Properties of Black Holes in Stellar Binary Systems

Recent X-ray timing and spectral observations of black hole binaries in outburst have redefined methods for investigating the properties of Galactic black holes and the physics of accretion flows. High-frequency X-ray QPOs in 5 systems (60--300 Hz) continue to be investigated as a possible means to constrain black hole mass and spin via interpretation as oscillations due to strong-field effects in General Relativity. In principle, black hole mass and spin may also be constrained via determination of the inner radius of the accretion disk, using spectroscopic parallax of the X-ray thermal component. However, an accurate application of this technique is fraught with difficulties. Monitoring programs that track the evolution of the thermal and power-law components in the X-ray spectrum provide new insights into modes of energy flow and the formation of relativistic jets