Stability of accretion in low mass X-ray binaries

Details Stability of accretion in low mass X-ray binaries Stability of accretion in low mass X-ray binaries

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...210..174s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 210, no. 1-2, Feb. 1989, p. 174-180. Research supported by Polska Akademia Nau

Astronomy and Astrophysics

Astrophysics

6

Accretion Disks, Neutron Stars, Red Giant Stars, Stellar Mass Accretion, Stellar Winds, X Ray Binaries, Faint Objects, Light Curve, Optical Thickness, Stellar Coronas, Stellar Mass

Scientific paper

X-ray heating is known to produce in low mass X-ray binaries (LMXRBs) a corona of an accretion disk and a wind. It is demonstrated that the wind is optically thick for X-rays propagating towards the cool companion. It is pointed out that modulation of heating of a red companion by absorption in the wind may stabilize self induced accretion in the source. Also considered is standard feedback between X-ray heating and mass loss from the disk and the red companion. Four types of behavior were found to be possible: stationary, oscillatory, chaotic, and runaway.

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