The Formation of Massive Star Systems by Accretion：（通过吸积大质量恒星系统的形成）.pdfVIP

The Formation of Massive Star Systems by Accretion 9 0 Mark R. Krumholz,1∗ Richard I. Klein,2,3 Christopher F. McKee,2,4 0 2 Stella S. R. Offner,4 and Andrew J. Cunningham3 n a J 1 Department of Astronomy, University of California, Santa Cruz 0 2 201 Interdisciplinary Sciences Building, Santa Cruz, CA 95064, USA ] 2Department of Astronomy, University of California, Berkeley R S 601 Campbell Hall, Berkeley, CA 94720-3411, USA h. 3Lawrence Livermore National Laboratory, AX Division p - 7000 East Avenue, Livermore, CA 94550, USA o 4 r Department of Physics, University of California, Berkeley t s 366 LeConte Hall, Berkeley, CA 94720-7300, USA a [ ∗ To whom correspondence should be addressed. E-mail: krumholz@. 1 v 7 5 Massive stars produce so much light that the radiation pressure they exert on 1 3 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 ac- 1 cretion. We present three-dimensional radiation-hydrodynamic simulations 0 9 of the collapse of a massive prestellar core and find that radiation pressure 0 does not halt accretion. Instead, gravitational and Rayleigh-Taylor instabil- : ities channel gas onto the star system through non-axisymmetric disks and v i filaments that self-shield against radiation, while allowing radiation to escape X through optically-thin bubbles. Gravitational instabilities cause the disk to