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Beyond the Iron Peak: r- and s-process Elemental Abundances in Stars with Planets (804)
BibTeX
@MISC{Bond804beyondthe,
author = {J. C. Bond and D. S. Lauretta and C. G. Tinney and R. P. Butler and G. W. Marcy and B. D. Carter and S. J. O’toole and J. Bailey},
title = {Beyond the Iron Peak: r- and s-process Elemental Abundances in Stars with Planets},
year = {804}
}
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Abstract
We present elemental abundances of 118 stars (28 of which are known extrasolar planetary host stars) observed as part of the Anglo-Australian Planet Search. Abundances of O, Mg, Cr, Y, Zr, Ba, Nd and Eu (along with previously published abundances for C and Si) are presented. This study is one of the first to specifically examine planetary host stars for the heavy elements produced by neutron capture reactions. We find that the host stars are chemically different to both the standard solar abundance and non-host stars in all elements studied, with enrichments over non-host stars ranging from 0.06 dex (for O) to 0.11 dex (for Cr and Y). Such abundance trends are in agreement with other previous studies of field stars and lead us to conclude that the chemical anomalies observed in planetary host stars are the result of normal galactic chemical evolution processes. Based on this observation, we conclude that the observed chemical traits of planetary host stars are primordial in origin, coming from the original nebula and not from a “pollution ” process occurring during or after formation and that planet formation occurs naturally with the evolution of stellar material.
Keyphrases
planetary host star iron peak s-process elemental abundance non-host star elemental abundance abundance trend neutron capture reaction previous study standard solar abundance pollution process normal galactic chemical evolution anglo-australian planet search planet formation stellar material chemical anomaly host star extrasolar planetary host star heavy element observed chemical trait field star original nebula
