Testing the Planet Absorption Paradigm for Rapidly Rotating K Giant Stars

Details Testing the Planet Absorption Paradigm for Rapidly Rotating K Giant Stars Testing the Planet Absorption Paradigm for Rapidly Rotating K Giant Stars

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007noao.prop..291m&link_type=abstract

NOAO Proposal ID #2007B-0291

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Scientific paper

Two competing mechanisms proposed to account for the anomalously large rotational velocities of single K giant stars are angular momentum dredge-up via a deepening of the convective layer and accretion of a low- mass companion such as a giant planet or brown dwarf. Both theories are capable of explaining the excess of ^7Li often seen in giant star rapid rotators; however, each mechanism should leave distinct chemical fingerprints in other elements. For example, it has been shown that stars with planet systems often show a trend of increasing abundances for increasing element condensation temperature, as might be expected for the ingestion of chemically-fractionated material. It is also expected that ingestion of large planets will alter the stellar ^12C/^13C ratio by a perceptible degree. We intend to measure the stellar parameters, abundances of elements from lithium to europium, and the ratio of ^12C/^13C among a sample of rapid rotators we have discovered to make four separate chemical tests of the planet ingestion model for giant stars. Because planets are known to exist commonly as systems, our control sample will include K giants with at least one known planetary companion, as well as non-rapid rotators spanning a similar giant star population. This research may open new avenues for studying, at least statistically, planets around evolved stars.

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