Planetesimal Metal Pollution of Planet-Bearing Stars

Details Planetesimal Metal Pollution of Planet-Bearing Stars Planetesimal Metal Pollution of Planet-Bearing Stars

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...19712807d&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #128.07; Bulletin of the American Astronomical Society, Vol. 33, p.711

Astronomy and Astrophysics

Astronomy

Scientific paper

As more stars have been identified to have planets, evidence has mounted that stars with planets are on average more metal-rich than field stars. This fact immediately suggests two possible explanations. One is that higher-Z gas clouds are more likely to form planets. The second is that the production of planets results in the injection of high-Z pollutants (planets, planetesimals, or remnant dust from the protostellar disk) into the star. In this study, we model the evolution of stars polluted by planetesimals to see if the observed heavy element abundances of planet-bearing stars can be explained. Since convective mixing can quickly dilute surface pollutants, stars with very low-mass convection zones provide the strongest tests of this picture. While relatively small pollutant masses could significantly alter the metallicities of these stars, diffusion will help regulate the metallicity enhancements. The dependence of the heavy element abundance on star mass also constrains the possible depth of penetration for the pollutants. The results of our stellar evolution modeling (including the effects of element diffusion) will be presented and discussed.

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