Detection and Properties of Extrasolar Planets in Double and Multiple Star Systems

Details Detection and Properties of Extrasolar Planets in Double and Multiple Star Systems Detection and Properties of Extrasolar Planets in Double and Multiple Star Systems

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aspc..321...93e&link_type=abstract

Extrasolar Planets: Today and Tomorrow, ASP Conference Proceedings, Vol. 321, held 30 June - 4 July 2003, Institut D'Astrophysiq

Physics

Optics

4

Scientific paper

Among the extrasolar planets known today, 19 are orbiting a component of a multiple star system. In this contribution, we show that the properties of planets found in multiple star systems seem to be different from the ones of planets orbiting isolated stars: (i) as pointed out by Zucker & Mazeh (2002), the most massive short-period planets are all found in binaries; (ii) planets orbiting a component of a multiple star system tend to have a very low eccentricity when their period is shorter than about 40 days. These observations suggest that some kind of migration has been present in the history of the short-period planets found in multiple star systems, but are not easily explained by the current models of planet formation and evolution. Our knowledge regarding the existence and the characteristics of extrasolar planets in multiple star systems is, however, far from being complete. In particular, the influence of stellar duplicity on planet formation and evolution is still to be quantified. This is the goal of our VLT/NACO adaptive optics survey, which is also discussed here.

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