grevesse

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Author name code: grevesse
ADS astronomy entries on 2022-09-14
author:"Grevesse, Nicolas"

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Title: The internal rotation of the Sun and its link to the solar
Li and He surface abundances
Authors: Eggenberger, P.; Buldgen, G.; Salmon, S. J. A. J.; Noels,
A.; Grevesse, N.; Asplund, M.
2022NatAs...6..788E Altcode: 2022NatAs.tmp..119E
The Sun serves as a natural reference for the modelling of the various
physical processes at work in stellar interiors. Helioseismology
results, which inform us on the characterization of the interior of
the Sun (such as, for example, the helium abundance in its envelope),
are, however, at odds with heavy element abundances. Moreover,
the solar internal rotation and surface abundance of lithium have
always been challenging to explain. We present results of solar models
that account for transport of angular momentum and chemicals by both
hydrodynamic and magnetic instabilities. We show that these transport
processes reconcile the internal rotation of the Sun, its surface
lithium abundance, and the helioseismic determination of the envelope
helium abundance. We also show that the efficiency of the transport of
chemicals required to account for the solar surface lithium abundance
also predicts the correct value of helium, independently from a specific
transport process.

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Title: The solar carbon, nitrogen, and oxygen abundances from a 3D
LTE analysis of molecular lines
Authors: Amarsi, A. M.; Grevesse, N.; Asplund, M.; Collet, R.
2021A&A...656A.113A Altcode: 2021arXiv210904752A
Carbon, nitrogen, and oxygen are the fourth, sixth, and third most
abundant elements in the Sun. Their abundances remain hotly debated due
to the so-called solar modelling problem that has persisted for almost
20 years. We revisit this issue by presenting a homogeneous analysis
of 408 molecular lines across 12 diagnostic groups, observed in the
solar intensity spectrum. Using a realistic 3D radiative-hydrodynamic
model solar photosphere and local thermodynamic equilibrium (LTE)
line formation, we find log ϵC = 8.47 ± 0.02, log
ϵN = 7.89 ± 0.04, and log ϵO = 8.70 ±
0.04. The stipulated uncertainties mainly reflect the sensitivity of
the results to the model atmosphere; this sensitivity is correlated
between the different diagnostic groups, which all agree with the
mean result to within 0.03 dex. For carbon and oxygen, the molecular
results are in excellent agreement with our 3D non-LTE analyses of
atomic lines. For nitrogen, however, the molecular indicators give
a 0.12 dex larger abundance than the atomic indicators, and our
best estimate of the solar nitrogen abundance is given by the mean:
7.83 dex. The solar oxygen abundance advocated here is close to our
earlier determination of 8.69 dex, and so the present results do
not significantly alleviate the solar modelling problem. Full
Table 2 is only available at the CDS via anonymous ftp to <A
href="http://cdsarc.u-strasbg.fr/">cdsarc.u-strasbg.fr</A>
(ftp://130.79.128.5) or via <A
href="http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/656/A113">http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/656/A113</A>

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Title: VizieR Online Data Catalog: The solar CNO abundances (Amarsi+,
2021)
Authors: Amarsi, A. M.; Grevesse, N.; Asplund, M.; Collet, R.
2021yCat..36560113A Altcode:
Table 2 contains the parameters, measured equivalent widths, and
abundances inferred from the different models, for the 408 lines used
in the present analysis. (1 data file).

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Title: The chemical make-up of the Sun: A 2020 vision
Authors: Asplund, M.; Amarsi, A. M.; Grevesse, N.
2021A&A...653A.141A Altcode: 2021arXiv210501661A
Context. The chemical composition of the Sun is a fundamental
yardstick in astronomy, relative to which essentially all cosmic
objects are referenced. As such, having accurate knowledge of the
solar elemental abundances is crucial for an extremely broad range
of topics. Aims: We reassess the solar abundances of all
83 long-lived elements, using highly realistic solar modelling and
state-of-the-art spectroscopic analysis techniques coupled with the
best available atomic data and observations. Methods: The
basis for our solar spectroscopic analysis is a three-dimensional
(3D) radiative-hydrodynamical model of the solar surface convection
and atmosphere, which reproduces the full arsenal of key observational
diagnostics. New complete and comprehensive 3D spectral line formation
calculations taking into account of departures from local thermodynamic
equilibrium (non-LTE) are presented for Na, Mg, K, Ca, and Fe using
comprehensive model atoms with reliable radiative and collisional
data. Our newly derived abundances for C, N, and O are based on a 3D
non-LTE analysis of permitted and forbidden atomic lines as well as
3D LTE calculations for a total of 879 molecular transitions of CH,
C2, CO, NH, CN, and OH. Previous 3D-based calculations for
another 50 elements are re-evaluated based on updated atomic data,
a stringent selection of lines, improved consideration of blends,
and new non-LTE calculations available in the literature. For elements
where spectroscopic determinations of the quiet Sun are not possible,
the recommended solar abundances are revisited based on complementary
methods, including helioseismology (He), solar wind data from the
Genesis sample return mission (noble gases), sunspot observations
(four elements), and measurements of the most primitive meteorites
(15 elements). Results: Our new improved analysis confirms
the relatively low solar abundances of C, N, and O obtained in
our previous 3D-based studies: log ϵC = 8.46 ± 0.04,
log ϵN = 7.83 ± 0.07, and log ϵO = 8.69 ±
0.04. Excellent agreement between all available atomic and molecular
indicators is achieved for C and O, but for N the atomic lines imply
a lower abundance than for the molecular transitions for unknown
reasons. The revised solar abundances for the other elements also
typically agree well with our previously recommended values, with only
Li, F, Ne, Mg, Cl, Kr, Rb, Rh, Ba, W, Ir, and Pb differing by more
than 0.05 dex. The here-advocated present-day photospheric metal mass
fraction is only slightly higher than our previous value, mainly due
to the revised Ne abundance from Genesis solar wind measurements:
Xsurface = 0.7438 ± 0.0054, Ysurface =
0.2423 ± 0.0054, Zsurface = 0.0139 ± 0.0006, and
Zsurface/Xsurface = 0.0187 ± 0.0009. Overall,
the solar abundances agree well with those of CI chondritic meteorites,
but we identify a correlation with condensation temperature such that
moderately volatile elements are enhanced by ≈0.04 dex in the CI
chondrites and refractory elements possibly depleted by ≈0.02 dex,
conflicting with conventional wisdom of the past half-century. Instead,
the solar chemical composition more closely resembles that of the
fine-grained matrix of CM chondrites with the expected exception of the
highly volatile elements. Conclusions: Updated present-day solar
photospheric and proto-solar abundances are presented for 83 elements,
including for all long-lived isotopes. The so-called solar modelling
problem - a persistent discrepancy between helioseismology and solar
interior models constructed with a low solar metallicity similar to
that advocated here - remains intact with our revised solar abundances,
suggesting shortcomings with the computed opacities and/or treatment of
mixing below the convection zone in existing standard solar models. The
uncovered trend between the solar and CI chondritic abundances with
condensation temperature is not yet understood but is likely imprinted
by planet formation, especially since a similar trend of opposite sign
is observed between the Sun and solar twins.

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Title: The 3D non-LTE solar nitrogen abundance from atomic lines
Authors: Amarsi, A. M.; Grevesse, N.; Grumer, J.; Asplund, M.; Barklem,
P. S.; Collet, R.
2020A&A...636A.120A Altcode: 2020arXiv200312561A
Nitrogen is an important element in various fields of stellar and
Galactic astronomy, and the solar nitrogen abundance is crucial as a
yardstick for comparing different objects in the cosmos. In order to
obtain a precise and accurate value for this abundance, we carried out
N I line formation calculations in a 3D radiative-hydrodynamic STAGGER
model solar atmosphere in full 3D non-local thermodynamic equilibrium
(non-LTE). We used a model atom that includes physically motivated
descriptions for the inelastic collisions of N I with free electrons and
with neutral hydrogen. We selected five N I lines of high excitation
energy to study in detail, based on their strengths and on their
being relatively free of blends. We found that these lines are slightly
strengthened from non-LTE photon losses and from 3D granulation effects,
resulting in negative abundance corrections of around - 0.01 dex and -
0.04 dex, respectively. Our advocated solar nitrogen abundance is log
ɛN = 7.77, with the systematic 1σ uncertainty estimated
to be 0.05 dex. This result is consistent with earlier studies after
correcting for differences in line selections and equivalent widths.

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Title: The Solar Chemical Composition: Past and Present
Authors: Grevesse, Nicolas
2019BSRSL..88....5G Altcode:
We briefly review the solar chemical composition derived last century
and the new, different solar chemical composition, obtained since
about 15 years.

