Author name code: grevesse ADS astronomy entries on 2022-09-14 author:"Grevesse, Nicolas" ------------------------------------------------------------------------ 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. Bibcode: 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. 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. Bibcode: 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 cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/656/A113 Title: VizieR Online Data Catalog: The solar CNO abundances (Amarsi+, 2021) Authors: Amarsi, A. M.; Grevesse, N.; Asplund, M.; Collet, R. Bibcode: 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). Title: The chemical make-up of the Sun: A 2020 vision Authors: Asplund, M.; Amarsi, A. M.; Grevesse, N. Bibcode: 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. 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. Bibcode: 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. Title: The Solar Chemical Composition: Past and Present Authors: Grevesse, Nicolas Bibcode: 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. 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. Bibcode: 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. Title: Understanding the Internal Chemical Composition and Physical Processes of the Solar Interior Authors: Basu, Sarbani; Grevesse, Nicolas; Mathis, Stephane; Turck-Chièze, Sylvaine Bibcode: 2017hdsi.book...55B Altcode: No abstract at ADS 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 Bibcode: 2016MNRAS.463....2S Altcode: 2016arXiv160405318S; 2016MNRAS.tmp.1051S We critically examine recent claims of a high solar metallicity by von Steiger & 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. Title: Understanding the Internal Chemical Composition and Physical Processes of the Solar Interior Authors: Basu, Sarbani; Grevesse, Nicolas; Mathis, Stephane; Turck-Chièze, Sylvaine Bibcode: 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. Title: The elemental composition of the Sun. III. The heavy elements Cu to Th Authors: Grevesse, Nicolas; Scott, Pat; Asplund, Martin; Sauval, A. Jacques Bibcode: 2015A&A...573A..27G Altcode: 2014arXiv1405.0288G We re-evaluate the abundances of the elements in the Sun from copper (Z = 29) to thorium (Z = 90). Our results are mostly based on neutral and singly-ionised lines in the solar spectrum. We use the latest 3D hydrodynamic solar model atmosphere, and in a few cases also correct for departures from local thermodynamic equilibrium (LTE) using non-LTE (NLTE) calculations performed in 1D. In order to minimise statistical and systematic uncertainties, we make stringent line selections, employ the highest-quality observational data and carefully assess oscillator strengths, hyperfine constants and isotopic separations available in the literature, for every line included in our analysis. Our results are typically in good agreement with the abundances in the most pristine meteorites, but there are some interesting exceptions. This analysis constitutes both a full exposition and a slight update of the relevant parts of the preliminary results we presented in Asplund et al. (2009, ARA&A, 47, 481), including full line lists and details of all input data that we have employed.

Tables 1-3 are available in electronic form at http://www.aanda.org 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 Bibcode: 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&A, 47, 481), including full line lists and details of all input data we employed.

Tables 1-3 are available in electronic form at http://www.aanda.org 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 Bibcode: 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 & 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 & 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&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 http://www.aanda.org Title: Photospheric Constraints, Current Uncertainties in Models of Stellar Atmospheres, and Spectroscopic Surveys Authors: Plez, Bertrand; Grevesse, Nicolas Bibcode: 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. Title: ``Old'' versus ``New'' Solar Chemical Composition Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P. Bibcode: 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 & Grevesse (1989), Grevesse & Noels (1993) and Grevesse & 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. Title: Why GN93 should not be used anymore Authors: Grevesse, N.; Asplund, M.; Sauval, J.; Scott, P. Bibcode: 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. Title: The New Solar Chemical Composition — from Z = 0.02 to Z = 0.013 Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P. Bibcode: 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. 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. Bibcode: 2012EAS....54....3S Altcode: No abstract at ADS 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. Bibcode: 2012EAS....54...65S Altcode: No abstract at ADS 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. Bibcode: 2012EAS....54.....S Altcode: No abstract at ADS 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. Bibcode: 2012EAS....54....1S Altcode: No abstract at ADS 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. Bibcode: 2012EAS....54..319S Altcode: No abstract at ADS 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. Bibcode: 2012EAS....54..255S Altcode: No abstract at ADS 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. Bibcode: 2012EAS....54..187S Altcode: No abstract at ADS Title: The chemical composition of the sun Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P. Bibcode: 2011CaJPh..89..327G Altcode: No abstract at ADS Title: The New Solar Composition and the Solar Metallicity Authors: Grevesse, Nicolas; Asplund, Martin; Sauval, A. Jacques; Scott, Pat Bibcode: 2011sswh.book...51G Altcode: No abstract at ADS Title: The chemical composition of the Sun Authors: Grevesse, N.; Asplund, M.; Sauval, A. J.; Scott, P. Bibcode: 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. Title: The Chemical Composition of the Sun Authors: Asplund, Martin; Grevesse, Nicolas; Sauval, A. Jacques; Scott, Pat Bibcode: 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. 