期刊
ASTROPHYSICAL JOURNAL
卷 725, 期 2, 页码 1485-1494出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/725/2/1485
关键词
accretion, accretion disks; binaries: general; radiative transfer; turbulence
资金
- NSF [AST-0901055, AST-0908553]
- Ontario
- NSERC
- NASA [NNX09AK31G]
- US Department of Energy at the Lawrence Livermore National Laboratory [DE-AC52-07NA 27344]
- Alfred P.Sloan Fellowship
- National Science Foundation [AST-0807739]
- Direct For Mathematical & Physical Scien [0908553, 0807739] Funding Source: National Science Foundation
- Division Of Astronomical Sciences [0908553, 0807739] Funding Source: National Science Foundation
We characterize the infall rate onto protostellar systems forming in self-gravitating radiation-hydrodynamics simulations. Using two dimensionless parameters to determine the disks' susceptibility to gravitational fragmentation, we infer limits on protostellar system multiplicity and the mechanism of binary formation. We show that these parameters give robust predictions even in the case of marginally resolved protostellar disks. We find that protostellar systems with radiation feedback predominately form binaries via turbulent fragmentation, not disk instability, and predict that turbulent fragmentation is the dominant channel for binary formation for low-mass stars. We clearly demonstrate that systems forming in simulations including radiative feedback have fundamentally different parameters than those in purely hydrodynamics simulations.
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