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Spin of Stellar-Mass Black Holes Estimated by a Model of Quasi-Periodic Oscillations

Shoji Kato·Jun Fukue
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Abstract

We have proposed in previous papers that the high-frequency pair QPOs observed in black-hole binaries with frequency ratio 3:2 are inertial-acoustic oscillations (nearly horizontal oscillations with no node in the vertical direction) or g-mode oscillations, which are resonantly excited on warped relativistic disks. The resonance occurs through horizontal motions. In this model the dimensionless spin parameter $a_*$ of the central sources can be estimated when their masses are known from other observations. This estimate is done for three sources (GRO J1665-40, XTE J1550-564, GRS 1915+105). For all of them we have $a_*\leq 0.45$.

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Shoji Kato, Jun Fukue. 2006-08-27. Spin of Stellar-Mass Black Holes Estimated by a Model of Quasi-Periodic Oscillations. https://doi.org/10.1093/pasj%2F58.5.909

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