Black Hole Mass and Spin from the 2:3 Twin-peak QPOs in Microquasars

Details Black Hole Mass and Spin from the 2:3 Twin-peak QPOs in Microquasars Black Hole Mass and Spin from the 2:3 Twin-peak QPOs in Microquasars

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...708.1442m&link_type=abstract

The Astrophysical Journal, Volume 708, Issue 2, pp. 1442-1451 (2010).

Physics

2

Accretion, Accretion Disks, Black Hole Physics, Hydrodynamics, Relativity, Shock Waves

Scientific paper

In the Galactic microquasars with double peak kHz quasi-periodic oscillations (QPOs) detected in X-ray fluxes, the ratio of the twin-peak frequencies is exactly, or almost exactly 2:3. This rather strongly supports the fact that they originate a few gravitational radii away from its center due to two modes of accretion disk oscillations. Numerical investigations suggest that post-shock matter, before they settle down in a subsonic branch, execute oscillations in the neighborhood region of "shock transition". This shock may excite QPO mechanism. The radial and vertical epicyclic modes of oscillating matter exactly match with these twin-peak QPOs. In fully general relativistic transonic flows, we investigate that shocks may form very close to the horizon around highly spinning Kerr black holes and appear as extremum in the inviscid flows. The extreme shock location provides upper limit of QPOs and hence fixes "lower cutoff" of the spin. We conclude that the 2:3 ratio exactly occurs for spin parameters a >= 0.87 and almost exactly, for wide range of spin parameter, for example, XTE 1550-564, and GRO 1655-40 a>0.87, GRS 1915+105 a>0.83, XTE J1650-500 a>0.78, and H 1743-322 a>0.68. We also make an effort to measure unknown mass for XTE J1650-500(9.1 ~ 14.1 M sun) and H 1743-322(6.6 ~ 11.3 M sun).

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