = 5.04 ± 0.05
  and log ɛ<SUB>Ca</SUB> = 6.32 ± 0.03. The uncertainties include both
  statistical and systematic errors. Our results are systematically
  smaller than most previous ones with the 1D semi-empirical
  Holweger &amp; Müller model, whereas the ⟨ 3D ⟩ model returns
  abundances very similar to the full 3D calculations. This analysis
  provides a complete description and a slight update of the results
  presented in Asplund et al. (2009, ARA&amp;A, 47, 481) for Na to
  Ca, and includes full details of all lines and input data used. <P
  />Tables 1-4 and Appendix A are available in electronic form at <A
  href="http://www.aanda.org/10.1051/0004-6361/201424109/olm">http://www.aanda.org</A>

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Title: “Old” versus “New” Solar Chemical Composition
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P.
2013ASPC..479..481G    Altcode:
  We follow the evolution since 1989 of element abundance determinations
  in the solar photosphere. We describe how the largely used high
  metallicity mixtures (Z = 0.02 to 0.017) of Anders &amp; Grevesse
  (1989), Grevesse &amp; Noels (1993) and Grevesse &amp; Sauval (1998)
  have been obtained and explain why these mixtures should not be used
  anymore. They are to be replaced by the more recent mixture of Asplund
  et al. (2009) which results from the first comprehensive and homogeneous
  analysis for many decades. We describe the main characteristics of this
  work and discuss some impacts of this low Z (Z = 0.0134) mixture. We
  also comment on another recent analysis by Caffau et al. (2011) that
  leads to somewhat larger metal abundances.

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Title: The New Solar Chemical Composition — from Z = 0.02 to Z
    = 0.013
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P.
2012ASPC..462...41G    Altcode:
  We review the current status of our knowledge of the chemical
  composition of the sun and present a redetermination of the solar
  abundances of all available elements. These new results have recently
  been published by Asplund et al. (2009). The basic ingredients of
  this work, the main results and their implications are discussed. We
  show why the abundances of the main contributors to the metallicity
  have decreased and why the old high solar metallicity, Z ∼ 0.02,
  is definitely obsolete and should not be used anymore. We also show
  why other recent analyzes of the solar composition report solar
  metallicities somewhat larger than the one we recommend.

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Title: The chemical composition of the sun
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P.
2011CaJPh..89..327G    Altcode:
  No abstract at ADS

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Title: The New Solar Composition and the Solar Metallicity
Authors: Grevesse, Nicolas; Asplund, Martin; Sauval, A. Jacques;
   Scott, Pat
2011sswh.book...51G    Altcode:
  No abstract at ADS

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Title: The chemical composition of the Sun
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P.
2010Ap&SS.328..179G    Altcode: 2010Ap&SS.tmp...48G
  We present a redetermination of the solar abundances of all available
  elements. The new results have very recently been published by
  Asplund et al. (Annu. Rev. Astron. Astrophys. 47:481, 2009). The
  basic ingredients of this work, the main results and some of their
  implications are summarized hereafter.

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Title: The Chemical Composition of the Sun
Authors: Asplund, Martin; Grevesse, Nicolas; Sauval, A. Jacques;
   Scott, Pat
2009ARA&A..47..481A    Altcode: 2009arXiv0909.0948A
  The solar chemical composition is an important ingredient in our
  understanding of the formation, structure, and evolution of both the
  Sun and our Solar System. Furthermore, it is an essential reference
  standard against which the elemental contents of other astronomical
  objects are compared. In this review, we evaluate the current
  understanding of the solar photospheric composition. In particular,
  we present a redetermination of the abundances of nearly all available
  elements, using a realistic new three-dimensional (3D), time-dependent
  hydrodynamical model of the solar atmosphere. We have carefully
  considered the atomic input data and selection of spectral lines, and
  accounted for departures from local thermodynamic equilibrium (LTE)
  whenever possible. The end result is a comprehensive and homogeneous
  compilation of the solar elemental abundances. Particularly noteworthy
  findings are significantly lower abundances of C, N, O, and Ne compared
  to the widely used values of a decade ago. The new solar chemical
  composition is supported by a high degree of internal consistency
  between available abundance indicators, and by agreement with
  values obtained in the Solar Neighborhood and from the most pristine
  meteorites. There is, however, a stark conflict with standard models
  of the solar interior according to helioseismology, a discrepancy that
  has yet to find a satisfactory resolution.

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Title: Experimental and theoretical radiative decay rates for highly
    excited ruthenium atomic levels and the solar abundance of ruthenium
Authors: Fivet, V.; Quinet, P.; Palmeri, P.; Biémont, É.; Asplund,
   M.; Grevesse, N.; Sauval, A. J.; Engström, L.; Lundberg, H.; Hartman,
   H.; Nilsson, H.
2009MNRAS.396.2124F    Altcode: 2009MNRAS.tmp..738F
  The solar photospheric abundance of ruthenium is revised on the basis
  of a new set of oscillator strengths derived for RuI transitions with
  wavelengths in the spectral range 2250-4710 Å. The new abundance value
  (in the usual logarithmic scale where the solar hydrogen abundance
  is equal to 12.00), A<SUB>Ru</SUB> = 1.72 +/- 0.10, is in agreement
  with the most recent meteoritic result, A<SUB>Ru</SUB> = 1.76 +/-
  0.03. The accuracy of the transition probabilities, obtained using a
  relativistic Hartree-Fock model including core-polarization effects,
  has been assessed by comparing the theoretical lifetimes with previous
  experimental results. A comparison is also made with new measurements
  performed in this work by the time-resolved laser-induced fluorescence
  spectroscopy for 10 highly excited odd-parity levels of RuI.

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Title: On the Solar Nickel and Oxygen Abundances
Authors: Scott, Pat; Asplund, Martin; Grevesse, Nicolas; Sauval,
   A. Jacques
2009ApJ...691L.119S    Altcode: 2008arXiv0811.0815S
  Determinations of the solar oxygen content relying on the neutral
  forbidden transition at 630 nm depend upon the nickel abundance,
  due to a Ni I blend. Here, we rederive the solar nickel abundance,
  using the same ab initio three-dimensional hydrodynamic model of the
  solar photosphere employed in the recent revision of the abundances
  of C, N, O, and other elements. Using 17 weak, unblended lines of
  Ni I together with the most accurate atomic and observational data
  available, we find log epsilon<SUB>Ni</SUB> = 6.17 ± 0.02(statistical)
  ± 0.05(systematic), a downward shift of 0.06-0.08 dex relative to
  previous abundances based on one-dimensional model atmospheres. We
  investigate the implications of the new nickel abundance for studies of
  the solar oxygen abundance based on the [O I] 630 nm line in the quiet
  Sun. Furthermore, we demonstrate that the oxygen abundance implied
  by the recent sunspot spectropolarimetric study of Centeno &amp;
  Socas-Navarro needs to be revised downward from log epsilon<SUB>O</SUB>
  = 8.86 ± 0.07 to 8.71 ± 0.10. This revision is based on the new
  nickel abundance, the application of the best available gf value for
  the 630 nm forbidden oxygen line, and a more transparent treatment of
  CO formation. Determinations of the solar oxygen content relying on
  forbidden lines now appear to converge around log epsilon<SUB>O</SUB>
  = 8.7.

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Title: The Solar Chemical Composition
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.
2007SSRv..130..105G    Altcode: 2007SSRv..tmp..105G
  We present our current knowledge of the solar chemical composition
  based on the recent significant downward revision of the solar
  photospheric abundances of the most abundant metals. These new solar
  abundances result from the use of a 3D hydrodynamic model of the solar
  atmosphere instead of the classical 1D hydrostatic models, accounting
  for departures from LTE, and improved atomic and molecular data. With
  these abundances, the new solar metallicity, Z, decreases to Z=0.012,
  almost a factor of two lower than earlier widely used values. We
  compare our values with data from other sources and analyse a number
  of impacts of these new photospheric abundances. While resolving a
  number of longstanding problems, the new 3D-based solar photospheric
  composition also poses serious challenges for the standard solar model
  as judged by helioseismology.

