QPOs, Black Hole Mass and Angular Momentum from Diskoseismology

Details QPOs, Black Hole Mass and Angular Momentum from Diskoseismology QPOs, Black Hole Mass and Angular Momentum from Diskoseismology

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprs11002w&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

Calculations of the frequencies of the g-, c-, and p-modes of relativistic thin accretion disks are compared with recent observations of high frequency QPOs in X-ray binaries with black hole candidates. These classes of modes encompass all adiabatic perturbations of such disks. The frequencies of these modes depend mainly on only the mass and angular momentum of the black hole; their weak dependence on disk luminosity is also explicitly indicated. Identifying the recently discovered relatively stable QPO pairs in two microquasars (GRO J1655-40 and GRS 1915+105) with the fundamental g- and c-modes provides a determination of the mass and angular momentum of the black hole. The masses agree with those determined from recent spectroscopy of the companion star. We also indicate the radial extent of these modes. The amplitude, frequency width, and energy dependence of these QPOs are also discussed in the context of these modes.

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