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Brown Dwarf Companions to Solar-Type Stars and other Brown Dwarfs

Published online by Cambridge University Press:  19 September 2017

Eduardo L. Martín ,
Mike Connelley ,
Dan Potter  and
Hervé Bouy
Eduardo L. Martín
Affiliation:
Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, U.S.A.
Mike Connelley
Affiliation:
Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, U.S.A.
Dan Potter
Affiliation:
Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, U.S.A.
Hervé Bouy
Affiliation:
European Southern Observatory, Karl Schwarzschildstraße 2, Garching, Germany

Abstract

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We report on our ongoing imaging efforts to detect brown dwarfs orbiting solar-type stars and other brown dwarfs. We study the properties of brown dwarf companions as a function of primary mass. Our results indicate that the frequency of brown dwarf companions around solar-type stars for separations larger than about 40 AU is non-negligible. The frequency of brown dwarf binaries is about 20%. There is a dearth of brown dwarf binaries with separations larger than ∼20 AU. We propose that brown dwarf systems are a scaled down version of stellar systems, which probably form via triggered collapse of small molecular cores.

Type
Extrasolar Planets
Information
Symposium - International Astronomical Union , Volume 213: Bioastronomy 2002: Life Among the stars , 2004 , pp. 111 - 114
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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