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Title: The Solar Chemical Composition
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.
2007coma.book..105G    Altcode:
  We present our current knowledge of the solar chemical composition
  based on the recent significant downward revision of the solar
  photospheric abundances of the most abundant metals. These new solar
  abundances result from the use of a 3D hydrodynamic model of the solar
  atmosphere instead of the classical 1D hydrostatic models, accounting
  for departures from LTE, and improved atomic and molecular data. With
  these abundances, the new solar metallicity, Z, decreases to Z=0.012,
  almost a factor of two lower than earlier widely used values. We
  compare our values with data from other sources and analyse a number
  of impacts of these new photospheric abundances. While resolving a
  number of longstanding problems, the new 3D-based solar photospheric
  composition also poses serious challenges for the standard solar model
  as judged by helioseismology.

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Title: Line formation in solar granulation. VII. CO lines and the
    solar C and O isotopic abundances
Authors: Scott, P. C.; Asplund, M.; Grevesse, N.; Sauval, A. J.
2006A&A...456..675S    Altcode: 2006astro.ph..5116S
  CO spectral line formation in the Sun has long been a source of
  consternation for solar physicists, as have the elemental abundances
  it seems to imply. We modelled solar CO line formation using a
  realistic, ab initio, time-dependent 3D radiative-hydrodynamic model
  atmosphere. Results were compared with space-based observations
  from the ATMOS space shuttle experiment. We employed weak
  <SUP>12</SUP>C<SUP>16</SUP>O, <SUP>13</SUP>C<SUP>16</SUP>O and
  <SUP>12</SUP>C<SUP>18</SUP>O lines from the fundamental (Δ v =
  1) and first overtone (Δ v = 2) bands to determine the solar
  carbon abundance, as well as the <SUP>12</SUP>C/<SUP>13</SUP>C
  and <SUP>16</SUP>O/<SUP>18</SUP>O isotopic ratios. A weighted
  solar carbon abundance of logɛ_C=8.39 ± 0.05 was found. We
  note with satisfaction that the derived abundance is identical to
  our recent 3D determination based on C i, [C i], C2 and CH lines,
  increasing our confidence in the accuracy of both results. Identical
  calculations were carried out using 1D models, but only the 3D
  model was able to produce abundance agreement between different
  CO lines and the other atomic and molecular diagnostics. Solar
  <SUP>12</SUP>C/<SUP>13</SUP>C and <SUP>16</SUP>O/<SUP>18</SUP>O ratios
  were measured as 86.8<SUP>+3.9</SUP><SUB>-3.7</SUB> (δ<SUP>13</SUP>C
  = 30<SUP>+46</SUP><SUB>-44</SUB>) and 479<SUP>+29</SUP><SUB>-28</SUB>
  (δ<SUP>18</SUP>O = 41<SUP>+67</SUP><SUB>-59</SUB>), respectively. These
  values may require current theories of solar system formation, such as
  the CO self-shielding hypothesis, to be revised. Excellent agreement
  was seen between observed and predicted weak CO line shapes, without
  invoking micro- or macroturbulence. Agreement breaks down for the
  strongest CO lines however, which are formed in very high atmospheric
  layers. Whilst the line asymmetries (bisectors) were reasonably
  well reproduced, line strengths predicted on the basis of C and O
  abundances from other diagnostics were weaker than observed. The
  simplest explanation is that temperatures are overestimated in the
  highest layers of the 3D simulation. Thus, our analysis supports
  the presence of a COmosphere above the traditional photospheric
  temperature minimum, with an average temperature of less than 4000
  K. This shortcoming of the 3D model atmosphere is not surprising,
  given that it was never intended to properly describe such high layers.

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Title: The new solar abundances - Part I: the observations
Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.
2006CoAst.147...76A    Altcode:
  The new solar abundances have been derived from analyses of the
  photospheric spectrum. They result from the use of a 3D hydrodynamical
  model of the solar atmosphere instead of the classical 1D hydrostatic
  models, accounting for departures from LTE when possible and improved
  atomic and molecular data. The new solar abundances are lower than
  previously recommended values and the present solar metallicity, Z,
  and Z/X, decrease to Z = 0.0122 and Z/X = 0.0165 respectively, almost
  a factor of two lower than earlier widely used values. We briefly
  discuss the new results for the most abundant elements, show why they
  are trustworthy and discuss some implications (see also Montalban et
  al. 2006, Part II).

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Title: The solar model problem resurrected
Authors: Asplund, M.; Grevesse, N.; Guedel, M.; Sauval, A. J.
2005astro.ph.10377A    Altcode:
  The new solar composition, when applied to compute a model of the Sun,
  leads to serious disagreement between the predictions of the model
  and the observations obtained by helioseismology. New measurements of
  the coronal Ne/O abundance ratio in nearby stars using X-ray spectra
  typically find high values of Ne/O=0.4 rather than 0.15 normally adopted
  for the Sun. Drake &amp; Testa (2005) suggest that this high Ne/O ratio
  is appropriate also for the Sun, which would bring the solar models
  back in agreement with the helioseismological observations. Here we
  present arguments why the high Ne/O ratio is unlikely to be applicable
  to the Sun.

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Title: The Solar Chemical Composition
Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.
2005ASPC..336...25A    Altcode:
  We review our current knowledge of the solar chemical composition
  as determined from photospheric absorption lines. In particular we
  describe the recent significant revisions of the solar abundances as a
  result of the application of a time-dependent, 3D hydrodynamical model
  of the solar atmosphere instead of 1D hydrostatic models. This has
  decreased the metal content in the solar convection zone by almost a
  factor of two compared with the widely used compilation by Anders &amp;
  Grevesse (1989). While resolving a number of long-standings problems,
  the new 3D-based element abundances also pose serious challenges,
  most notably for helioseismology.

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Title: Line formation in solar granulation. IV. [O I], O I and OH
    lines and the photospheric O abundance
Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.; Allende Prieto,
   C.; Kiselman, D.
2005A&A...435..339A    Altcode:
  A&amp;A, 417, 751-768 (2004), DOI:10.1051/0004-6361:20034328

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Title: Line formation in solar granulation. VI. [C I], C I, CH and
    C<SUB>2</SUB> lines and the photospheric C abundance
Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.; Allende Prieto,
   C.; Blomme, R.
2005A&A...431..693A    Altcode: 2004astro.ph.10681A
  The solar photospheric carbon abundance has been determined from [C
  I], C I, CH vibration-rotation, CH A-X electronic and C<SUB>2</SUB>
  Swan electronic lines by means of a time-dependent, 3D, hydrodynamical
  model of the solar atmosphere. Departures from LTE have been considered
  for the C I lines. These turned out to be of increasing importance for
  stronger lines and are crucial to remove a trend in LTE abundances
  with the strengths of the lines. Very gratifying agreement is found
  among all the atomic and molecular abundance diagnostics in spite of
  their widely different line formation sensitivities. The mean value
  of the solar carbon abundance based on the four primary abundance
  indicators ([C I], C I, CH vibration-rotation, C<SUB>2</SUB> Swan)
  is log ɛ<SUB>C</SUB> = 8.39 ± 0.05, including our best estimate of
  possible systematic errors. Consistent results also come from the CH
  electronic lines, which we have relegated to a supporting role due
  to their sensitivity to the line broadening. The new 3D based solar C
  abundance is significantly lower than previously estimated in studies
  using 1D model atmospheres.

