The formation of brown dwarfs and low-mass stars by disc fragmentation

Details The formation of brown dwarfs and low-mass stars by disc fragmentation The formation of brown dwarfs and low-mass stars by disc fragmentation

2008-09-29

arxiv.org/abs/0809.5042v1

Astronomy and Astrophysics

Astrophysics

4 pages, 2 figures, to appear in the proceedings of the Cool Stars 15 conference

Scientific paper

10.1063/1.3099172

We suggest that a high proportion of brown dwarfs are formed by gravitational fragmentation of massive, extended discs around Sun-like stars. We argue that such discs should arise frequently, but should be observed infrequently, precisely because they fragment rapidly. By performing an ensemble of radiation-hydrodynamic simulations, we show that such discs typically fragment within a few thousand years to produce mainly brown dwarfs (including planetary-mass brown dwarfs) and low-mass hydrogen-burning stars. Subsequently most of the brown dwarfs are ejected by mutual interactions. We analyse the properties of these objects that form by disc fragmentation, and compare them with observations.

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