Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21542312f&link_type=abstract
American Astronomical Society, AAS Meeting #215, #423.12; Bulletin of the American Astronomical Society, Vol. 42, p.328
Astronomy and Astrophysics
Astronomy
Scientific paper
It has been observed that stars with known planets are more metal-rich than surrounding field stars. One explanation is the accretion of hydrogen-depleted planetary matter into the atmospheres of the planet hosts. In such a case, trends of increasing abundances with increasing element Tc may be expected for a given host star. The presence of 6Li, which is expected to be completely destroyed during the pre-main sequence evolution of solar-type stars, could also be a strong accretion signal. High-resolution spectra (R 120,000, S/N=500-850) were obtained for 10 solar-type stars with planets in order to search for these accretion signatures. As the initial step in our analysis, stellar parameters - effective temperatures, surface gravities, and microturbulent velocities and Fe abundances - of the target stars have been derived from Fe I and Fe II lines via measurements of equivalent widths. Here we present the derived stellar parameters, Fe abundances, and the abundances of other elements of our planetary host sample. These results are complemented by our search for 6Li in these stars, which is presented in a companion paper at this meeting.
This research was supported by the NOAO/KPNO Research Experiences for Undergraduates (REU) Program which is funded by the National Science Foundation Research Experiences for Undergraduates Program and the Department of Defense ASSURE program through Scientific Program Order No. 13 (AST-0754223) of the Cooperative Agreement No. AST-0132798 between the Association of Universities for Research in Astronomy (AURA) and the NSF.
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