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Title: 3D non-LTE line formation of neutral carbon in the Sun
Authors: Amarsi, A. M.; Barklem, P. S.; Collet, R.; Grevesse, N.;
Asplund, M.
2019A&A...624A.111A Altcode: 2019arXiv190308838A
Carbon abundances in late-type stars are important in a variety of
astrophysical contexts. However C I lines, one of the main abundance
diagnostics, are sensitive to departures from local thermodynamic
equilibrium (LTE). We present a model atom for non-LTE analyses of C
I lines, that uses a new, physically-motivated recipe for the rates
of neutral hydrogen impact excitation. We analyse C I lines in the
solar spectrum, employing a three-dimensional (3D) hydrodynamic
model solar atmosphere and 3D non-LTE radiative transfer. We find
negative non-LTE abundance corrections for C I lines in the solar
photosphere, in accordance with previous studies, reaching up to
around 0.1 dex in the disk-integrated flux. We also present the first
fully consistent 3D non-LTE solar carbon abundance determination:
we infer log ɛC = 8.44 ± 0.02, in good agreement with
the current standard value. Our models reproduce the observed solar
centre-to-limb variations of various C I lines, without any adjustments
to the rates of neutral hydrogen impact excitation, suggesting that
the proposed recipe may be a solution to the long-standing problem of
how to reliably model inelastic collisions with neutral hydrogen in
late-type stellar atmospheres.

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Title: Implications of solar wind measurements for solar models
and composition
Authors: Serenelli, Aldo; Scott, Pat; Villante, Francesco L.;
Vincent, Aaron C.; Asplund, Martin; Basu, Sarbani; Grevesse, Nicolas;
Peña-Garay, Carlos
2016MNRAS.463....2S Altcode: 2016arXiv160405318S; 2016MNRAS.tmp.1051S
We critically examine recent claims of a high solar metallicity by von
Steiger &amp; Zurbuchen (2016, vSZ16) based on in situ measurements
of the solar wind, rather than the standard spectroscopically inferred
abundances (Asplund et al. 2009, hereafter AGSS09). We test the claim
by Vagnozzi et al. (2016) that a composition based on the solar wind
enables one to construct a standard solar model in agreement with
helioseismological observations and thus solve the decades-old solar
modelling problem. We show that, although some helioseismological
observables are improved compared to models computed with spectroscopic
abundances, most are in fact worse. The high abundance of refractory
elements leads to an overproduction of neutrinos, with a predicted
8B flux that is nearly twice its observed value, and
7Be and CNO fluxes that are experimentally ruled out at high
confidence. A combined likelihood analysis shows that models using the
vSZ16 abundances are worse than AGSS09 despite a higher metallicity. We
also present astrophysical and spectroscopic arguments showing the vSZ16
composition to be an implausible representation of the solar interior,
identifying the first ionization potential effect in the outer solar
atmosphere and wind as the likely culprit.

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Title: Understanding the Internal Chemical Composition and Physical
Processes of the Solar Interior
Authors: Basu, Sarbani; Grevesse, Nicolas; Mathis, Stephane;
Turck-Chièze, Sylvaine
2015SSRv..196...49B Altcode: 2014SSRv..tmp....3B
The Sun, the closest and most well studied of stars, is generally used
as a standard that other stars are compared to. Models of the Sun are
constantly tested with helioseismic data. These data allow us to probe
the internal structure and dynamics of the Sun. Among the main sources
of the data is the SOHO spacecraft that has been continuously observing
the Sun for more than a solar cycle. Current solar models, although
good, do not include all the physical processes that are present in the
Sun. In this chapter we focus on specific inputs to solar models and
discuss generally neglected dynamical physical processes whose inclusion
could result in models that are much better representatives of the Sun.

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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&amp;A, 47, 481),
including full line lists and details of all input data that we have
employed. 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
ɛSc = 3.16 ± 0.04, log ɛTi = 4.93 ± 0.04,
log ɛV = 3.89 ± 0.08, log ɛCr = 5.62 ± 0.04,
log ɛMn = 5.42 ± 0.04, log ɛFe = 7.47 ± 0.04,
log ɛCo = 4.93 ± 0.05 and log ɛNi = 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. 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 ɛNa = 6.21 ± 0.04, log
ɛMg = 7.59 ± 0.04, log ɛAl = 6.43 ± 0.04,
log ɛSi = 7.51 ± 0.03, log ɛP = 5.41 ± 0.03,
log ɛS = 7.13 ± 0.03, log ɛK = 5.04 ± 0.05
and log ɛCa = 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. 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: Photospheric Constraints, Current Uncertainties in Models of
Stellar Atmospheres, and Spectroscopic Surveys
Authors: Plez, Bertrand; Grevesse, Nicolas
2015ASSP...39..183P Altcode: 2014arXiv1409.2282P
We summarize here the discussions around photospheric constraints,
current uncertainties in models of stellar atmospheres, and reports
on ongoing spectroscopic surveys. Rather than a panorama of the state
of the art, we chose to present a list of open questions that should
be investigated in order to improve future analyses.

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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: Why GN93 should not be used anymore
Authors: Grevesse, N.; Asplund, M.; Sauval, J.; Scott, P.
2013EPJWC..4301004G Altcode:
We show why the solar chemical composition of [1] (GN93) and the
similar values of [2] (AG89) and [3] (GS98), characterized by values
of the metallicity of the order of 0.017 to 0.020, largely used in
solar and stellar modeling, are now obsolete. They should be replaced
by the new and more precise results of [4] (AGSS09), with a much lower
metallicity of 0.0134.

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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: Chapter 1 : How to Derive Oxygen Abundances
Authors: Stasińska, G.; Prantzos, N.; Meynet, G.; Simón-Díaz,
S.; Chiappini, C.; Dessauges-Zavadsky, M.; Charbonnel, C.; Ludwig,
H. -G.; Mendoza, C.; Grevesse, N.; Arnould, M.; Barbuy, B.; Lebreton,
Y.; Decourchelle, A.; Hill, V.; Ferrando, P.; Hébrard, G.; Durret,
F.; Katsuma, M.; Zeippen, C. J.
2012EAS....54....3S Altcode:
No abstract at ADS

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Title: Chapter 2 : A Panorama of Oxygen in the Universe
Authors: Stasińska, G.; Prantzos, N.; Meynet, G.; Simón-Díaz,
S.; Chiappini, C.; Dessauges-Zavadsky, M.; Charbonnel, C.; Ludwig,
H. -G.; Mendoza, C.; Grevesse, N.; Arnould, M.; Barbuy, B.; Lebreton,
Y.; Decourchelle, A.; Hill, V.; Ferrando, P.; Hébrard, G.; Durret,
F.; Katsuma, M.; Zeippen, C. J.
2012EAS....54...65S Altcode:
No abstract at ADS

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Title: Oxygen in the Universe
Authors: Stasińska, G.; Prantzos, N.; Meynet, G.; Simón-Díaz,
S.; Chiappini, C.; Dessauges-Zavadsky, M.; Charbonnel, C.; Ludwig,
H. -G.; Mendoza, C.; Grevesse, N.; Arnould, M.; Barbuy, B.; Lebreton,
Y.; Decourchelle, A.; Hill, V.; Ferrando, P.; Hébrard, G.; Durret,
F.; Katsuma, M.; Zeippen, C. J.
2012EAS....54.....S Altcode:
No abstract at ADS

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Title: Foreword
Authors: Stasińska, G.; Prantzos, N.; Meynet, G.; Simón-Díaz,
S.; Chiappini, C.; Dessauges-Zavadsky, M.; Charbonnel, C.; Ludwig,
H. -G.; Mendoza, C.; Grevesse, N.; Arnould, M.; Barbuy, B.; Lebreton,
Y.; Decourchelle, A.; Hill, V.; Ferrando, P.; Hébrard, G.; Durret,
F.; Katsuma, M.; Zeippen, C. J.
2012EAS....54....1S Altcode:
No abstract at ADS

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Title: Appendix A : The atomic physics of oxygen
Authors: Stasińska, G.; Prantzos, N.; Meynet, G.; Simón-Díaz,
S.; Chiappini, C.; Dessauges-Zavadsky, M.; Charbonnel, C.; Ludwig,
H. -G.; Mendoza, C.; Grevesse, N.; Arnould, M.; Barbuy, B.; Lebreton,
Y.; Decourchelle, A.; Hill, V.; Ferrando, P.; Hébrard, G.; Durret,
F.; Katsuma, M.; Zeippen, C. J.
2012EAS....54..319S Altcode:
No abstract at ADS

