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Comparison between Extrasolar Planets and Low-Mass Secondaries

Published online by Cambridge University Press:  13 May 2016

Tsevi Mazeh  and
Shay Zucker
Tsevi Mazeh
Affiliation:
School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv, Israel
Shay Zucker
Affiliation:
School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv, Israel

Abstract

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This paper compares the statistical features of the sample of discovered extrasolar planets with those of the secondaries in nearby spectroscopic binaries, in order to enable us to distinguish between the two populations. Based on 32 planet candidates discovered until March 2000, we find that their eccentricity and period distribution are surprisingly similar to those of the binary population, while their mass distribution is remarkably different. The mass distributions definitely support the idea of two distinct populations, suggesting the planet candidates are indeed extrasolar planets. The transition between the two populations probably occurs at 10–30 Jupiter masses. We point out a possible negative correlation between the orbital period of the planets and the metallicity of their parent stars, which holds only for periods less than about 100 days. These short-period systems are characterized by circular or almost circular orbits.

Type
XIII. Planet Formation in Binary Systems
Information
Symposium - International Astronomical Union , Volume 200: The Formation of Binary Stars , 2001 , pp. 519 - 528
Copyright
Copyright © Astronomical Society of the Pacific 2001 

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