期刊
SCIENCE
卷 323, 期 5915, 页码 754-757出版社
AMER ASSOC ADVANCEMENT SCIENCE
DOI: 10.1126/science.1165857
关键词
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资金
- NSF [AST-0807739, AST-0606831]
- Spitzer Space Telescope Theoretical Research Program
- NASA
- Jet Propulsion Laboratory
- Astrophysics Theory and Fundamental Physics Program [NAG 05-12042, NNG 06-GH96G]
- U.S. Department of Energy at Lawrence Livermore National Laboratory [B-542762]
- NSF San Diego Supercomputer Center [UCB267]
Massive stars produce so much light that the radiation pressure they exert on the gas and dust around them is stronger than their gravitational attraction, a condition that has long been expected to prevent them from growing by accretion. We present three- dimensional radiation-hydrodynamic simulations of the collapse of a massive prestellar core and find that radiation pressure does not halt accretion. Instead, gravitational and Rayleigh- Taylor instabilities channel gas onto the star system through nonaxisymmetric disks and filaments that self- shield against radiation while allowing radiation to escape through optically thin bubbles. Gravitational instabilities cause the disk to fragment and form a massive companion to the primary star. Radiation pressure does not limit stellar masses, but the instabilities that allow accretion to continue lead to small multiple systems.
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