Solar origins: Place and Chemical Composition
Abstract
We discuss a chemical evolution model with Z-dependent yields that reproduces the O/H, C/H, and C/O gradients of the Galactic disk and the chemical history of the solar vicinity. The model fits the H, He, C, and O abundances derived from recombination lines of the HII region M17 (including the fraction of C and O atoms embedded in dust); the protosolar H, He, C, O, and Fe abundances; and the C/O-O/H, C/Fe-Fe/H, and O/Fe-Fe/H relations derived from stars of the solar vicinity. The agreement of the model with the protosolar abundances at the Sun-formation time implies that the Sun originated from a well mixed ISM at a galactocentric distance of 7.6 0.8 kpc.
Keywords
Cite
@article{arxiv.1102.2937,
title = {Solar origins: Place and Chemical Composition},
author = {Leticia Carigi and Manuel Peimbert},
journal= {arXiv preprint arXiv:1102.2937},
year = {2011}
}
Comments
to appear in Rev. Mex. Astron and Astrofis. Conf. Ser. Proceedings of XIII Latin American Regional IAU Meeting. 2 pages and 1 figure