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. Bibcode: 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. Title: The solar abundance of Oxygen Authors: Grevesse, N. Bibcode: 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 Bibcode: 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 & 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 & 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. Bibcode: 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. Bibcode: 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 & 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. 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. Bibcode: 2005A&A...435..339A Altcode: A&A, 417, 751-768 (2004), DOI:10.1051/0004-6361:20034328 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 2000IAUTA..24..380R Altcode: No abstract at ADS Title: The solar abundance of iron and the photospheric model Authors: Grevesse, N.; Sauval, A. J. Bibcode: 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. Bibcode: 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 Bibcode: 1999SSRv...88..606G Altcode: No abstract at ADS Title: Standard Solar Composition Authors: Grevesse, N.; Sauval, A. J. Bibcode: 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. Bibcode: 1998sce..conf..161G Altcode: No abstract at ADS Title: Le soleil, une étoile, notre étoile. Authors: Grevesse, N. Bibcode: 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. Bibcode: 1996SSRv...77..369M Altcode: No abstract at ADS Title: Standard Abundances Authors: Grevesse, N.; Noels, A.; Sauval, A. J. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1995sews.book.....N Altcode: No abstract at ADS Title: Solar abundances, convection and the standard solar model Authors: Noels, A.; Grevesse, N.; Mazzitelli, I. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1994IAUS..154..543J Altcode: No abstract at ADS Title: Molecules in the Sun and Molecular Data Authors: Grevesse, Nicolas; Sauval, A. Jacques Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1993SSRv...65..365W Altcode: No abstract at ADS Title: Cosmic abundances of the elements. Authors: Grevesse, N.; Noels, A. Bibcode: 1993oee..conf...15G Altcode: No abstract at ADS Title: La composition chimique du Soleil. Authors: Grevesse, N.; Noels, A. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 Bibcode: 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. Bibcode: 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. Bibcode: 1991IAUS..145...63G Altcode: No abstract at ADS Title: The Infrared Solar Spectrum Authors: Grevesse, N.; Sauval, A. J. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 Bibcode: 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 Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1981C&T....97S.193G Altcode: No abstract at ADS Title: La photosphére: Champ magnétique Authors: Grevesse, N. Bibcode: 1981C&T....97V.111G Altcode: No abstract at ADS Title: La composition chimique du Soleil: Abondances isotopiques Authors: Grevesse, N. Bibcode: 1981C&T....97R.193G Altcode: No abstract at ADS Title: La composition chimique du soleil. Authors: Grevesse, N. Bibcode: 1981C&T....97..217G Altcode: No abstract at ADS Title: La photosphére: Oscillations solaires Authors: Grevesse, N. Bibcode: 1981C&T....97T.111G Altcode: No abstract at ADS Title: La photosphère: Spectre Authors: Grevesse, N. Bibcode: 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. Bibcode: 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. Bibcode: 1981C&T....97S.111G Altcode: No abstract at ADS Title: La photosphére: Granulation Authors: Grevesse, N. Bibcode: 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. Bibcode: 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. Bibcode: 1980A&A....84..242B Altcode: No abstract at ADS Title: Molecular Data Needed in Stellar Spectroscopy Studies Authors: Grevesse, N.; Sauval, A. J. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1976ApL....17..199L Altcode: No abstract at ADS Title: The Solar Photospheric Abundance of Iron Authors: Biemont, E.; Grevesse, N. Bibcode: 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<λ<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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1973A&A....27..163B Altcode: Summary. Infrared wavelengths (1 < <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 &le Z <= 20 Authors: Biemont, E.; Grevesse, N. Bibcode: 1973ADNDT..12..217B Altcode: Infrared wavelengths (1μ < λ < 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. Bibcode: 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. > 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. Bibcode: 1972BSRSL..42..307B Altcode: No abstract at ADS Title: A Search for CH+ in the Solar Photospheric Spectrum Authors: Grevesse, N.; Sauval, A. J. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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 Bibcode: 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. Bibcode: 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. Bibcode: 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 Bibcode: 1970raea.book.....G Altcode: No abstract at ADS Title: Abundances of the rare earths in the sun Authors: Grevesse, N.; Blanquet, G. Bibcode: 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. Bibcode: 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 Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1969MSRSL..25..209S Altcode: 1969tisa.conf..209S No abstract at ADS Title: Solar Abundances of Lithium, Beryllium and Boron Authors: Grevesse, Nicolas Bibcode: 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 < 2.80 (in the log NH = 12.00 scale), are lower than the previously admitted abundances for these elements. The far UV spectrum (λ < 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. Bibcode: 1968ode..conf..177G Altcode: No abstract at ADS Title: The Abundance of Lead in the Sun Authors: Grevesse, Nicolas Bibcode: 1967ApJ...149L..37G Altcode: No abstract at ADS Title: Largeurs équivalentes et abondance du strontium dans le soleil Authors: Grevesse, N. Bibcode: 1966AnAp...29..287G Altcode: No abstract at ADS Title: Discussion de l'identification de raies du bismuth dans le soleil Authors: Grevesse, N. Bibcode: 1966AnAp...29..365G Altcode: No abstract at ADS Title: High Resolution Solar Spectroscopy at the Jungfraujoch Scientific Station Authors: Grevesse, N. Bibcode: 1965ASSL....2..357G Altcode: 1965istr.conf..357G No abstract at ADS