Line formation in solar granulation IV. (O I), O I and OH lines and the photospheric O abundance

By Martin Asplund, N. Grevesse, A. Sauval, C. Allende Prieto, D. Kiselman. 2003

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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 loss es in the lines. We derive a solar oxygen abundance of log ǫO = 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 met al 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.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/bae5755add6598a6f354e8b2357b837dbed2ed8c

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Citations in the corpus

• Predicting dust extinction from the stellar mass of a galaxy (2010, result): “All (O/H) abundances can be converted to solar metallicities, using a value of 12 + log10(O/H) = 8.66 (Asplund et al. 2004), and the range 8.1 < 12 + log10(O/H) < 9 corresponds to 0.28 < Z/Z < 2.19.”
• Metallicities and Physical Conditions in Star-forming Galaxies at z ~ 1.0-1.5 (2008, methodology): “For comparison, we use the solar oxygen abundance expressed as 12 + log(O/H) = 8.66 (Allende Prieto et al. 2002; Asplund et al. 2004).”
• SINFONI Integral Field Spectroscopy of z ~ 2 UV-selected Galaxies: Rotation Curves and Dynamical Evolution (2006, background): “For an assumed solar value of 12þ log (O/H)¼ 8:65 (e.g., Asplund et al. 2004), we infer an oxygen abundance of about 1.25 times solar toward the center of Q2343-BX610 and approximately solar for the rest of the galaxy.”
• Probing the structure of protoplanetary disks: a comparative study of DM Tau, LkCa 15, and MWC 480 (2007, background): “In Fig.8, we present here also results for a metallicity Z = 0.01, much closer to the new Solar metallicity (0.0126, see Asplund et al. 2004; Grevesse et al. 2005, and references therein).”
• Stellar Abundance and Galactic Chemical Evolution through LAMOST Spectroscopic Survey (2006, background): “For the Sun the NLTE corrections for these lines are about −0.2 dex (Asplund et al. 2004), while it is reduced to about −0.1 dex when the hydrogen collisions from Drawin (1968) are included (Takeda 2003).”
• Physical parameters and wind properties of galactic early B supergiants (2005, methodology): “Solar abundances were taken from Grevesse & Sauval (1998) except oxygen, which was set at log(O/H)+12 = 8.66 (Asplund et al. 2004).”
• Physical Properties of Wolf-Rayet Stars (2006, methodology): “CNO compromises ∼1.1% by mass of the Solar photosphere (Asplund et al. 2004) versus 0.48% in the LMC and 0.24% in the SMC (Russell & Dopita 1990).”
• Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 solar masses (2009, critical): “Some more recent studies (e.g., Caffau et al. 2008, and references therein) confirm the high O abundances typical of older compilations of solar abundances, rather than the low values claimed by Asplund et al.(2004).”
• OXYGEN ABUNDANCES IN NEARBY FGK STARS AND THE GALACTIC CHEMICAL EVOLUTION OF THE LOCAL DISK AND HALO (2013, background): “Moreover, our solar oxygen abundance is within 0.01dex of the abundance inferred from the triplet lines by Asplund et al. (2004).”
• Improved Laboratory Transition Probabilities for Neutral Chromium and Redetermination of the Chromium Abundance for the Sun and Three Stars (2007, methodology): “Other model types we then tried include: MARCS (Gustaffson et al. 1975), ATLAS (Kurucz 1993), Grevesse & Sauval (1999), newMARCS (Gustaffson et al. 2003), and Asplund et al. (2004).”
• Helioseismology and Solar Abundances (2007, methodology): “They used the MULTI3D code (Botnen 1997; Botnen & Carlsson 1999; Asplund et al. 2003) to do non-LTE calculations.”