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Title: Chapter 4 : The Evolution of Oxygen in Galaxies
Authors: Stasińska, G.; Prantzos, N.; Meynet, G.; Simón-Díaz,
S.; Chiappini, C.; Dessauges-Zavadsky, M.; Charbonnel, C.; Ludwig,
H. -G.; Mendoza, C.; Grevesse, N.; Arnould, M.; Barbuy, B.; Lebreton,
Y.; Decourchelle, A.; Hill, V.; Ferrando, P.; Hébrard, G.; Durret,
F.; Katsuma, M.; Zeippen, C. J.
2012EAS....54..255S Altcode:
No abstract at ADS

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Title: Chapter 3 : Oxygen Production and Destruction
Authors: Stasińska, G.; Prantzos, N.; Meynet, G.; Simón-Díaz,
S.; Chiappini, C.; Dessauges-Zavadsky, M.; Charbonnel, C.; Ludwig,
H. -G.; Mendoza, C.; Grevesse, N.; Arnould, M.; Barbuy, B.; Lebreton,
Y.; Decourchelle, A.; Hill, V.; Ferrando, P.; Hébrard, G.; Durret,
F.; Katsuma, M.; Zeippen, C. J.
2012EAS....54..187S 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.
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), ARu = 1.72 +/- 0.10, is in agreement
with the most recent meteoritic result, ARu = 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: The solar abundance of Oxygen
Authors: Grevesse, N.
2009CoAst.158..151G Altcode:
With Martin Asplund (Max Planck Institute of Astrophysics, Garching) and Jacques Sauval (Observatoire Royal de Belgique,
Brussels) I recently published detailed reviews on the solar
chemical composition ({Asplund et al. 2005}, {Grevesse et
al. 2007}). A new one, with Pat Scott (Stockholm University) as
additional co-author, will appear in Annual Review of Astronomy and
Astrophysics ({Asplund et al. 2009}). Here we briefly analyze
recent works on the solar abundance of Oxygen and recommend a value
of 8.70 in the usual astronomical scale.

---------------------------------------------------------
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 epsilonNi = 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 epsilonO
= 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 epsilonO
= 8.7.

---------------------------------------------------------
Title: The solar chemical composition
Authors: Grevesse, N.
2008CoAst.157..156G Altcode:
We give a brief review on the solar abundances emphasizing ”hot
topics” like the abundances of oxygen and neon.

---------------------------------------------------------
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.

---------------------------------------------------------
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.

---------------------------------------------------------
Title: The solar chemical composition
Authors: Asplund, Martin; Grevesse, Nicolas; Jacques Sauval, A.
2006NuPhA.777....1A Altcode: 2004astro.ph.10214A
We present what we believe to be the best estimates of the chemical
compositions of the solar photosphere and the most pristine meteorites.

---------------------------------------------------------
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
12C16O, 13C16O and
12C18O lines from the fundamental (Δ v =
1) and first overtone (Δ v = 2) bands to determine the solar
carbon abundance, as well as the 12C/13C
and 16O/18O 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
12C/13C and 16O/18O ratios
were measured as 86.8+3.9-3.7 (δ13C
= 30+46-44) and 479+29-28
(δ18O = 41+67-59), 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.

---------------------------------------------------------
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).

---------------------------------------------------------
Title: The new solar abundances - Part II: the crisis and possible
solutions
Authors: Montalban, J.; Miglio, A.; Theado, S.; Noels, A.; Grevesse, N.
2006CoAst.147...80M Altcode:
Recent 3D, NLTE analysis of the solar spectrum (Asplund et al. 2006,
Part I; Asplund et al. 2005) have led to a significant reduction of the
CNO and Ne abundances leading to a (Z/X) 30% smaller than the previously
recommended value. The corresponding decrease in opacity increases
dramatically the discrepancies between the sound-speed derived from
helioseismology and our new standard solar models (SSM). We present in
this paper some numerical experiments trying to reduce this discrepancy.

---------------------------------------------------------
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.

---------------------------------------------------------
Title: Introduction --- Historical Remarks: A view of David Lambert's
career
Authors: Grevesse, N.
2005ASPC..336....1G Altcode:
We attempt to cover David Lambert's career, stressing his most prominent
achievements, certainly biased by personal views.

---------------------------------------------------------
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.

---------------------------------------------------------
Title: Line formation in solar granulation. VI. [C I], C I, CH and
C2 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 C2
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, C2 Swan)
is log ɛC = 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.

---------------------------------------------------------
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.

---------------------------------------------------------
Title: Solar Model with CNO Revised Abundances
Authors: Montalbán, J.; Miglio, A.; Noels, A.; Grevesse, N.; di Mauro,
M. P.
2004ESASP.559..574M Altcode: 2004soho...14..574M; 2004astro.ph..8055M
Recent three-dimensional, NLTE analyses of the solar spectrum have shown
a significant reduction in the C, N, O and Ne abundances leading to a
Z/X ratio of the order of 0.0177. We have computed solar models with
this new mixture in the OPAL opacity tables. The present He abundance we
find seems rather consistent with the helioseismic value. However, the
convective envelope is too shallow, and diffusion, even if it reduces
the discrepancy, is not able to give the current value. We present some
numerical experiments consisting in changing the diffusion velocities
and/or the value of opacity at the base of the convective envelope.

---------------------------------------------------------
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 ɛO = 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.

---------------------------------------------------------
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: 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: Commission 14: Atomic and Molecular Data: (Donnees Atomiques
et Moleculaires)
Authors: Rostas, F.; Smith, P. L.; Berrington, K. A.; Feautrier, N.;
Grevesse, N.; Johansson, S.; Jørgensen, U. G.; Martin, W. C.; Mason,
H.; Parkinson, W.; Tchang-Brillet, W. -Ü. L.
2000IAUTA..24..380R 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, AFe=7.50+/-0.05,
which perfectly agrees with the meteoritic value. (1 data file).

---------------------------------------------------------
Title: I. Cherchneff and T. J. Millar (eds.), Dust and Molecules in
Evolved Stars
Authors: Grevesse, Nicolas
1999SSRv...88..606G Altcode:
No abstract at ADS

---------------------------------------------------------
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: Le soleil, une étoile, notre étoile.
Authors: Grevesse, N.
1997Ciel...59..265G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Book reviews
Authors: Marx, G.; Jaffe, W.; Maltby, P.; Grevesse, N.; Wu, S. T.;
Lüst, R.; Kleczek, J.; Chupp, E. L.; Bloemen, Hans; de Jager,
Cornelis; van Teeseling, A.; Shea, M. A.; Butcher, H.; van der Kruit,
P. C.; Nieuwenhuijzen, H.; Steeghs, Danny; Fälthammar, Carl-Günne;
Greenberg, J. M.; Rasool, S. I.
1996SSRv...77..369M 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; Jmax″= 48.5), as well as to the (1-0), (2-1),
and (3-2) vibration-rotation bands (Jmax″= 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 X2Π 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: 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: Convection Treatment in Solar Type Stars
Authors: Neuforge, C.; Fernandes, J.; Noels, A.; Grevesse, N.;
Baglin, A.
1995LIACo..32..207N Altcode: 1995sews.book..207N
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: Stellar evolution: what should be done
Authors: Noels, A.; Fraipont-Caro, D.; Gabriel, M.; Grevesse, N.;
Demarque, P.
1995sews.book.....N Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Solar abundances, convection and the standard solar model
Authors: Noels, A.; Grevesse, N.; Mazzitelli, I.
1995LNP...458..203N Altcode:
A new observed Z/X ratio is proposed for the Sun. We apply it to
recalibrating the Sun with two different convection theories, the
classical MLT and the recent theory of Canuto and Mazzitelli.

---------------------------------------------------------
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: Book reviews
Authors: Murawski, K.; Grevesse, N.; Piteri, S.; Nieuwenhuyzen, H.;
van der Hage, J. C. H.; Icke, Vincent; Hovenier, J. W.; Rutten, R. J.;
De Greve, J. P.; Kaufmann, P.; Burki, G.; de Jager, Cornelis
1993SSRv...65..365M Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Ti-ii transition probabilities and radiative lifetimes in TI
and the solar titanium abundance
Authors: Bizzarri, A.; Huber, M. C. E.; Noels, A.; Grevesse, N.;
Bergeson, S. D.; Tsekeris, P.; Lawler, J. E.
1993A&A...273..707B Altcode:
Transition probabilities of 100 Ti-II emission lines, originating
from 7 different atomic levels, have been determined by combining
branching fractions with radiative lifetimes. The branching fractions
were measured using Fourier transform spectroscopy on a hollow
cathode. The radiative lifetimes of these 7 - and 35 additional -
levels were measured using time resolved laser-induced fluorescence
on a slow Ti ion beam. The transition probabilities of 21 very
weak lines have been used to derive a solar titanium abundance of
αTi = log(NTi/NH) + 12=5.04±0.04 dex,
which is insensitive to the solar model. This value is in disagreement
with the meteoritic titanium abundance (4.93±0.02).