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Title: The New Solar Chemical Composition
Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.
2005EAS....17...21G    Altcode:
  We present our current knowledge of the solar chemical composition based
  on the recent significant downward revision of the solar photospheric
  abundances of the most abundant metals very recently reviewed in detail
  by Asplund et al. (2005a). These new solar abundances result from the
  use of a 3D hydrodynamical model of the solar atmosphere instead of
  the classical 1D hydrostatic models, accounting for departures from
  LTE, and improved atomic and molecular data. With these abundances,
  the new solar metallicity, Z, and Z/X, decrease to Z = 0.012 and Z/X =
  0.0165 respectively, almost a factor of 2 lower than earlier widely
  used values. While resolving a number of longstanding problems, the new
  3D-based solar photospheric composition also poses serious challenges
  for the standard solar model.

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Title: Line formation in solar granulation. IV. [O I], O I and OH
    lines and the photospheric O abundance
Authors: Asplund, M.; Grevesse, N.; Sauval, A. J.; Allende Prieto,
   C.; Kiselman, D.
2004A&A...417..751A    Altcode: 2003astro.ph.12290A
  The solar photospheric oxygen abundance has been determined from
  [O I], O I, OH vibration-rotation and OH pure rotation lines by
  means of a realistic time-dependent, 3D, hydrodynamical model of
  the solar atmosphere. In the case of the O I lines, 3D non-LTE
  calculations have been performed, revealing significant departures
  from LTE as a result of photon losses in the lines. We derive a solar
  oxygen abundance of log ɛ<SUB>O</SUB> = 8.66 ± 0.05. All oxygen
  diagnostics yield highly consistent abundances, in sharp contrast
  with the results of classical 1D model atmospheres. This low value
  is in good agreement with measurements of the local interstellar
  medium and nearby B stars. This low abundance is also supported by
  the excellent correspondence between lines of very different line
  formation sensitivities, and between the observed and predicted line
  shapes and center-to-limb variations. Together with the corresponding
  down-ward revisions of the solar carbon, nitrogen and neon abundances,
  the resulting significant decrease in solar metal mass fraction to Z =
  0.0126 can, however, potentially spoil the impressive agreement between
  predicted and observed sound speed in the solar interior determined
  from helioseismology.

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Title: ISO-SWS calibration and the accurate modelling of cool-star
    atmospheres.  III. A0 to G2 stars
Authors: Decin, L.; Vandenbussche, B.; Waelkens, K.; Eriksson, C.;
   Gustafsson, B.; Plez, B.; Sauval, A. J.
2003A&A...400..695D    Altcode: 2002astro.ph..7636D
  Vega, Sirius, beta Leo, alpha Car and alpha Cen A belong to a
  sample of twenty stellar sources used for the calibration of
  the detectors of the Short-Wavelength Spectrometer on board the
  Infrared Space Observatory (ISO-SWS). While general problems with
  the calibration and with the theoretical modelling of these stars
  are reported in {Decin} et al. (\cite{Decin2000b}), each of these
  stars is discussed individually in this paper. As demonstrated in
  {Decin} et al. (\cite{Decin2000b}), it is not possible to deduce the
  effective temperature, the gravity and the chemical composition from
  the ISO-SWS spectra of these stars. But since ISO-SWS is absolutely
  calibrated, the angular diameter (theta<SUB>d</SUB> ) of these
  stellar sources can be deduced from their ISO-SWS spectra, which
  consequently yields the stellar radius (R), the gravity-inferred mass
  (M<SUB>g</SUB>) and the luminosity (L) for these stars. For Vega,
  we obtained theta<SUB>d</SUB> = 3.35 +/- 0.20 mas, R = 2.79 +/-
  0.17 R<SUB>sun</SUB>, M<SUB>g</SUB> = 2.54 +/- 1.21 M<SUB>sun</SUB>
  and L = 61 +/- 9 L<SUB>sun</SUB>; for Sirius theta<SUB>d</SUB> =
  6.17 +/- 0.38 mas, R = 1.75 +/- 0.11 R<SUB>sun</SUB>, M<SUB>g</SUB>
  = 2.22 +/- 1.06 M<SUB>sun</SUB> and L = 29 +/- 6 L<SUB>sun</SUB>;
  for beta Leo theta<SUB>d</SUB> = 1.47 +/- 0.09 mas, R = 1.75 +/-
  0.11 R<SUB>sun</SUB>, M<SUB>g</SUB> = 1.78 +/- 0.46 M<SUB>sun</SUB>
  and L = 15 +/- 2 L<SUB>sun</SUB>; for alpha Car theta<SUB>d</SUB> =
  7.22 +/- 0.42 mas, R = 74.39 +/- 5.76 R<SUB>sun</SUB>, M<SUB>g</SUB>
  = 12.80<SUP>+24.95</SUP><SUB>-6.35</SUB> M<SUB>sun</SUB> and L = 14573
  +/- 2268 L<SUB>sun</SUB> and for alpha Cen A theta<SUB>d</SUB> = 8.80
  +/- 0.51 mas, R = 1.27 +/- 0.08 R<SUB>sun</SUB>, M<SUB>g</SUB> = 1.35
  +/- 0.22 M<SUB>sun</SUB> and L = 1.7 +/- 0.2 L<SUB>sun</SUB>. These
  deduced parameters are confronted with other published values and the
  goodness-of-fit between observed ISO-SWS data and the corresponding
  synthetic spectrum is discussed. <P />Based on observations with ISO,
  an ESA project with instruments funded by ESA Member States (especially
  the PI countries France, Germany, The Netherlands and the UK) and with
  the participation of ISAS and NASA.}\fnmsep\thanks{Appendices A and
  B are only available in electronic form at http://www.edpsciences.org}

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Title: ISO-SWS calibration and the accurate modelling of cool-star
    atmospheres.  IV. G9 to M2 stars
Authors: Decin, L.; Vandenbussche, B.; Waelkens, C.; Decin, G.;
   Eriksson, K.; Gustafsson, B.; Plez, B.; Sauval, A. J.
2003A&A...400..709D    Altcode: 2002astro.ph..7653D
  A detailed spectroscopic study of 11 giants with spectral type
  from G9 to M2 is presented. The 2.38-4.08 mu m wavelength-range of
  band 1 of ISO-SWS (Short-Wavelength Spectrometers on board of the
  Infrared Space Observatory) in which many different molecules -
  with their own dependence on each of the stellar parameters - are
  absorbing, enables us to estimate the effective temperature, the
  gravity, the microturbulence, the metallicity, the CNO-abundances,
  the <SUP>12</SUP>C/<SUP>13</SUP>C-ratio and the angular diameter from
  the ISO-SWS data. Using the Hipparcos' parallax, the radius, luminosity
  and gravity-inferred mass are derived. The stellar parameters obtained
  are in good agreement with other published values, though also some
  discrepancies with values deduced by other authors are noted. For a
  few stars (delta Dra, xi Dra, alpha Tuc, H Sco and alpha Cet) some
  parameters - e.g. the CNO-abundances - are derived for the first
  time. By examining the correspondence between different ISO-SWS
  observations of the same object and between the ISO-SWS data and
  the corresponding synthetic spectrum, it is shown that the relative
  accuracy of ISO-SWS in band 1 (2.38-4.08 mu m) is better than 2%
  for these high-flux sources. The high level of correspondence between
  observations and theoretical predictions, together with a confrontation
  of the estimated T<SUB>eff</SUB> (ISO) value with T<SUB>eff</SUB> values
  derived from colours - which demonstrates the consistency between V-K,
  BC<SUB>K</SUB>, T<SUB>eff</SUB> and theta<SUB>d</SUB> derived from
  optical or IR data - proves that both the used MARCS models to derive
  the stellar quantities and the flux calibration of the ISO-SWS detectors
  have reached a high level of reliability. <P />Based on observations
  with ISO, an ESA project with instruments funded by ESA Member States
  (especially the PI countries France, Germany, The Netherlands and the
  UK) and with the participation of ISAS and NASA. <P />Appendices A-D
  are only available in electronic form at http://www.edpsciences.org

