We compare our calculations of the frequencies of the fundamental g , c , and p–modes of relativistic thin accretion disks 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 with the fundamental g and c modes provides a determination of the mass and angular momentum of the black hole .
For GRO J1655–40 , M = 5.9 \pm 1.0 M _ { \sun } , J = ( 0.917 \pm 0.024 ) GM ^ { 2 } / c , in agreement with spectroscopic mass determinations .
For GRS 1915+105 , M = 42.4 \pm 7.0 M _ { \sun } , J = ( 0.926 \pm 0.020 ) GM ^ { 2 } / c or ( less favored ) M = 18.2 \pm 3.1 M _ { \sun } , J = ( 0.701 \pm 0.043 ) GM ^ { 2 } / c .
We briefly address the issues of the amplitude , frequency width , and energy dependence of these QPOs .