---------------------------------------------------------
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, ADy = 1.14±0.08,
is in pretty good agreement with the meteoritic value.

---------------------------------------------------------
Title: Atomic data and the spectrum of the solar photosphere.
Authors: Grevesse, N.; Noels, A.
1993PhST...47..133G Altcode:
Even though the solar photospheric abundances are now on the whole
in very good agreement with the meteoritic values, some problems
remain which will only be solved with a higher level of accuracy in
the atomic data, especially the transition probabilities for faint
lines. The authors justify this request for many more very accurate
gf-values through a few particularly striking points.

---------------------------------------------------------
Title: Book-Review - Accuracy of Element Abundances from Stellar
Atmospheres
Authors: Wehrse, R.; Grevesse, N.
1993SSRv...65..365W Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Cosmic abundances of the elements.
Authors: Grevesse, N.; Noels, A.
1993oee..conf...15G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: La composition chimique du Soleil.
Authors: Grevesse, N.; Noels, A.
1993pavc.conf..205G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Small and intermediate mass stellar evolution - main sequence
and close to it.
Authors: Noels, A.; Grevesse, N.
1993ASPC...40..410N Altcode: 1993ist..proc..410N; 1993IAUCo.137..410N
The authors present the standard models for small and intermediate
main sequence stars and discuss some of the problems arising with
semiconvection and overshooting. The surface abundance of Li serves
as a test for other physical mechanisms, including microscopic and
turbulent diffusion, rotation and mass loss.

---------------------------------------------------------
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: Lifetimes in Fe II and the solar abundance of iron
Authors: Hannaford, P.; Lowe, R. M.; Grevesse, N.; Noels, A.
1992A&A...259..301H Altcode:
New atomic lifetimes have been determined for eight quartet (z 4D, z
4F) levels and ten sextet (z 6D, z 6F, z 6P) levels in Fe II and the
results for seven of these levels have been combined with existing
experimental branching fractions to obtain a revised set of log
gf-values for 15 solar lines in Fe II. The new log gf data are used
together with equivalent widths determined from the Liege solar atlas
to derive a value for the iron photospheric abundance: 7.48 +/- 0.04,
which is consistent with the currently accepted meteoritic result, 7.51
+/- 0.01. The results are compared with the atomic lifetime data, log
gf data and solar analyses used in three other recent solar abundance
determinations based on Fe II lines.

---------------------------------------------------------
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: Updating Solar Abundances
Authors: Grevesse, N.
1992eatc.conf...49G Altcode:
No abstract at ADS

---------------------------------------------------------
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
12C16O have been measured up to J = 133, those
of 13C16O and of 12C18O
up to J = 103 and 91, respectively. The first overtone bands of
12C16O 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 Uij. The present set of
coefficients reproduces all accurate laboratory positions and our solar
measurements of high rotational excitation with a standard deviation
of about 10-5 cm-1 (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. 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: Calibration of the alpha Centauri system : metallicity and age.
Authors: Noels, A.; Grevesse, N.; Magain, P.; Neuforge, C.; Baglin,
A.; Lebreton, Y.
1991A&A...247...91N Altcode:
The binary system Alpha Cen A and B, with its well known parallax,
its high quality orbit and the reasonable hypothesis of a common
origin and age for both components, is a useful test of stellar
evolution models. Evolutionary sequences are computed for 1.085
and 0.9 solar masses with different values of Z, Y and alpha (=
l/Hp). Adopting luminosities and effective temperatures as derived from
the observations, Z = 0.04, Y = 0.32, alpha = 1.6 and t = 5 Gyr. The
Z-value derived from evolutionary sequences is very sensitive to the
difference in effective temperature between the two components.

---------------------------------------------------------
Title: Atomic data and solar photospheric spectroscopy.
Authors: Grevesse, N.
1991JPhy4...1..181G Altcode:
This review is an updated version of an earlier one. The author insists
on the role atomic data and their accuracy play in the interpretation
of the solar photospheric spectrum, leading to a better knowledge
of the physical conditions, physical processes and abundances of the
elements in the solar outer layers.

---------------------------------------------------------
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: Solar element abundances.
Authors: Grevesse, Nicolas; Anders, Edward
1991sia..book.1227G Altcode:
The elemental abundances of the sun are derivable from spectroscopic
studies of the photosphere, sunspots, chromosphere and corona, as well
as from solar-wind and solar energetic particle measurements and the
gamma-ray spectroscopy of solar flares. It is presently noted that
photospheric results yield the most accurate and reliable set of solar
abundances due to the exceptional quality of the photospheric spectra;
in addition, the physical conditions and processes in question are
more fully understood than elsewhere in the sun.

---------------------------------------------------------
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: Solar Abundances: the Reference System
Authors: Grevesse, N.
1991IAUS..145...63G Altcode:
No abstract at ADS

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

---------------------------------------------------------
Title: The abundance of cadmium in the solar photosphere
Authors: Youssef, N. H.; Doenszelmann, A.; Grevesse, N.
1990A&A...239..367Y Altcode:
The transition probability of the only good indicator of the solar
abundance of cadmium, the Cd I line at 5085.823 A, has very recently
been measured with high accuracy. A new value of the solar abundance
of Cd is derived from a careful analysis of this line and it is found
that A(cd) = 1.77 + or - 0.11, in agreement with the meteoritic value.

---------------------------------------------------------
Title: Contamination of the Th II line and the age of the Galaxy
Authors: Lawler, J. E.; Whaling, W.; Grevesse, N.
1990Natur.346..635L Altcode:
THE age of the Galaxy may be estimated from observations of the ratio
of stellar abundances of thorium, which has only one long-lived isotope
with a half-life comparable to the suspected age of the Galaxy, and
neodymium, a stable element. The Th/Nd abundance ratio in a sample
of G-dwarf stars of different ages was derived by Butcher1
from the intensities of one Th II and one Nd II absorption line, and
indicated a rather young galactic age of 9.6 Gyr. But the Th II line is
blended with a Co I line. Here we determine the transition probability
of the Co I line by combining radiative lifetime and branching-ratio
measurements. We show that the Co I contribution cannot be neglected
in deriving Th/Nd ratios. By comparing our results with predictions
based on models of galactic chemical evolution, we suggest a revised
age of the Galaxy of 15-20 Gyr.

---------------------------------------------------------
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: Fe II transition probabilities and the solar iron abundance
Authors: Pauls, U.; Grevesse, N.; Huber, M. C. E.
1990A&A...231..536P Altcode:
Branching fractions for three near-infrared Fe II lines are presented
that fulfill the requirements necessary for an accurate solar
abundance determination. The lines belong to the dominant ionization
stage and are weak enough to lie on the linear part of the curve of
growth. The resulting abundance is insensitive to deviations from
local thermodynamic equilibrium and is independent of assumptions
concerning the temperature model and line-broadening parameters. From
the transition probabilities and from accurate solar equivalent widths,
a solar photospheric iron abundance is obtained.

---------------------------------------------------------
Title: Lifetimes in Sm II and the solar abundance of samarium.
Authors: Biemont, E.; Grevesse, N.; Hannaford, P.; Lowe, R. M.
1989A&A...222..307B Altcode:
Radiative lifetimes for 35 levels of Sm II have been measured by
laser-induced fluorescence from sputtered metal vapor. Oscillator
strengths for a number of lines of solar interest have been determined
by combining the lifetime data with branching ratios taken mainly
from the NBS tables. The mean solar abundance of samarium deduced
from a sample of 26 lines is A(Sm) = 1.01 + or - 0.06, where A(Sm) =
log N(Sm)/N(H) with log N(H) = 12.00, in agreement with the meteoritic
value.

---------------------------------------------------------
Title: Solar-system abundances of the elements: A new table
Authors: Grevesse, Nicolas; Anders, Edward
1989AIPC..183....1G Altcode: 1989cam..conf....1G
We present an abridged version of a new abundance compilation (Anders
and Grevesse, 1988), representing an update of Anders and Ebihara
(1982) and Grevesse (1984). It includes revised meteoritic abundances
as well as photospheric and coronal abundances, based on literature
through mid-1988.