---------------------------------------------------------
Title: ISO-SWS calibration and the accurate modelling of cool-star
    atmospheres.  II. General results
Authors: Decin, L.; Vandenbussche, B.; Waelkens, C.; Eriksson, K.;
   Gustafsson, B.; Plez, B.; Sauval, A. J.; Hinkle, K.
2003A&A...400..679D    Altcode: 2002astro.ph..7621D
  The fine calibration of the ISO-SWS detectors (Infrared Space
  Observatory - Short Wavelength Spectrometer) has proven to be a delicate
  problem. We therefore present a detailed spectroscopic study in the
  2.38-12 mu m wavelength range of a sample of 16 A0-M2 stars used for
  the calibration of ISO-SWS. By investigating the discrepancies between
  the ISO-SWS data of these sources, the theoretical predictions of their
  spectra, the high-resolution FTS-KP (Kitt Peak) spectrum of alpha Boo
  and the solar FTS-ATMOS (Atmospheric Trace Molecule Spectroscopy)
  spectrum, both calibration problems and problems in computing the
  theoretical models and the synthetic spectra are revealed. The
  underlying reasons for these problems are sought for and the impact
  on the further calibration of ISO-SWS and on the theoretical modelling
  is discussed extensively. <P />Based on observations with ISO, an ESA
  project with instruments funded by ESA Member States (especially the
  PI countries France, Germany, The Netherlands and the UK) and with
  the participation of ISAS and NASA. <P />Appendix is only available
  in electronic form at http://www.edpsciences.org

---------------------------------------------------------
Title: The Composition of the solar photosphere
Authors: Grevesse, N.; Sauval, A. J.
2002AdSpR..30....3G    Altcode:
  The Sun is unique because chemical composition data can be derived from
  very different layers, from the center to the outermost coronal layers,
  using very different techniques like helioseismology, spectroscopy,
  particle collection techniques, … Differences in chemical composition
  are observed allowing to discover how the different solar layers
  evolve. The composition of the solar photosphere, which represents
  the composition of the outer convective zone, is the basic reference
  source of elemental abundances. We review the current status of our
  knowledge of the chemical composition of this layer and compare it
  with data from other solar sources as well as with meteoritic data.

---------------------------------------------------------
Title: ISO-SWS calibration and the accurate modelling of cool-star
    atmospheres. I. Method
Authors: Decin, L.; Waelkens, C.; Eriksson, K.; Gustafsson, B.; Plez,
   B.; Sauval, A. J.; Van Assche, W.; Vandenbussche, B.
2000A&A...364..137D    Altcode: 2000astro.ph..8316D
  A detailed spectroscopic study of the ISO-SWS data of the red
  giant alpha Tau is presented, which enables not only the accurate
  determination of the stellar parameters of alpha Tau, but also serves
  as a critical review of the ISO-SWS calibration. This study is situated
  in a broader context of an iterative process in which both accurate
  observations of stellar templates and cool star atmosphere models
  are involved to improve the ISO-SWS calibration process as well as the
  theoretical modelling of stellar atmospheres. Therefore a sample of cool
  stars, covering the whole A0 - M8 spectral classification, has been
  observed in order to disentangle calibration problems and problems
  in generating the theoretical models and corresponding synthetic
  spectrum. By using stellar parameters found in the literature large
  discrepancies were seen between the ISO-SWS data and the generated
  synthetic spectrum of alpha Tau. A study of the influence of various
  stellar parameters on the theoretical models and synthetic spectra,
  in conjunction with the Kolmogorov-Smirnov test to evaluate objectively
  the goodness-of-fit, enables us to pin down the stellar parameters with
  a high accuracy: T<SUB>eff</SUB> = 3850 +/- 70 K, log g = 1.50 +/- 0.15,
  M = 2.3 +/- 0.8 M<SUB>sun</SUB>, z = -0.15 +/- 0.20 dex, xi<SUB>t</SUB>
  = 1.7 +/- 0.3 km s<SUP>-1</SUP>, <SUP>12</SUP>C/<SUP>13</SUP>C = 10
  +/- 1, varepsilon (C) = 8.35 +/- 0.20 dex, varepsilon (N) = 8.35 +/-
  0.25 dex, varepsilon (O) = 8.83 +/- 0.15 dex and theta<SUB>d</SUB> =
  20.77 +/- 0.83 mas. These atmospheric parameters were then compared
  with the results provided by other authors using other methods
  and/or spectra. Based on observations with ISO, an ESA project with
  instruments funded by ESA Member States (especially the PI countries
  France, Germany, the Netherlands and the United Kingdom) and with the
  participation of ISAS and NASA.

---------------------------------------------------------
Title: ISO Impact on Stellar Models and Viceversa
Authors: Decin, L.; Waelkens, C.; Eriksson, K.; Gustafsson, B.; Plez,
   B.; Sauval, A. J.; van Assche, W.; Vandenbussche, B.
2000ESASP.456..289D    Altcode: 2000astro.ph..8362D; 2000ibp..conf..289D
  We present a detailed spectroscopic study of a sample of bright,
  mostly cool, stars observed with the Short-Wavelength Spectrometer
  (SWS) on board ISO, which enables the accurate determination of the
  stellar parameters of the cool giants, but also serves as a critical
  review of the ISO-SWS calibration.

---------------------------------------------------------
Title: Solar Abundances
Authors: Grevesse, N.; Sauval, A.
2000eaa..bookE1979G    Altcode:
  What is the Sun made of? This fundamental question only received an
  answer about 70 years ago. H N RUSSELL, whose name is associated with
  much pioneering research in astrophysics during the first half of this
  century as well as with a series of basic work in atomic spectroscopy,
  made the first quantitative analysis of the chemical composition of
  the SOLAR PHOTOSPHERE in 1929. Using eye estimates ...

---------------------------------------------------------
Title: Abundances of the Elements in the Sun
Authors: Grevesse, N.; Sauval, A. J.
2000orel.conf..261G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The solar abundance of iron and the photospheric model
Authors: Grevesse, N.; Sauval, A. J.
1999A&A...347..348G    Altcode:
  Numerous papers on the solar photospheric abundance of iron have
  recently been published leading to a longstanding debate concerning
  rather different results obtained from the analyses of Fe i lines
  and, to a lesser extent, of Fe ii lines. Based on a set of 65 solar
  Fe i lines, with accurate transition probabilities as well as new
  accurate damping constants, we construct a new empirical photospheric
  model. We succeed to reconcile abundance results obtained from low
  and high excitation Fe i lines as well as from Fe ii lines and derive
  a solar photospheric abundance of iron, A_Fe = 7.50 +/- 0.05, which
  perfectly agrees with the meteoritic value. A detailed version of
  Table~2 is available in electronic form at the CDS via anonymous ftp
  to cdsarc.u-strasbg.fr (130.79.128.5) or at the ORB via anonymous ftp
  to ftpserver.oma.be/pub/astro/jacques.

---------------------------------------------------------
Title: VizieR Online Data Catalog: Solar abundance of iron (Grevesse+,
    1999)
Authors: Grevesse, N.; Sauval, A. J.
1999yCat..33470348G    Altcode:
  Numerous papers on the solar photospheric abundance of iron have
  recently been published leading to a longstanding debate concerning
  rather different results obtained from the analyses of Fe I lines
  and, to a lesser extent, of Fe II lines. Based on a set of 65 solar
  Fe I lines, with accurate transition probabilities as well as new
  accurate damping constants, we construct a new empirical photospheric
  model. We succeed to reconcile abundance results obtained from low
  and high excitation Fe I lines as well as from Fe II lines and derive
  a solar photospheric abundance of iron, A<SUB>Fe</SUB>=7.50+/-0.05,
  which perfectly agrees with the meteoritic value. (1 data file).

