High-Resolution Spectroscopy of Exoplanetary Hosts: Accretion & ^6Li

Details High-Resolution Spectroscopy of Exoplanetary Hosts: Accretion & ^6Li High-Resolution Spectroscopy of Exoplanetary Hosts: Accretion & ^6Li

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006noao.prop..473s&link_type=abstract

NOAO Proposal ID #2006B-0473

Astronomy and Astrophysics

Astrophysics

Scientific paper

Over the past decade, the study of solar-type stars has climaxed with not only the discovery that distant Suns harbor exoplanets, but speculation that they might ingest them as well. Indeed, it is now well established that stars with planets tend to be more metal-rich than random field stars, and a trend of increasing abundances with increasing elemental condensation temperatures (T_c) has been found for a subset of known exoplanetary hosts. Accretion of H-depleted circumstellar material has been proposed as a possible explanation for both of these observations. If true, such accretion might have a wealth of astrophysical implications for planetary evolution, Galactic chemical evolution, and the astration of photospheric light elements. We propose to obtain very high-resolution (R=150,000) and high S/N (~400 per pixel) echelle spectra of a sample of 8 exoplanetary hosts that exhibit T_c-dependent abundance trends. The proposed spectra will be used to search for measurable abundances of ^6Li like that seen in the multiple exoplanet system HD 82943 and believed to be a unique signature of accretion in old solar-type dwarfs. If found, the presence of ^6Li combined with T_c-dependent abundance trends, along with potentially enhanced ^7Li abundances, would provide strong evidence that at least a subset of exoplanetary hosts have accreted H- depleted material.

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