---------------------------------------------------------
Title: The abundances of matter in the sun
Authors: Grevesse, Nicolas
1989AIPC..183....9G Altcode: 1989cam..conf....9G
We present a review of the abundances as derived from the outer
solar layers essentially based on photospheric results. After briefly
discussing the present status of the solar, atomic and molecular data
used in abundance determinations, we present the best solar abundances
in a second paper (Grevesse and Anders, this volume).

---------------------------------------------------------
Title: Revision of the absolute scale of the Oxford TI I oscillator
strengths and the solar titanium abundance
Authors: Grevesse, N.; Blackwell, D. E.; Petford, A. D.
1989A&A...208..157G Altcode:
The Oxford relative oscillator strengths for Ti I (0.00eV-2.31eV),
previously placed on an absolute scale using data from the Bell
et al. (1975) atomic beam technique and lifetimes obtained by the
beam-foil technique, are placed on a more accurate, absolute scale
using the precise lifetime measurements of Rudolph and Helbig (1982)
obtained by selective pulsed laser excitation in an atomic beam. As
a consequence, it is proposed that all published Oxford oscillator
strengths for Ti I should be increased by 0.056 dex (14 percent). The
corresponding titanium solar abundance found from their use should be
decreased to log A = 4.99.

---------------------------------------------------------
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 X2Π ground state of CH.

---------------------------------------------------------
Title: Lifetimes and transition probabilities in V II and the solar
abundance of vanadium.
Authors: Biemont, E.; Grevesse, N.; Faires, L. M.; Marsden, G.;
Lawler, J. E.; Whaling, W.
1989A&A...209..391B Altcode:
The laser-induced fluorescence method is used to measure the radiative
lifetimes and emission branching fractions in six levels in V II. The
emission branching fractions were determined for an additional 17 V
II levels with known lifetimes. Also, 14 V II transition probabilities
were measured with an inductively coupled argon plasma spectral source
in which the level populations vary with level excitation energy in a
predictable way. The equivalent widths of V lines were measured and the
solar V abundance was calculated with the models of Holweger-Mueller
(1974) and Maltby et al. (1986). It is found that the mean solar V
abundance, base on V I and V II lines is 4.00 + or - 0.02.

---------------------------------------------------------
Title: Abundances of the elements: Meteoritic and solar
Authors: Anders, E.; Grevesse, N.
1989GeCoA..53..197A Altcode:
New abundance tables have been compiled for Cl chondrites and the
solar photosphere and corona, based on a critical review of the
literature to mid-1988. The meteorite data are generally accurate to
± 5-10%. Significant discrepancies between Sun and meteorites occur
only for Fe, Mn, Ge, Pb, and W; other well-determined elements agree
to ±9% on the average. There is no evidence for group fractionations
in Cl chondrites of cosmochemically similar elements (refractories,
siderophiles, volatiles, etc.), but a selective fractionation of Fe
cannot be ruled out. Abundances of odd- A nuclides between A = 65 and
209 show a generally smooth trend, with elemental abundances conforming
to the slope defined by isotopic abundances. Significant irregularities
occur in the NdSmEu region, however, suggesting that the abundance
curve is dependably smooth only down to the ∼20% level.

---------------------------------------------------------
Title: A Photospheric Solar Iron Abundance from Weak FeII Lines
Authors: Pauls, U.; Grevesse, N.; Huber, M. C. E.
1988IAUS..132..425P Altcode:
The high resolution and the high light-gathering power of a
Fourier-transform spectrometer afford the observation of very weak
lines in laboratory spectra. Thus it became possible to determine an
accurate solar iron abundance from Fe II lines that are weak in the
solar spectrum: the authors measured the branching fractions of a few
such lines whose upper levels lifetimes are known.

---------------------------------------------------------
Title: A photospheric solar iron abundance from weak Fe II lines
Authors: Pauls, U.; Huber, M. C. E.; Grevesse, N.
1988ASSL..138...79P Altcode: 1988IAUCo..94...79P; 1988pffl.proc...79P
The main difficulties encountered in determining a photospheric solar
iron abundance are considered and a way is shown to circumvent most
of them. Branching fractions of weak Fe II lines are measured from a
hollow-cathode discharge to derive accurate transition probabilities
from a previously determined lifetime. These transition probabilities -
together with accurate equivalent widths from the solar spectrum - are
subsequently used to calculate a photospheric iron abundance. The choice
of suitable lines results in an abundance value nearly independent of
any assumption concerning the temperature model and line-broadening
parameters.

---------------------------------------------------------
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: Hipparcos, le projet aux 100.000 étoiles.
Authors: Grevesse, N.; Malaise, D.
1986Ciel...48..397G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Absolute transition probabilities in vanadium I and the solar
abundance of vanadium
Authors: Whaling, W.; Hannaford, P.; Lowe, R. M.; Biemont, E.;
Grevesse, N.
1985A&A...153..109W Altcode:
The radiative lifetimes of 39 levels in V I have been measured
by the method of laser-induced fluorescence from sputtered metal
vapor. Emission branching ratios have been measured for these levels
to determine absolute transition probabilities for 208 lines in the
wavelength range 3180 Å to 16,400 Å. These transition probabilities
are used together with high quality solar spectra to derive an improved
solar abundance of vanadium, AV = 3.99±0.01. Hyperfine
structure effects were included in the abundance calculation.

---------------------------------------------------------
Title: Germanium and Lead: Significant Differences Between Meteoritic
and Photospheric Abundances?
Authors: Grevesse, N.; Meyer, J. P.
1985ICRC....3....5G Altcode: 1985ICRC...19c...5G
The order of the Galactic cosmic ray source (GCRS) composition in terms
of first ionization potential (FIP) was examined. For most elements,
the degree of volatility is (positively) correlated with the value of
the FIP, so that it is not easy to distinguish a correlation of GCRS
abundances anomalies with FIP from a correlation with volatility. Only
a few permit to distinguish between the two kinds of ordering: if
they are depleted relative to refractory metals, volatility must be
relevant, if not, FIP is relevant. Among them Cu and Zn would seem
to favor FIP. Among the best indicators are Ge and Pb. The abundance
anomalies in GCRS are defined relative to a standard which, for
the heavy elements concerned, is commonly taken as C1 Carbonaceous
Chondrites. Photospheric abundances are more directly representative
of the protosolar nebula, and hence of ordinary local galactic (LG)
matter. The Ge and Pb reference abundance determinations in the
Photosphere and in C1 meteorites are examined and their relevance to
the problem with FIP vs. volatility in GCRs is discussed.

---------------------------------------------------------
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-1). The role these lines could play in solar and stellar
spectroscopy is discussed.

---------------------------------------------------------
Title: Radiative lifetimes for Nb II and the problem of the solar
abundance of niobium
Authors: Hannaford, P.; Lowe, R. M.; Biemont, E.; Grevesse, N.
1985A&A...143..447H Altcode:
The radiative lifetimes of 27 levels in Nb II have been measured by the
method of laser-induced fluorescence from sputtered metal vapor. These
results have been combined with recent solar data to determine the solar
abundance of niobium. The result, A(Nb) = 1.42 + or - 0.06, which is
in good agreement with observations of meteorites, is by a factor of
5 lower than that recently derived from Nb I lines by Kwiatkowski et
al. (1982). Some possible explanations of the discrepancy are given.

---------------------------------------------------------
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.

---------------------------------------------------------
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.

---------------------------------------------------------
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.

---------------------------------------------------------
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).

---------------------------------------------------------
Title: Lifetimes, branching ratios, and transition probabilities in
Mo I
Authors: Whaling, W.; Hannaford, P.; Lowe, R. M.; Biemont, E.;
Grevesse, N.
1984JQSRT..32...69W Altcode:
The radiative lifetimes of 56 levels in Mo I have been measured
by the method of laser-induced fluorescence from sputtered metal
vapor. Emission branching ratios have been measured for these levels
to determine transition probabilities for 570 Mo I transitions in the
wavelength range 2944 - 9767 Å. The uncertainty in the transition
probability of stronger branches is typically less than 5%.

---------------------------------------------------------
Title: An improved solar abundance of osmium based on new lifetime
measurements in OS I
Authors: Kwiatkowski, M.; Zimmermann, P.; Biemont, E.; Grevesse, N.
1984A&A...135...59K Altcode:
A new solar abundance of osmium, AOs = 1.45±0.10, in
agreement with meteorites, is derived from 9 lines of Os I observed
in the photospheric spectrum. This result is based on new lifetime
measurements for 6 levels of Os I performed by time-resolved observation
of the reemitted fluorescence after pulsed laser excitation.

