Open AccessSpin of Stellar-Mass Black Holes Estimated by a Model of Quasi-Periodic Oscillations
Author(s) -
Shoji Kato,
Jun Fükue
Publication year - 2006
Publication title -
publications of the astronomical society of japan
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.99
H-Index - 110
eISSN - 2053-051X
pISSN - 0004-6264
DOI - 10.1093/pasj/58.5.909
Subject(s) - physics , dimensionless quantity , spin (aerodynamics) , excited state , black hole (networking) , oscillation (cell signaling) , quasi periodic , astrophysics , inertial frame of reference , quantum electrodynamics , classical mechanics , mechanics , atomic physics , routing (electronic design automation) , biology , genetics , thermodynamics , computer science , computer network , routing protocol , link state routing protocol
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 $a_*\leq 0.45$
Accelerating Research
Robert Robinson Avenue,
Oxford Science Park, Oxford
OX4 4GP, United Kingdom
Address
John Eccles HouseRobert Robinson Avenue,
Oxford Science Park, Oxford
OX4 4GP, United Kingdom