Using binary statistics in Taurus-Auriga to distinguish between brown dwarf formation processes

Whether BDs form as stars through gravitational collapse ("star-like") or BDs and some very low-mass stars constitute a separate population which form alongside stars comparable to the population of planets, e.g. through circumstellar disk ("peripheral") fragmentation, is one of...

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Bibliographic Details
Published in:arXiv.org 2017-06
Main Authors: Marks, M, Martín, E L, Béjar, V J S, Lodieu, N, Kroupa, P, Manjavacas, M E, Thies, I, López, R Rebolo, Velasco, S
Format: Article
Language:English
Subjects:
Accretion disks
Binary stars
Density
Dependence
Fragmentation
Gravitational collapse
Initial mass function
Low mass stars
Populations
Slopes
Star & galaxy formation
Star clusters
Star formation
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Summary:Whether BDs form as stars through gravitational collapse ("star-like") or BDs and some very low-mass stars constitute a separate population which form alongside stars comparable to the population of planets, e.g. through circumstellar disk ("peripheral") fragmentation, is one of the key questions of the star-formation problem. For young stars in Taurus-Auriga the binary fraction is large with little dependence on primary mass above ~0.2Msun, while for BDs it is
ISSN:2331-8422
DOI:10.48550/arxiv.1706.01464