---------------------------------------------------------
Title: Lifetime measurements for RU I and the solar abundance of
ruthenium
Authors: Biemont, E.; Grevesse, N.; Kwiatkovski, M.; Zimmermann, P.
1984A&A...131..364B Altcode:
Reference is made to studies by Biemont et al. (1982) and Kwiatkowski
et al. (1982), in which 'modern' radiative lifetimes obtained by laser
excitation were used to refine and update solar abundance values. The
same procedure is extended here to Ru I. Radiative lifetimes are
measured by laser excitation for 12 levels of Ru I. The results
are combined with branching ratios taken from Corliss and Bozman
(1962) in order to provide an accurate set of oscillator strengths
for transitions of solar interest. From studying nine Ru I lines,
the photospheric abundance is found to be 1.84 + or - 0.07.

---------------------------------------------------------
Title: Abundance of the Elements in the Sun
Authors: Grevesse, N.
1984faa..conf...71G Altcode:
The different sources of abundances of the elements in the sun are
reviewed. The author summarizes the present solar abundances of all
the elements and compare these data with the meteoritic results.

---------------------------------------------------------
Title: Accurate atomic data and solar photospheric spectroscopy.
Authors: Grevesse, N.
1984PhST....8...49G Altcode: 1984PhyS....8...49G
This paper reviews the requests for high precision atomic data in
studies of the solar atmosphere. A table is presented summarizing
the presently accepted solar abundances and comparing these data with
meteoritic values.

---------------------------------------------------------
Title: Rythmes solaires et terrestres.
Authors: Grevesse, N.
1984Ciel...46..273G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A redetermination of the solar abundance of molybdenum
Authors: Biemont, E.; Grevesse, N.; Hannaford, P.; Lowe, R. M.;
Whaling, W.
1983ApJ...275..889B Altcode:
New accurate transition probabilities are used together with
high-quality solar spectra to derive an improved solar abundance of
molybdenum, AMO = 1.92±0.05.

---------------------------------------------------------
Title: Oscillator strengths for Y I and Y II and the solar abundance
of yttrium.
Authors: Hannaford, P.; Lowe, R. M.; Grevesse, N.; Biemont, E.;
Whaling, W.
1982ApJ...261..736H Altcode:
Oscillator strengths for 154 Y I lines and 66 Y II lines with
wavelengths between 2948 and 7055 A are determined by combining
laboratory measurements of radiative lifetimes and branching
ratios. Lifetimes are presented for 34 levels of Y I and 14 levels
of Y II; branching ratios are given for all levels below 9000 A
with parity change and delta J equals plus or minus 1, 0. Together
with equivalent widths measured on a photometric atlas of the solar
photospheric spectrum for eight Y I lines and 41 Y II lines with
laboratory wavelenths between 2467 and 7882 A, the data are used
to determine the solar abundance of yttrium. Mean logarithmic solar
abundances of 2.18 plus or minus 0.12 for Y I and 2.25 plus or minus
0.03 for Y II are deduced, and an yttrium abundance of 2.24 plus
or minus 0.03 is derived. It is noted that the data presented have
important implications for the yttrium abundances in both cool and
hot stars, particularly in chemically peculiar stars.

---------------------------------------------------------
Title: New lifetime measurements for Nb I and Rh I and the solar
photospheric abundances of Nb and Rh.
Authors: Kwiatkowski, M.; Zimmermann, P.; Biemont, E.; Grevesse, N.
1982A&A...112..337K Altcode:
New lifetime measurements for 11 levels in Nb I and 13 levels in Rh
I have been performed by time-resolved observation of the reemitted
fluorescence after pulsed laser excitation. New f-values have been
deduced and used in order to redetermine the photospheric abundances
of niobium and rhodium. The result for Rh, ARh equals 1.12
plus or minus 0.12, is in excellent agreement with the meteoritic value,
but the result for Nb, ANb equals 2.10 plus or minus 0.10,
is about four times larger than the meteoritic abundance.

---------------------------------------------------------
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 C2 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:
f00 = 1.41 10-3, f10 = 1.38
10-3, and f01 = 1.12 10-3. These
solar f-values are discussed in section 3.1 and compared with recent
laboratory data. For the Ballik-Ramsay system, only a few
unblended solar lines have been available, from which we deduced 0.6
10-3 ≪ f00 ≪ 1.2 10-3.

---------------------------------------------------------
Title: Radiative lifetimes for Pd I and the solar abundance of
palladium
Authors: Biemont, E.; Grevesse, N.; Kwiatkowski, M.; Zimmermann, P.
1982A&A...108..127B Altcode:
New lifetime measurements obtained using laser excitation are reported
for levels in the 4d95p configuration of Pd I. These
results are combined with branching ratios taken from Corliss and
Bozman (1962) in order to provide a new set of oscillator strengths
for eight transitions of solar interest. The photo spheric abundance
deduced from the study of these lines is APd =1.69±0.04.

---------------------------------------------------------
Title: Oscillator strengths for Zr I and Zr II and a new determination
of the solar abundance of zirconium.
Authors: Biemont, E.; Grevesse, N.; Hannaford, P.; Lowe, R. M.
1981ApJ...248..867B Altcode:
A new determination of the solar abundance of zirconium has been made
using equivalent-width data measured on the Jungfraujoch solar atlas
together with new oscillator strengths derived from measurements of
atomic lifetimes and branching ratios for 34 lines of Zr I and 24 lines
of Zr II. Excellent agreement is found between the results derived
from Zr I and Zr II lines and also with recent meteoritic results. The
mean abundance of zirconium in the sun is found to be A/Zr/ equals
2.56 plus or minus 0.05.

---------------------------------------------------------
Title: La photosphère: Modèles de la photosphére
Authors: Grevesse, N.
1981C&T....97R.111G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: La composition chimique du Soleil: Abondances (photosphère,
taches solaires, chromosphère, couronne, vent solaire, rayons
cosmiques solaires)
Authors: Grevesse, N.
1981C&T....97Q.193G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: La composition chimique du Soleil: Pourquoi déterminer la
composition chimique du Soleil?
Authors: Grevesse, N.
1981C&T....97S.193G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: La photosphére: Champ magnétique
Authors: Grevesse, N.
1981C&T....97V.111G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: La composition chimique du Soleil: Abondances isotopiques
Authors: Grevesse, N.
1981C&T....97R.193G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: La composition chimique du soleil.
Authors: Grevesse, N.
1981C&T....97..217G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: La photosphére: Oscillations solaires
Authors: Grevesse, N.
1981C&T....97T.111G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: La photosphère: Spectre
Authors: Grevesse, N.
1981C&T....97Q.111G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: New transition probabilities for Y II and Zr II and the
Sr-Y-Zr abundance patterns in CP stars
Authors: Grevesse, N.; Biemont, E.; Lowe, R. M.; Hannaford, P.
1981LIACo..23..211G Altcode: 1981cpsu.conf..211G
Problems related to the oscillator strengths in Sr II, Y II, and Zr II
are discussed, and new accurate transition probabilities are reported
that are derived from measurements of lifetimes and branching ratios of
Y II and Zr II lines present in the spectra of chemically peculiar stars
of the upper main sequence. These oscillator strengths are compared
with other sets of gf-values often used to determine abundances in CP
stars. The data are then applied to a normalization of a large number
of published abundance results concerning CP stars of different types.

---------------------------------------------------------
Title: La photosphère: Caractéristiques générales
Authors: Grevesse, N.
1981C&T....97S.111G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: La photosphére: Granulation
Authors: Grevesse, N.
1981C&T....97U.111G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: A solar abundance of nickel independent of line broadening
parameters
Authors: Biemont, E.; Grevesse, N.; Huber, M. C. E.; Sandeman, R. J.
1980A&A....87..242B Altcode:
The solar abundance of nickel is determined on the basis of two
recent sets of accurate f values independent of line broadening
parameters. Solar equivalent widths of 12 very weak neutral nickel lines
between 3946.200 and 7062.978 A for which accurate oscillator strengths
were available were measured on spectra of the center of the solar disk,
and solar profiles were computed by the direct integration of profiles
using two different empirical solar models in the LTE hypothesis. A
photospheric nickel abundance of 6.22 plus or minus 0.13 is obtained,
in reasonable agreement with coronal values and in excellent agreement
with the abundance of Ni in chondritic meteorites.