---------------------------------------------------------
Title: Standard Solar Composition
Authors: Grevesse, N.; Sauval, A. J.
1998SSRv...85..161G    Altcode:
  We review the current status of our knowledge of the chemical
  composition of the Sun, essentially derived from the analysis of the
  solar photospheric spectrum. The comparison of solar and meteoritic
  abundances confirms that there is a very good agreement between the
  two sets of abundances. They are used to construct a Standard Abundance
  Distribution.

---------------------------------------------------------
Title: Standard Solar Composition
Authors: Grevesse, N.; Sauval, A. J.
1998sce..conf..161G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Standard Abundances
Authors: Grevesse, N.; Noels, A.; Sauval, A. J.
1996ASPC...99..117G    Altcode: 1996coab.proc..117G
  No abstract at ADS

---------------------------------------------------------
Title: A new analysis of the OH radical spectrum from solar infrared
    observations.
Authors: Melen, F.; Sauval, A. J.; Grevesse, N.; Farmer, C. B.;
   Servais, Ch.; Delbouille, L.; Roland, G.
1995JMoSp.174..490M    Altcode:
  The solar spectrum offered the opportunity to discover OH lines with
  high rotational quantum numbers, which do not appear on laboratory
  spectra. On solar absorption spectra, the authors have identified
  about 580 lines, among which about 400 were observed for the first
  time. They belong to pure rotational transitions in the ground state
  (υ = 0→3; J<SUB>max</SUB>″= 48.5), as well as to the (1-0), (2-1),
  and (3-2) vibration-rotation bands (J<SUB>max</SUB>″= 32.5). Previous
  pure rotation, vibration-rotation, and Λ-doubling data sets related
  to the υ = 0 up to 3 levels were fitted simultaneously together with
  this new set of data, in order to obtain a very complete and accurate
  set of molecular constants for the X<SUP>2</SUP>Π ground state.

---------------------------------------------------------
Title: High excitation Rydberg levels of Fe I from the ATMOS solar
    spectrum at 2.5 and 7 μm.
Authors: Schoenfeld, W. G.; Chang, E. S.; Geller, M.; Johansson, S.;
   Nave, G.; Sauval, A. J.; Grevesse, N.
1995A&A...301..593S    Altcode:
  The quadrupole-polarization theory has been applied to the
  3d^6^4s(^6^D)4f and 5g subconfigurations of Fe I by a parametric fit,
  and the fitted parameters are used to predict levels in the 6g and
  6h subconfigurations. Using the predicted values, we have computed
  the 4f-6g and 5g-6h transition arrays and made identifications in the
  ATMOS infrared solar spectrum. The newly identified 6g and 6h levels,
  based on ATMOS wavenumbers, are combined with the 5g levels and found to
  agree with the theoretical values with a root mean-squared-deviation of
  0.042cm^-1^. Our approach yields a polarizability of 28.07 a_o_^3^and
  a quadrupole moment of 0.4360+/-0.0010ea_o_^2^for Fe II, as well as
  an improved ionization potential of 63737.700+/-0.010cm^-1^ for Fe I.

---------------------------------------------------------
Title: Charles FIEVEZ; 13 Years of Spectroscopy at the Observatoire
    Royal de Bruxelles (1877-1890)
Authors: Sauval, A. J.
1995ASPC...81....3S    Altcode: 1995lahr.conf....3S
  No abstract at ADS

---------------------------------------------------------
Title: A New Analysis of the OH Radical Spectrum from Solar Infrared
    Observations
Authors: Melen, F.; Grevesse, N.; Delbouille, L.; Roland, G.; Servais,
   C.; Sauval, A. J.; Farmer, C. B.
1995ASPC...81..320M    Altcode: 1995lahr.conf..320M
  No abstract at ADS

---------------------------------------------------------
Title: Workshop on Laboratory and Astronomical High Resolution
Spectra : held in Brussels, Belgium 29 August-2 September 1994 in
    honour of the 150th birthday of Charles Vievez (1844-1890), the
    pioneer of astronomical spectroscopy in Belgium
Authors: Sauval, A. J.; Blomme, R.; Grevesse, N.
1995ASPC...81.....S    Altcode: 1995lahr.conf.....S
  No abstract at ADS

---------------------------------------------------------
Title: Atomic and Molecular Data in Solar Photospheric Spectroscopy
Authors: Grevesse, N.; Noels, A.; Sauval, A. J.
1995ASPC...81...74G    Altcode: 1995lahr.conf...74G
  No abstract at ADS

---------------------------------------------------------
Title: Statement
Authors: Sauval, A. J.; Blomme, R.; Grevasse, N.
1995ASPC...81..627S    Altcode: 1995lahr.conf..627S
  No abstract at ADS

---------------------------------------------------------
Title: Analysis of the 3d 64 s( 6D)4f--5g Supermultiplet of Fe i in
    Laboratory and Solar Infrared Spectra
Authors: Johansson, S.; Nave, G.; Geller, M.; Sauval, A. J.; Grevesse,
   N.; Schoenfeld, W. G.; Change, E. S.; Farmer, C. B.
1994ApJ...429..419J    Altcode: 1994astro.ph..4050J
  The combined laboratory and solar analysis of the highly-excited
  subconfigurations 4f and 5g of Fe I has allowed us to classify 87
  lines of the 4f-5g supermultiplet in the spectral region 2545-2585
  cm-1. The level structure of these JK-coupled configurations
  is predicted by semiempirical calculations and the quadrupolic
  approximation. Semiempirical gf-values have been calculated and
  are compared to gf values derived from the solar spectrum. The solar
  analysis has shown that these lines, which should be much less sensitive
  than lower excitation lines to departures from LTE and to temperature
  uncertainties, lead to a solar abundance of iron which is consistent
  with the meteoritic value (A_Fe = 7.51).

---------------------------------------------------------
Title: The Sun as a Laboratory Source for IR Molecular Spectroscopy
Authors: Sauval, A. J.; Grevesse, N.
1994IAUS..154..549S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Analysis of Very High Excitation Fe I Lines (4f - 5g) in the
    Solar Infrared Spectrum
Authors: Johansson, S.; Nave, G.; Geller, M.; Sauval, A. J.;
   Grevesse, N.
1994IAUS..154..543J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Molecules in the Sun and Molecular Data
Authors: Grevesse, Nicolas; Sauval, A. Jacques
1994LNP...428..196G    Altcode: 1994mse..conf..196G; 1994IAUCo.146..196G
  No abstract at ADS

---------------------------------------------------------
Title: Solar Abundances of C; N; O
Authors: Grevesse, N.; Sauval, A. J.; Blomme, R.
1994IAUS..154..539G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Line Shifts Asymmetries in the IR Solar Spectrum
Authors: Blomme, R.; Sauval, A. J.; Grevesse, N.
1994IAUS..154..533B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Data for the CN red System from solar lines
Authors: Sauval, A. J.; Blomme, R.; Grevesse, N.
1994msep.conf..107S    Altcode: 1994IAUCo.146P.107S
  No abstract at ADS

---------------------------------------------------------
Title: A revision of the solar abundance of dysprosium
Authors: Grevesse, N.; Noels, A.; Sauval, A. J.
1993A&A...271..587G    Altcode:
  The solar abundance of dysprosium is reevaluated from a new analysis of
  solar Dy II lines for which new accurate gf-values have recently been
  measured by Kusz (1992). The new result, A<SUB>Dy</SUB> = 1.14±0.08,
  is in pretty good agreement with the meteoritic value.

