Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 709, Issue 2, Pages L114-L118Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/709/2/L114
Keywords
binaries: general; planetary systems; planets and satellites: formation; protoplanetary disks
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Funding
- American Astronomical Society
- National Science Foundation
- Agence Nationale de la Recherche [ANR-07-BLAN-0221]
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In this Letter, I examine several observational trends regarding protoplanetary disks, debris disks, and exoplanets in binary systems in an attempt to constrain the physical mechanisms of planet formation in such a context. Binaries wider than about 100 AU are indistinguishable from single stars in all aspects. Binaries in the 5-100 AU range, on the other hand, are associated with shorter lived but (at least in some cases) equally massive disks. Furthermore, they form planetesimals and mature planetary systems at a similar rate as wider binaries and single stars, albeit with the peculiarity that they predominantly produce high-mass planets. I posit that the location of a stellar companion influences the relative importance of the core accretion and disk fragmentation planet formation processes, with the latter mechanism being predominant in binaries tighter than 100 AU.
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