---------------------------------------------------------
Title: A solar abundance of nickel independent of line broadening
parameters.
Authors: Biémont, E.; Grevesse, N.; Huber, M. C. E.; Sandeman, R. J.
1980A&A....84..242B Altcode:
No abstract at ADS

---------------------------------------------------------
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

---------------------------------------------------------
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

---------------------------------------------------------
Title: Beam-foil lifetime measurements in Fe v and Fe vi
Authors: Dumont, P. D.; Baudinet-Robinet, Y.; Garnir, H. P.; Biemont,
E.; Grevesse, N.
1979PhRvA..20.1347D Altcode:
The authors have recorded beam-foil spectra of Fe v and Fe vi between
1100 and 1900 Å at ion energies ranging from 0.4 to 1.5 MeV. For the
first time, lifetimes have been measured for thirteen 3d34p
levels in Fe v and six 3d24p levels in Fe vi. These lifetime
results are not in agreement with the available theoretical values
deduced from the transition probabilities calculated by Abbott.

---------------------------------------------------------
Title: Solar abundance of praseodymium
Authors: Biemont, E.; Grevesse, N.; Hauge, O.
1979SoPh...61...17B Altcode: 1978SoPh...61...17B
16 lines of Pr II possibly present in the solar photospheric spectrum
have been studied. When including hyperfine structure in synthetic
calculations, investigations of 9 lines result in an abundance
APr = 0.71 ± 0.08 in the log AH = 12.00 scale.

---------------------------------------------------------
Title: Il y a 50 ans, contribution fondamentale de H. N. Russell à
la composition de l'atmosphère solaire
Authors: Grevesse, N.
1979C&T....95..389G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The elements and their isotopes in the universe; International
Conference on Astrophysics, 22nd, Liege, Belgium, June 20-22,
1978, Reports
Authors: Boury, A.; Grevesse, N.; Remy-Battiau, L.
1979LIACo..22.....B Altcode: 1979eisu.conf......
The Conference focused on nuclear astrophysics, abundances of elements
in the sun, carbonaceous chondrite abundances, isotopic heterogeneities
in the solar system, abundances in unevolved cool stars, and changes in
stellar abundances due to nonnuclear mechanisms. Papers were presented
on galactic importance of Li-7 production in nova explosions, Al-26
production in explosive burning of hydrogen-helium layers, abundance
determination in the solar chromosphere obtained from eclipse data,
the elemental and isotopic abundances of H, C, N, Na, and O in comets,
non-LTE analysis of sd O-stars, chemical composition of stars in
globular clusters, high dispersion studies of CP stars, and the argon
abundance in the solar neighborhood.

---------------------------------------------------------
Title: On the chromium abundance in the solar photosphere.
Authors: Biemont, E.; Grevesse, N.; Huber, M. C. E.
1978A&A....67...87B Altcode:
Summary. The solar abundance of chromium is inferred from high-quality
photospheric spectra with the aid of several recent sets of experimental
and theoretical oscillator strengths for Cr 1. The mean abundance,
Acr = log (Ncr/N ) + 12 = 5.64, obtained with an LTEanalysis, agrees
with the meteoritic value. The uncertainty of Acr stemming from the
oscillator strengths is +0.03 dex only; an additional uncertainty of
the order of +0.1 dex may, however, have to be assigned to the solar
model calculations that yield the abundance. Key words: chromium
abundance - gf-values.

---------------------------------------------------------
Title: Book reviews
Authors: Plavec, Miroslav; Hoekstra, R.; de Jager, C.; Grygar, Jiři;
Otterman, J.; van den Dool, H. M.; Namba, O.; Gunsing, C. J. Th.;
Pecker, Jean-Claude; Kwee, K. K.; Perek, L.; Callebaut, D.; Kuijpers,
Jan; de Graaff, W.; Reijnen, G. C. M.; Swanenburg, B.; Grevesse,
N.; Kleczek, J.; Piquet, P.; Fokker, A. D.; van Bueren, H. G.; Page,
D. Edgar; van Duinen, R. J.; Pacini, Franco
1978SSRv...21..469P Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Book reviews
Authors: Reijnen, G. C. M.; Ness, Norman F.; Kliore, Arvydas J.;
Sonnenschein, F. J.; Hoogenboom, A. M.; Hack, Margherita; Johnson,
F. S.; Reijnen, G. C. M.; Kleczek, J.; van Bueren, H. G.; de Graaff,
W.; Hoyng, P.; Swider, W.; Grevesse, N.
1977SSRv...20..677R Altcode:
No abstract at ADS

---------------------------------------------------------
Title: f-values and abundances of the elements in the sun and stars.
Authors: Biemont, E.; Grevesse, N.
1977PhyS...16...39B Altcode:
The article reviews the atomic and molecular f-values currently needed
to determine solar abundances. The abundances of chemical elements in
stellar objects are discussed along with a photospheric model, local
thermodynamic equilibrium, line opacity, and spectrum synthesis. The
oscillator strengths required for small astrophysical models are
described, and various problems encountered in stellar spectroscopy
are outlined.

---------------------------------------------------------
Title: Spectroscopic studies of Si V and Si VI between 500 and 1300
Å using the beam-foil method.
Authors: Garnir, H. P.; Livingston, A. E.; Baudinet-Robinet, Y.;
Dumont, P. D.; Biemont, E.; Grevesse, N.
1977JOSA...67..751G Altcode: 1977OSAJ...67..751G
No abstract at ADS

---------------------------------------------------------
Title: Radiative-Lifetime Measurements for Sulfur and Silicon
Transitions Observed in Interstellar Absorption Spectra" erratum, 199
Authors: Livingston, A. E.; Garnir, H.; Baudinet-Robinet, Y.; Dumont,
P. D.; Biemont, E.; Grevesse, N.
1976ApL....17...23L Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Erratum: "Radiative-lifetime measurements for sulfur and
silicon transitions observed in interstellar absorption spectra"
[Astrophys. Lett., Vol. 17, p. 23 - 25 (1976)].
Authors: Livingston, A. E.; Garnir, H.; Baudinet-Robinet, Y.; Dumont,
P. D.; Biémont, E.; Grevesse, N.
1976ApL....17..199L Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Solar Photospheric Abundance of Iron
Authors: Biemont, E.; Grevesse, N.
1975SoPh...45...59B Altcode:
A new value of the solar photospheric abundance of iron, independent
of line-shape parameters, is derived. Our analysis is based on a
study of 40 weak infrared lines (0.85&lt;λ&lt;2.5 μ) for which
theoretical oscillator strengths (calculated with configuration
interactions taken into account) have recently been computed by Kurucz
(1974). The abundance obtained, AFe = 7.57±0.11 (in the
usual scale where log NH = 12.00) is in agreement with the
`high' solar values recently reported in the literature and with the
meteoritic abundance.

---------------------------------------------------------
Title: Lifetimes and transition probabilities in NV.
Authors: Baudinet-Robinet, Y.; Dumont, P. D.; Biemont, E.; Grevesse, N.
1975PhyS...11..371B Altcode:
Lifetimes of excited levels in N V have been measured by the beam-foil
technique using lines in the ultraviolet spectral range. Transition
probabilities are deduced from these results using branching ratios
computed in the Coulomb approximation.

---------------------------------------------------------
Title: Transition probabilities for vacuum ultraviolet lines of N
I through N IV.
Authors: Dumont, P. D.; Biemont, E.; Grevesse, N.
1974JQSRT..14.1127D Altcode:
No abstract at ADS

---------------------------------------------------------
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

---------------------------------------------------------
Title: Atomic Wavelengths and Transition Probabilities in the Infrared
Authors: Biemont, E.; Grevesse, N.
1973A&A....27..163B Altcode:
Summary. Infrared wavelengths (1 &lt; &lt;25 and oscillator strengths,
based on the Coulomb approximation, have been calculated for a large
number of permitted lines of the following elements: Li 1, Be I and Be
ii, Bi, Ci, Ni, Oi, Nai, Mgi and Mgii, Ali and Al ii, Sii and Si ii,
Pi and Pii, Si, Ki, Cai and Ca ii. Key words: wavelengths - transition
probabilities - infrared

---------------------------------------------------------
Title: Infrared Wavelengths and Transition Probabilities for Atoms,
3 &amp;le Z &lt;= 20
Authors: Biemont, E.; Grevesse, N.
1973ADNDT..12..217B Altcode:
Infrared wavelengths (1μ &lt; λ &lt; 25μ) and oscillator strengths
based on the Coulomb approximation, have been calculated for a large
number of permitted lines of the following spectra:

---------------------------------------------------------
Title: The Solar Abundance of Silicon from Forbidden Lines of SI I
Authors: Grevesse, N.; Swings, J. P.
1972ApJ...171..179G Altcode:
The low-excitation (E.P. = 0.78 eV) [Si I] line at 10,991.41 A is
blended by a telluric water-vapor line when observed at the center of
the solar disk, but can be detected on Doppler-shifted spectra obtained
at the west limb of the Sun. A description of our observations at =
cos 0 = 1.0 and at = 0.2, 0.13, and 0.11 is given. The intensity of
the line detected near the limb, which we attribute to [Si I], leads
to a solar silicon abundance in agreement with the value deduced
from higher-excitation permitted lines (E.P. &gt; S eV) and from
extreme-ultraviolet coronal lines, i.e., log Ns = 7.5 (if log NH =
12.00). Future observations of infrared [Si i] lines on the disk and
in sunspots are envisaged.

