Constraints on Planet Formation in Close Binary Systems

Details Constraints on Planet Formation in Close Binary Systems Constraints on Planet Formation in Close Binary Systems

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.8107j&link_type=abstract

American Astronomical Society, AAS Meeting #211, #81.07; Bulletin of the American Astronomical Society, Vol. 39, p.872

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Scientific paper

Circumstellar disks around stars in close binaries will be tidally truncated by the orbit of the stellar companion. The truncation is still more severe if the orbit is eccentric. Can planets form in such systems, or is the protoplanetary disk too truncated for planets to form? Recent discoveries of planets in systems such as γ-Cep and the dispute over whether or not a planet exists in HD 188753 have brought this question into sharp focus. We examine the mass, temperatures, and other properties of truncated disks in close binary star systems to determine whether or not they can support in situ planet formation. While HD 188753 is too closely truncated to allow in situ planet formation, we find that sufficient disk material in γ-Cep does remain. We explore a range of stellar orbital parameters to determine limits on how closely stars are allowed to orbit each other and still support planet formation.

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