Statistical properties of exoplanets

Free access article

Issue		A&A Volume 417, Number 1, April I 2004


Page(s)		353 - 360
Section		Planets and planetary systems
DOI		http://dx.doi.org/10.1051/0004-6361:20034164

A&A 417, 353-360 (2004)
DOI: 10.1051/0004-6361:20034164

III. Planet properties and stellar multiplicity

A. Eggenberger, S. Udry and M. Mayor

Observatoire de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland
(Received 6 August 2003 / Accepted 3 December 2003)

Abstract
Among the hundred or so extrasolar planets discovered to date, 19 are orbiting a component of a double or multiple star system. In this paper, we discuss the properties of these planets and compare them to the characteristics of planets orbiting isolated stars. Although the sample of planets found in multiple star systems is not large, some differences between the orbital parameters and the masses of these planets and the ones of planets orbiting single stars are emerging in the mass-period and in the eccentricity-period diagrams. As pointed out by [CITE], the most massive short-period planets are all found in multiple star systems. We show here that the planets orbiting in multiple star systems also tend to have a very low eccentricity when their period is shorter than about 40 days. These observations seem to indicate that some kind of migration has been at work in the history of these systems. The properties of the five short-period planets orbiting in multiple star systems seem, however, difficult to explain with the current models of planet formation and evolution, at least if we want to invoke a single mechanism to account for all the characteristics of these planets.

Key words: stars: planetary systems -- stars: binaries: general

Offprint request: A. Eggenberger, Anne.Eggenberger@obs.unige.ch

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