On the Formation of Brown Dwarfs

Details On the Formation of Brown Dwarfs On the Formation of Brown Dwarfs

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004rmxac..21..227j&link_type=abstract

The Environment and Evolution of Double and Multiple Stars, Proceedings of IAU Colloquium 191, held 3-7 February, 2002 in Merida

Astronomy and Astrophysics

Astronomy

Stars: Low Mass, Brown Dwarfs

Scientific paper

The observational properties of brown dwarfs pose challenges to the theory of star formation. Because their masses are much smaller than the typical Jeans mass of interstellar clouds, brown dwarfs are most likely formed through secondary fragmentation processes, rather than through the direct collapse of a molecular cloud core. In order to prevent substantial post-formation mass accretion, young brown dwarfs must leave the high-density formation regions in which they form. We propose here that brown dwarfs are formed in the optically thin outer regions of circumbinary disks. Through post-formation dynamical interaction with their host binary stars, young brown dwarfs are either scattered to large distance or removed, with modest speed, from their cradles.

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