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3-D Hydro dynamic Simulation of Accretion Disk Formation in LMC-X4

Published online by Cambridge University Press:  12 April 2016

Michael P. Owen  and
John M. Blondin
Michael P. Owen
Affiliation:
Dept. of Physics, NCSU, Raleigh, NC 27695–8202
John M. Blondin
Affiliation:
Dept. of Physics, NCSU, Raleigh, NC 27695–8202

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We present preliminary results of a time-dependent, three-dimensional hydrodynamic simulation of LMC-X4, an HMXB known to be undergoing RLOF. The simulation is initialized with the collapsed companion embedded in the undisturbed primary wind. The primary is in contact with the Roche surface, although no tidal stream or accretion disk is initialed; they are allowed to form independently.

Several features of general interest to disk-fed HMXBs are apparent in the simulation. First, the primary immediately develops a compressed-wind disk in the orbital plane. This may be a natural result in most disk-fed HMXBs. Fora circularized system in an orbit close enough for RLOF to take place, we may expect the primary to be in corotation. The surface velocity may then be a significant fraction of the breakup velocity, leading to a compressed-wind disk.

Type
Part 15. Poster Papers
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 779
Copyright
Copyright © Astronomical Society of the Pacific 1997