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Does the Sun have a subsolar metallicity?

Published online by Cambridge University Press:  01 April 2008

Martin Asplund
Martin Asplund*
Affiliation:
Max Planck Institute for Astrophysics, Postfach 1317, D-85741 Garching b. München, Germany email: asplund@mpa-garching.mpg.de
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Abstract

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The solar chemical composition has recently undergone a drastic revision, in particular in terms of the C, N, O and Ne abundances that have been lowered by almost a factor of two. In this invited review I will describe the different compounding reasons for this change (3D model atmospheres, non-LTE line formation, improved atomic/molecular data) and discuss some astrophysical implications thereof, which fall under both good (solar neighborhood) and bad (helioseismology) news. The most recent literature regarding the solar O abundance is surveyed and a critical evaluation whether or not these support the low solar abundance scale is presented. Finally I venture to make some predictions to what the real solar O abundance may be.

Keywords

Convectionline: formationradiative transferSun: abundancesSun: atmosphereSun: granulation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 13 - 26
Copyright
Copyright © International Astronomical Union 2008

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