---------------------------------------------------------
Title: On the accuracy of CO line positions for high resolution IR
    stellar spectroscopy
Authors: Sauval, A. J.; Farrenq, R.; Guelachvili, G.; Grevesse, N.;
   Farmer, C. B.; Norton, R. H.
1992A&A...265..355S    Altcode:
  The paper demonstrates the high accuracy of line positions derived from
  improved sets of Dunham coefficients for the four more abundant isotopic
  species of carbon monoxide - (C-12)(O-16), (C-13)(O-16), (C-12)(O-18),
  and (C-12)(O-17) - which are present in the sun and in cool stellar
  atmospheres. These new spectroscopic constants make it possible to
  predict very accurate positions of CO lines at any J-values, especially
  at very high rotational excitation (up to J around 135). Earlier
  proposed identifications of CO lines at large J-values are checked,
  and some incorrect identifications in sunspot spectra are found. The
  present accurate line positions are also compared with predictions from
  other available sets of molecular constants. It is concluded that the
  present improved sets of molecular constants are the most appropriate
  to all problems of high-resolution stellar and solar spectroscopy at
  any J- and v-values, particularly for synthetic spectra of cool stars.

---------------------------------------------------------
Title: Photospheric abundances.
Authors: Grevesse, Nicolas; Noels, A.; Sauval, A. J.
1992ESASP.348..305G    Altcode: 1992cscl.work..305G
  The authors review the photospheric abundances of the chemical elements
  which are observed in the coronal spectrum, in the solar wind and in
  solar energetic particle events.

---------------------------------------------------------
Title: Molecular Data from Solar Spectroscopy
Authors: Grevesse, N.; Sauval, A. J.
1992RMxAA..23...71G    Altcode:
  We show through a few examples how the analysis of molecular transitions
  present in the solar visible and infrared spectrum can be used to refine
  our knowledge of the molecular constants and to test the accuracy of
  available molecular data like transition probabilities and dissociation
  energies for a few diatomic molecules. Key words: ATOMIC PROCESSES -
  MOLECULAR PROCESSES - SUN: ATMOSPHERE - SUN: SPECTRA

---------------------------------------------------------
Title: Improved Dunham coefficients for CO from infrared solar lines
    of high rotational excitation
Authors: Farrenq, R.; Guelachvili, G.; Sauval, A. J.; Grevesse, N.;
   Farmer, C. B.
1991JMoSp.149..375F    Altcode:
  About 4500 unblended CO lines have been selected and their wavenumbers
  accurately measured on high resolution solar spectra obtained from
  space with the ATMOS Fourier transform spectrometer. Half of these lines
  are of high rotational excitation energy and have never been observed
  before in the laboratory. Line positions of the fundamental bands of
  <SUP>12</SUP>C<SUP>16</SUP>O have been measured up to J = 133, those
  of <SUP>13</SUP>C<SUP>16</SUP>O and of <SUP>12</SUP>C<SUP>18</SUP>O
  up to J = 103 and 91, respectively. The first overtone bands of
  <SUP>12</SUP>C<SUP>16</SUP>O have been measured up to J = 110. These
  new solar CO wavenumbers, with an additional selected set of about 14
  000 accurate laboratory measurements, have been simultaneously fitted to
  the Dunham expression utilizing 10 recently published relations between
  isotopically invariant parameters U<SUB>ij</SUB>. The present set of
  coefficients reproduces all accurate laboratory positions and our solar
  measurements of high rotational excitation with a standard deviation
  of about 10<SUP>-5</SUP> cm<SUP>-1</SUP> (300kHz). This new set is
  particularly recommended for all high resolution studies of infrared
  laboratory and stellar spectra showing CO lines of high J-values. <P
  />It is with deep sorrow that we report the demise of R. H. Norton on
  March 22, 1991. His participation in this research was much appreciated.

---------------------------------------------------------
Title: First identification of pure rotation lines of NH in the
    infrared solar spectrum
Authors: Geller, M.; Farmer, C. B.; Norton, R. H.; Sauval, A. J.;
   Grevesse, N.
1991A&A...249..550G    Altcode:
  Pure rotation lines of NH of the v = 0 level and v = 1 level are
  detected in high-resolution solar spectra obtained from the Atmospheric
  Trace Molecule Spectroscopy (ATMOS) experimental observations. It
  is pointed out that the identification of the lines is favored by the
  typical appearance of the triplet lines of nearly equal intensities. The
  observed equivalent widths of these triplet lines are compared with
  predicted intensities, and it is observed that these widths are
  systematically larger than the predicted values. It is noted that
  because these very faint lines are observed in a region where the signal
  is very low, a systematic error in the measurements of the equivalent
  widths cannot be ruled out; therefore, the disagreement between the
  observed and predicted intensities is not considered to be real.

---------------------------------------------------------
Title: Vibration-rotation bands of CH in the solar infrared spectrum
    and the solar carbon abundance
Authors: Grevesse, N.; Lambert, D. L.; Sauval, A. J.; van Dishoeck,
   E. F.; Farmer, C. B.; Norton, R. H.
1991A&A...242..488G    Altcode:
  High resolution solar spectra obtained from the ATMOS Fourier Transform
  Spectrometer (Spacelab 3 flight on April 29-May 6, 1985) have made
  it possible to identify and measure a large number of lines of the
  vibration-rotation fundamental bands of the X2 Pi state of CH. From
  about 100 lines of the 1-0, 2-1, and 3-2 bands and adopting theoretical
  transition probabilities, a solar carbon abundance of 8.60 + or -
  0.05 is derived. This value is compared with new results inferred
  from other carbon abundance indicators. The final recommended solar
  abundance of carbon is 8.60 + or - 0.05.

---------------------------------------------------------
Title: The infrared solar spectrum
Authors: Grevesse, N.; Sauval, A. J.
1991STIN...9413502G    Altcode:
  The spectrum of the quiet Sun at wavelengths larger than about 1
  micrometer (or wavenumbers shorter than 10,000/cm) are described. The
  main characteristics of studying the solar spectrum in the infrared
  region are summarized. The new high resolution low noise solar spectra
  obtained by the Atmospheric Trace Molecule Spectroscopy (ATMOS) Fourier
  transform spectrometer experiment on board the Space Shuttle are
  considered. Atomic and molecular spectroscopy/line identification are
  discussed. Solar observations in the infrared are summarized. Recent
  analyses have led to a better understanding of the heterogeneous
  structure of the solar outer layers: thermal bifurcation between the
  cool photosphere and the hot flux tube chromosphere, convective motions
  in the photosphere, oscillations in the photosphere and chromosphere,
  magnetic fields and shapes of the flux tubes, etc.

---------------------------------------------------------
Title: The Infrared Solar Spectrum
Authors: Grevesse, N.; Sauval, A. J.
1991isrs.conf..215G    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Identification of solar vibration-rotation lines of NH and
    the solar nitrogen abundance
Authors: Grevesse, N.; Lambert, D. L.; Sauval, A. J.; van Dishoeck,
   E. F.; Farmer, C. B.; Norton, R. H.
1990A&A...232..225G    Altcode:
  High resolution solar spectra obtained from the ATMOS Fourier Transform
  Spectrometer (Spacelab 3 flight on April 29 - May 6, 1985) made it
  possible to detect for the first time vibration-rotation lines of NH
  from the X3 Sigma(-) state near 3 microns. Using recent theoretical
  results for the transition probabilities of 23 selected measured lines
  of the 1-0 and 2-1 bands, a solar abundance of nitrogen of 8.06 + or -
  0.07 is derived. This value is compared with the result derived from
  N I lines and agrees with the abundance obtained from the 3s-3p, 3p-3d
  and 3s-prime - 3p-prime transitions, A(N) = 8.00 + or - 0.09. The final
  recommended solar abundance of nitrogen is A(N) = 8.00 + or - 0.05.

