Black Hole Spin in X-Ray Binaries: Observational Consequences | Zendy

ShuangNan Zhang | Zendy; Wei Cui | Zendy; Wan Chen | Zendy

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Black Hole Spin in X-Ray Binaries: Observational Consequences

Author(s) -

ShuangNan Zhang,

Wei Cui,

Wan Chen

Publication year - 1997

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/310705

Subject(s) - physics , astrophysics , black hole (networking) , accretion (finance) , stellar black hole , spin flip , intermediate mass black hole , rotating black hole , accretion disc , active galactic nucleus , astronomy , x ray binary , spinning , thin disk , galaxy , neutron star , computer network , routing protocol , routing (electronic design automation) , computer science , link state routing protocol , mechanical engineering , engineering

We discuss the observational consequences of black hole spin in X-raybinaries within the framework of the standard thin accretion disk model. Whencompared to theoretical flux distribution from the surface of a thin disksurrounding a Kerr black hole, the observed X-ray properties of the Galacticsuperluminal jet sources, GRO J1655-40 and GRS 1915+105, strongly suggest thateach contains a black hole spinning rapidly in the same direction as theaccretion disk. We show, however, that some other black hole binaries with anultra-soft X-ray component probably harbor only non- or slowly-spinning blackholes, and we argue that those with no detectable ultra-soft component above1-2 keV in their high luminosity state may contain a fast-spinning black holebut with a retrograde disk. Therefore, all classes of known black hole binariesare united within one scheme. Furthermore, we explore the possibility thatspectral state transitions in Cyg X-1 are simply due to temporary diskreversal, which can occur in a wind accretion system.Comment: 18 pages, 1 table, 2 figures. Accepted for ApJ Letters, to appear in Vol. 482, June 2

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