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2010MNRAS.401..727S - Mon. Not. R. Astron. Soc., 401, 727-742 (2010/January-2)
A numerical study of brown dwarf formation via encounters of protostellar discs.
SHEN S., WADSLEY J., HAYFIELD T. and ELLENS N.
Abstract (from CDS):
The newly formed objects had masses ranging from 0.9 to 127MJ, with the majority in the BD regime. These often resided in star-BD multiples and in some cases also formed hierarchical orbiting systems. Most of them had large angular momenta and highly flattened, disc-like shapes. With the inclusion of the appropriate physics, these could reasonably be expected to evolve into proto-BD discs with jets and subsequent planet formation around the BD. The objects had radii ranging from 0.1 to 10au at the time of formation. The disc gas was assumed to be locally isothermal, appropriate for the short cooling times in extended protostellar discs but not for condensed objects. An additional case with explicit cooling that reduced to zero for optically thick gas was simulated to test the extremes of cooling effectiveness and it was still possible to form objects in this case. Detailed radiative transfer (not studied here) is expected to lengthen the internal evolution time-scale for these objects so that they spend considerable time as puffed-up, prolate ellipsoids, but not to alter the basic result that proto-BD discs can form during protostellar encounters.
Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS
Journal keyword(s): hydrodynamics - instabilities - methods: numerical - stars: formation - stars: low-mass, brown dwarfs
Simbad objects: 7
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