---------------------------------------------------------
Title: A new analysis of the vibration-rotation spectrum of CH from
    solar spectra
Authors: Melen, F.; Grevesse, N.; Sauval, A. J.; Farmer, C. B.;
   Norton, R. H.; Bredohl, H.; Dubois, I.
1989JMoSp.134..305M    Altcode:
  In the solar spectrum, CH vibration-rotation lines are excited to
  higher vibrational and much higher rotational quantum numbers than in
  any laboratory source. We have observed, for the first time, a very
  large number of new lines (1-0 and 2-1 up to J = 34.5, 3-2 up to J =
  31.5, and even 4-3, never seen before, up to J = 24.5) on solar spectra
  obtained from space, with the ATMOS-SL3 instrument. A total of 558
  lines have been used to derive new accurate molecular constants for
  the X<SUP>2</SUP>Π ground state of CH.

---------------------------------------------------------
Title: Concentrations of hydrogen chloride and hydrogen fluoride
    measured during the MAP/GLOBUS campaign of September 1983
Authors: Zander, R.; Roland, G.; Delbouille, L.; Sauval, A. J.;
   Marché, P.; Karcher, F.; Amoudei, M.; Dufour, B.
1987P&SS...35..665Z    Altcode:
  Within the context of the MAP/GLOBUS campaign of September 1983,
  several trace species have been observed by absorption spectroscopy
  at the two ground stations of the Jungfraujoch, Switzerland (3580
  m altitude) and the Observatoire de Haute-Provence, France (1905 m
  altitude). The results obtained for HCl and for HF, expressed in terms
  of mean integrated columns above these sites are: Jungfraujoch: (2.1 ±
  0.2) E15 mol cm <SUP>-2</SUP> HCl (4.8 ± 0.2) E14 mol cm <SUP>-2</SUP>
  HF Haute-Provence: (2.6 ± 0.2) E15 mol cm <SUP>-2</SUP> HCl. Taking
  into account the difference in the altitude of the two stations,
  the reported HC1 results are in agreement to within their respective
  uncertainties. The integrated column density of HCl and HF above 11 km
  altitude, deduced from airplane observations on 9 September 1983, are:
  (1.65 ± 0.25) E15 mol cm <SUP>-2</SUP> HCl above 11 km (3.7 ± 1.7)
  E14 mol cm <SUP>-2</SUP> HF above 10 km supporting satisfactorily the
  ground measurements.

---------------------------------------------------------
Title: Diatomic molecules in the solar infrared spectrum from
    ATMOS-SL3 highresolution observations.
Authors: Grevesse, Nicolas; Sauval, A. J.; Farmer, C. B.; Norton, R. H.
1987LIACo..27..111G    Altcode: 1987oahp.proc..111G
  The ATMOS Fourier Transform Spectrometer has observed, for the first
  time, the solar infrared spectrum, from 2 to 16 microns, free of
  any telluric absorption. A very large number of molecular lines are
  present on these high quality spectra: vibration-rotation lines of CO
  (Delta-v = 1 and 2; including the isotopic species C-13, O-18 and O-17),
  CH, NH, OH and pure rotation lines of OH. The analysis of these lines
  will allow to derive accurate values for the solar abundances of C,
  N and O and the isotopic ratios C-13/C-12, O-18/O-16, and O-17/O-16,
  to test the photospheric model from high to deep layers, to test the
  electric dipole moment functions of the different molecules and to
  derive much better molecular constants for CH.

---------------------------------------------------------
Title: Identification of vibration-rotation lines of CH in the solar
    infrared spectrum
Authors: Sauval, A. J.; Grevesse, N.
1985AExpr...1..153S    Altcode:
  Transitions of the fundamental band of CH have recently been measured
  with very high accuracy by Lubic and Amano (1984). The lines are
  shown to be present in the solar infrared spectrum (2580 - 2940
  cm<SUP>-1</SUP>). The role these lines could play in solar and stellar
  spectroscopy is discussed.

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Title: The Interest of Simultaneous Spectral and Spatial High
    Resolution Spectroscopy in the Infrared
Authors: Delbouille, L.; Grevesse, N.; Sauval, A. J.
1985LNP...233..108D    Altcode: 1985hrsp.proc..108D
  Up to the present, small scale structures on the sun have mostly been
  studied through observations made in the visible and ultraviolet. After
  having recalled some of the main advantages of infrared observations,
  the authors give a few samples of high spectral resolution/low noise
  solar spectra now routinely obtained in this spectral range by using
  Fourier transform spectrometers. The authors then show that such high
  spectral resolution spectra could be obtained in short period of time
  and for small scale solar structures, using a LEST type collector.

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Title: The interest of simultaneous spectral and spatial high
    resolution spectroscopy in the infrared.
Authors: Delbouille, L.; Grevesse, N.; Sauval, A. J.
1985CoORB..80.....D    Altcode:
  After having recalled some of the main advantages of infrared
  observations, the authors give a few samples of high spectral
  resolution/low noise solar spectra now routinely obtained in this
  spectral range by using Fourier transform spectrometers. They then show
  that such high resolution spectra could be obtained in a short period of
  time and for small-scale solar structures, using a LEST type collector.

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Title: An analysis of vibration-rotation lines of OH in the solar
    infrared spectrum
Authors: Grevesse, N.; Sauval, A. J.; van Dishoeck, E. F.
1984A&A...141...10G    Altcode:
  High resolution solar spectra have permitted the measurement with great
  accuracy of equivalent widths of vibration-rotation lines of OH in the
  X2Pi state near 3-micron wavelength. Using recent theoretical results
  for the transition probabilities, a solar oxygen abundance of (8.93 +
  or - 0.02) is derived which is in perfect agreement with the abundance
  deduced from the OH pure rotation lines. The solar abundance of oxygen
  is therefore A(O) = 8.92 + or - 0.035, as inferred from the analysis
  of 43 vibration-rotation lines and 81 pure rotation lines of the OH
  molecule. It is confirmed that the dipole moment function of Werner,
  Rosmus and Reinsch (1983) together with the Holweger-Mueller (1974)
  solar atmosphere model are to be preferred in the analysis of the data.

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Title: A set of partition functions and equilibrium constants for
    300 diatomic molecules of astrophysical interest
Authors: Sauval, A. J.; Tatum, J. B.
1984ApJS...56..193S    Altcode:
  Polynomial developments for partition functions and equilibrium
  constants of 300 diatomic molecules and of relevant atoms are given for
  a temperature range from 1000 to 9000K. All molecular spectroscopic
  data, with a few exceptions, are derived from the book by Huber and
  Herzberg in order to lead to a homogeneous set of data.

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Title: The pure rotation spectrum of OH and the solar oxygen abundance
Authors: Sauval, A. J.; Grevesse, N.; Zander, R.; Brault, J. W.;
   Stokes, G. M.
1984ApJ...282..330S    Altcode:
  High-resolution low-noise spectroscopic observations of the sun obtained
  in the 10.6-13-micron range using the Fourier-transform spectrometer at
  Kitt Peak National Observatory are reported. About 100 pure rotation
  lines of the X 2Pi electronic state of OH with v = 0, 1, 2, and 3
  are identified and characterized. The data are presented in tables
  and graphs and used to calculate the solar O abundance as 8.91 + or -
  0.01 (in agreement with Lambert, 1978). Agreement is also found with
  the electric-dipole-moment function of Werner et al. (1983) and the
  photospheric model of Holweger and Mueller (1974).

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Title: Molecules in red-giant stars. I - Column densities in models
    for K and M stars
Authors: Johnson, H. R.; Sauval, A. J.
1982A&AS...49...77J    Altcode:
  Weighted column densities have been calculated for neutral atoms
  and ions of most elements and for many molecules in 6 selected model
  atmospheres of red-giant stars (2500 ≤ T<SUB>eff</SUB> ≤ 4000 K)
  with solar composition. These comprise the most abundant molecules from
  a total of about 1600 compounds analyzed. This calculation provides
  a guide for identification of new molecular bands in cool stellar
  spectra and for laboratory analysis of those molecules of stellar
  interest which are as yet not studied spectroscopically.

