Three-dimensional structure of accretion disks in close binary systems

Details Three-dimensional structure of accretion disks in close binary systems Three-dimensional structure of accretion disks in close binary systems

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasj...43..809h&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 43, no. 6, 1991, p. 809-821.

Astronomy and Astrophysics

Astronomy

49

Accretion Disks, Companion Stars, Three Dimensional Models, X Ray Binaries, Dwarf Novae, Light Curve, Normal Density Functions, Time Dependence

Scientific paper

Time-dependent, 3D particle simulations of an accretion disk interacting with an incoming stream were performed as a model for disks in close binary systems. The half-thickness of the disk, which is calculated assuming a Gaussian density profile in the vertical direction, is much larger everywhere in the outer portions of the disk than the value expected from hydrostatic balance; the ratio of the vertical height (H) to the radius (r) is on average 10-20 percent, and is especially enhanced at the eclipse phases, above 0.8 and 0.2, where H/r is about 0.15. This is a result of a violent collision of the incoming stream with disk material. The gas in the disk is hit by the stream, thereby being given a vertical velocity component, which results in material moving up and down in the vertical direction with the Keplerian time-scale of the outer rim. Finally, it is suggested that the calculated extended rim structures are quite reminiscent of what is indicated from the orbital X-ray variation in some X-ray binaries, such as the accretion disk corona sources and the dipping sources, and in some dwarf novae, such as U Gem and OY Car.

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