---------------------------------------------------------
Title: Raies atomiques dans l'infrarouge, longueurs d'onde,
probabilités de transition et identifications dans le spectre
solaire.
Authors: Biémont, E.; Grevesse, N.
1972BSRSL..42..307B Altcode:
No abstract at ADS

---------------------------------------------------------
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

---------------------------------------------------------
Title: Forbidden Fe i Lines in Sunspots
Authors: Grevesse, N.; Swings, J. P.
1971A&A....13..329G Altcode:
In a recent paper, Grevesse et al. (1971) have identified [Fe I]
lines in sunspot spectra. This was shown to be in agreement with the
high value of the solar iron abundance: log NFv = 7.5. We report here
the identification of another [Fe I] line, 5696.36 A, in sunspot
spectra. This represents an additional argument in favour of the
high value of the iron abundance in the sun. Key words: sunspot -
iron abundance - forbidden lines

---------------------------------------------------------
Title: The Solar Abundance of Silicon from Forbidden Si I Lines.
Authors: Grevesse, N.; Swings, J. P.
1971BAAS....3..377G Altcode:
No abstract at ADS

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

---------------------------------------------------------
Title: [Fe i) lines: Their transition probabilities and occurrences
in sunspots
Authors: Grevesse, N.; Nussbaumer, H.; Swings, J. P.
1971MNRAS.151..239G Altcode:
Magnetic dipole and electric quadrupole transition probabilities have
been calculated for all the transitions in the configurations 3d74s and
3d64s2 of Fe I. Configuration interaction has been included. A search
with the Kitt Peak solar telescope has been made in sunspots for the
lines corresponding to the strongest predicted transitions. Lines of
the multiplets a5D-a3P, a5D-b3F, and a5D-a5P have been tentatively
identified. Their equivalent widths confirm the high solar iron
abundance: log NFe = 7.5. The possible presence of [Fe i] lines in
the absorption spectrum of Arcturus is also discussed.

---------------------------------------------------------
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.

---------------------------------------------------------
Title: Solar and meteoritic abundances of mercury
Authors: Grevesse, Nicolas
1970GeCoA..34.1129G Altcode:
It is shown, from the absence of Hg I lines in the solar photospheric
spectrum, that the solar mercury abundance must be much lower than
the value found in carbonaceous chondrites.

---------------------------------------------------------
Title: The solar abundance of nickel from photospheric [Ni ii] lines
Authors: Grevesse, N.; Swings, J. P.
1970SoPh...13...19G Altcode:
The detailed study of the possible presence of four [NiII] lines in
solar absorption leads to an abundanceANi = logNNi
= 6.30±0.30 (in the usual scale where logNH = 12.00),
in agreement with the coronal and meteoritic values.

---------------------------------------------------------
Title: Deuterium in the Solar Photospheric Spectrum
Authors: Grevesse, N.
1970MSRSL..19..249G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Recherche sur les abondances des elements dans l'atmosphere
d'une etoile G2V de la sequence principale: le soleil.
Authors: Grevesse, Nicolas
1970raea.book.....G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Abundances of the rare earths in the sun
Authors: Grevesse, N.; Blanquet, G.
1969SoPh....8....5G Altcode:
We have determined the solar abundances of the rare earths (La, Ce, Pr,
Nd, Sm, Eu, Gd, Dy, Er, Tm, Yb, Lu) on the basis of measurements made
on new high-resolution tracings of the solar spectrum obtained at the
International Scientific Station of the Jungfraujoch (Switzerland)
by L. Delbouille, L. Neven and G. Roland. Our results (Table XV)
are compared with those of other authors for the sun and meteorites
as well as with the abundances predicted by nucleosynthesis theories.

---------------------------------------------------------
Title: Forbidden Lines of Fe II in the Solar Photospheric Spectrum
Authors: Grevesse, N.; Swings, J. P.
1969A&A.....2...28G Altcode:
The theoretical profiles and equivalent widths of [Fe H] lines in
the solar photospheric spectrum are predicted. They are compared to
the values observed on ne direct intensity tracings obtained at the
International Scientific Station, Jungfraujoch (Switzerland). Twenty
faint solar absorption lines may be assigned to [Fe H]; each of them
is studied in detail. The photospheric iron abundance deduced from this
investigation is log = 7.50 (in the scale log NH = 12.00) in agreement
with the coronal and meteoritic values. The possible presence of [Fe I]
lines is also discussed. Two observed solar features at 5303.99 A and
5220.57 A may be due to [Fe I]; their transition probabilities are
estimated on the assumption that the identifications are correct. A
discussion of the discrepancies between the solar and theoretical
wavelengths of the [Fe H] lines is given in an Appendix.

---------------------------------------------------------
Title: Abundances of Heavy Elements in the Sun
Authors: Grevesse, Nicolas
1969SoPh....6..381G Altcode:
Solar abundances have been derived for Pb, Bi, Th and U. For the
three first elements, the abundances are determined from the profiles
of their lines obtained with the high resolution solar spectrometer
installed at the Jungfraujoch Scientific Station (Switzerland) and
from new oscillator strengths based on life-time measurements (Pb and
Bi). The possible presence of U in the solar spectrum is also examined.

---------------------------------------------------------
Title: Forbidden Sulphur I Lines in the Solar Spectrum
Authors: Swings, J. P.; Lambert, D. L.; Grevesse, N.
1969SoPh....6....3S Altcode:
The [SI] lines are due to transitions within the
3s23p4 ground configuration of neutral
sulphur. The results are presented from a search for the
[SI] lines in the Fraunhofer spectrum. Two identifications
are proposed with faint features in the Fraunhofer spectrum:
1D2-1S0 at λ⊙
= 7725.02 Å and 3P2-1D2
at λ⊙ = 10821.23 Å. Their measured equivalent widths
are shown to confirm the value for the solar abundance of sulphur,
logNS = 7.21 (in the scale logNH = 12.00),
which is derived from the permitted high-excitation lines. These
lines give the first convincing identification of [SI] lines in an
astrophysical source.

---------------------------------------------------------
Title: 20. Forbidden Sulphur I Lines in the Solar Spectrum
Authors: Swings, J. P.; Lambert, D. L.; Grevesse, N.
1969LIACo..15..209S Altcode: 1969MSRSL..17..209S
No abstract at ADS

---------------------------------------------------------
Title: Forbidden sulphur I lines in the solar spectrum.
Authors: Swings, J. P.; Lambert, D. L.; Grevesse, N.
1969MSRSL..25..209S Altcode: 1969tisa.conf..209S
No abstract at ADS

---------------------------------------------------------
Title: Solar Abundances of Lithium, Beryllium and Boron
Authors: Grevesse, Nicolas
1968SoPh....5..159G Altcode:
New solar abundances have been derived for Li, Be and B. They are
mainly based on high-resolution spectra obtained at the Jungfraujoch
Scientific Station (Switzerland). For Li, the abundance results from
a discussion of the photospheric and sunspot spectra. Our results, log
NLi = 0.42, log NBe = 1.17 and log NB
&lt; 2.80 (in the log NH = 12.00 scale), are lower than the
previously admitted abundances for these elements. The far UV spectrum
(λ &lt; 3000 Å) has also been considered in each case. The meaning
of our results is discussed from the point of view of the destruction
of these elements during the evolution of the sun.

---------------------------------------------------------
Title: Abundances solaires de quelques éléments représentatifs
au point de vue de la nucléosynthèse.
Authors: Grevesse, N.; Blanquet, G.; Boury, A.
1968ode..conf..177G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: The Abundance of Lead in the Sun
Authors: Grevesse, Nicolas
1967ApJ...149L..37G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Largeurs équivalentes et abondance du strontium dans le soleil
Authors: Grevesse, N.
1966AnAp...29..287G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: Discussion de l'identification de raies du bismuth dans
le soleil
Authors: Grevesse, N.
1966AnAp...29..365G Altcode:
No abstract at ADS

---------------------------------------------------------
Title: High Resolution Solar Spectroscopy at the Jungfraujoch
Scientific Station
Authors: Grevesse, N.
1965ASSL....2..357G Altcode: 1965istr.conf..357G
No abstract at ADS