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Title: Infrared bands of C2 in the solar photospheric spectrum
Authors: Brault, J. W.; Testerman, L.; Grevesse, N.; Sauval, A. J.;
   Delbouille, L.; Roland, G.
1982A&A...108..201B    Altcode:
  Lines of the C<SUB>2</SUB> Phillips system have been successfully
  searched for on new tracings of high resolution solar spectra. From a
  rather large number of lines of the (0,0), (1,0), and (0, 1) bands,
  we derive empirical values for the band oscillator strengths:
  f<SUB>00</SUB> = 1.41 10<SUP>-3</SUP>, f<SUB>10</SUB> = 1.38
  10<SUP>-3</SUP>, and f<SUB>01</SUB> = 1.12 10<SUP>-3</SUP>. These
  solar f-values are discussed in section 3.1 and compared with recent
  laboratory data. <P />For the Ballik-Ramsay system, only a few
  unblended solar lines have been available, from which we deduced 0.6
  10<SUP>-3</SUP> ≪ f<SUB>00</SUB> ≪ 1.2 10<SUP>-3</SUP>.

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Title: Molecular Data Needed in Stellar Spectroscopy Studies
Authors: Grevesse, N.; Sauval, A. J.
1980LIACo..21..289G    Altcode: 1980smsl.conf..289G
  No abstract at ADS

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Title: Theoretical molecular abundances in cool stellar models
Authors: Johnson, H. R.; Sauval, A. J.
1980LIACo..21..201J    Altcode: 1980smsl.conf..201J
  No abstract at ADS

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Title: A search for faint molecular lines in the solar photospheric
    spectrum
Authors: Sauval, A. J.; Biemont, E.; Grevesse, N.; Zander, R.
1980LIACo..21..235S    Altcode: 1980smsl.conf..235S
  No abstract at ADS

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Title: Predicted presence and tentative identification of new
    molecules in the pure S star R Cyg.
Authors: Sauval, A. J.
1978A&A....62..295S    Altcode:
  A new approach to the problem of the identification of molecular
  features observed in the spectra of pure S stars has been
  attempted. From calculations of the chemical equilibrium in cool
  stellar models, including a very large number of compounds, a first
  selection has been made among molecules which ought to be present in
  S stars. On the basis of these predictions, a search has been made
  for bands of these new compounds in spectrograms of R Cyg recently
  obtained by Wyckoff and Wehinger. The presence of some new molecules,
  such as HfO and TaO, in this pure S star is proposed, but the lack of
  complete laboratory data and the existence of numerous blends in the
  stellar spectrum render very difficult any definite identification.

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Title: Conditions d'observation des Comètes périodiques Encke et
    Grigg-Skjellerup en 1977
Authors: Debehogne, H.; Sauval, A. J.
1976C&T....92..333D    Altcode:
  No abstract at ADS

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Title: Influence of Uncertainties of Molecular Data upon the
    Determination of Abundances in Cool Stars
Authors: Sauval, A. J.
1976IAUS...72...21S    Altcode:
  No abstract at ADS

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Title: The CO fundamental bands in the solar spectrum.
Authors: Muller, C.; Sauval, A. J.
1975A&A....39..445M    Altcode:
  The result of a study of CO lines in the delta v equals 1 bands in
  the solar disk spectrum is presented. Recently, the photospheric
  spectrum has been recorded using a balloon-borne spectrometer from
  40 km altitude. From a comparison between the observed and synthetic
  solar spectra, an agreement is shown using the best available solar
  and molecular data. Results are discussed and compared with other
  investigations in order to explain an apparent discrepancy between
  previous results.

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Title: The CO fundamental bands in the solar spectrum
Authors: Muller, C.; Sauval, A. J.
1975STIN...7530990M    Altcode:
  The results of a study of CO lines in the * delta v equals 1 bands in
  the solar disk spectrum are presented. The photospheric spectrum is
  recorded using a balloon-borne spectrometer from 40 km altitude. From
  a comparison between the observed and synthetic solar spectra are
  compared. An agreement is shown using the best available solar
  and molecular data. Results are discussed and compared with other
  investigations and explain an apparent discrepancy among previous
  results.

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Title: K. R. Lang - Astrophysical Formulae
Authors: Sauval, A. J.
1975C&T....91..320S    Altcode:
  No abstract at ADS

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Title: A Study of Molecular Lines in the Solar Photospheric Spectrum
Authors: Grevesse, N.; Sauval, A. J.
1973A&A....27...29G    Altcode:
  Summary. We have analysed the behaviour of lines of C2, CH, CN, MgH,
  NH and OH in the solar photospheric spectrum. Recently observed
  profiles of these lines have been measured and compared with
  profiles computed using recent solar and molecular data. The main
  results of this comparison are (I) there is good agreement between
  observed and calculated profiles for most of the molecular bands;
  (11) but large disagreements appear in the case of CN and MgH; these
  discrepancies cannot be explained satisfactorily, although different
  possible suggestions are investigated. In the Appendix, a review of
  the different experimental band oscillator strengths is presented
  and mean laboratory values are proposed. Key words: solar spectrum -
  molecular lines - molecular oscillator strengths

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Title: A Search for CH+ in the Solar Photospheric Spectrum
Authors: Grevesse, N.; Sauval, A. J.
1971A&A....14..477G    Altcode:
  We present the results of a search for lines of CH+ (A1H - X1 +
  transition) in the solar photospheric spectrum. We conclude that if CH+
  is present, the equivalent widths of the most intense lines cannot
  exceed 2 mA. An empirical solar !00-value is derived and compared
  with a laboratory value and other available astrophysical values. Some
  possible reasons are given for explaining the large discrepancy between
  laboratory and astrophysical !00-values - Key words: solar spectrum -
  molecules - oscillator strengths

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Title: Oscillator strengths for SiH and SiH<SUP>+</SUP> deduced from
    the solar spectrum.
Authors: Grevesse, N.; Sauval, A. J.
1971JQSRT..11...65G    Altcode:
  No abstract at ADS

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Title: Identification of SiH~ in the Solar Photospheric Spectrum
Authors: Grevesse, N.; Sauval, A. J.
1970A&A.....9..232G    Altcode:
  We present the first convincing identification of a molecular ion in a
  stellar atmosphere: the absorption band spectrum of SiH+ (transition
  A 1H - X i +) in the solar photospheric spectrum. Values of the band
  oscillator strengths have been deduced for two bands: too = 0.0005
  and !oi = 0.0004.

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Title: Identification of SiH Lines in the Solar Disk Spectrum
Authors: Sauval, A. J.
1969SoPh...10..319S    Altcode:
  A new investigation of the presence of SiH lines in the solar disk
  spectrum has been performed. It may be concluded that molecular
  absorption lines of SiH are present in the disk spectrum with maximum
  equivalent widths of about 2 mÅ. A value of the oscillator strength
  of SiH has been derived (f<SUB>00</SUB> = 0.0008 ± 0.0004).

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Title: The solar continuum from 900 to 130 000 Å and the photospheric
    temperature model
Authors: Sauval, A.
1968SoPh....3...89S    Altcode:
  In order to obtain a better agreement between observed and computed
  values of the solar intensity, an improved temperature distribution is
  deduced for the range 0.02&lt;τ0&lt; 10. The intensity observations
  here considered refer to the wavelength region between λ 1980 and λ
  129 500, and the center-limb variations generally go down to cosθ =
  0.1. The improved model, given in Figure 4 and Table II, differs rather
  little from the Utrecht 1964 model, used here as a reference.

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Title: Le projet West Ford
Authors: Sauval, A.
1963C&T....79...12S    Altcode:
  No abstract at ADS