Mass estimate of the XTE J1650-500 black hole from the extended orbital resonance model for high-frequency QPOs

Abstract

Context. XTE J1650-500 is a Galactic black-hole binary system for which at least one high-frequency QPO at 250 Hz was reported. Moreover there are indications that the system harbours a near-extreme Kerr black-hole with a spin a∗ ≃ 0.998 and mass MBH . 7.3 M⊙. Recently it was discovered that the orbital 3-velocity of t est-particle (geodesical) discs orbiting Kerr black holes with the spin a∗ > 0.9953, being analyzed in the locally non-rotating frames, reveals a hump near the marginally stable orbit. Further it was suggested that the hump could excite the epicyclic motion of particles near the ISCO with frequencies typical for high-frequency QPOs. Characteristic frequency of the hump-induced oscillations was defined as the maximal positive rate of change of th e LNRFrelated orbital velocity with the proper radial distance. I f the characteristic “humpy frequency” and the radial epicyclic frequency are commensurable, strong resonant phenomena are expected. Aims. Application of the idea of hump-induced oscillations in accretion discs around near-extreme Kerr black holes to estimate the black-hole mass in XTE J1650-500 binary system. Methods. For the Kerr black hole with spin a∗ ≃ 0.9982 the characteristic “humpy frequency” and the radial epicyclic frequency at the orbit, where the positive rate of change of the LNRF-related orbital velocity with the proper radial distance is maxi mal, are in ratio 1:3. Identifying the radial epicyclic frequency with the ob served 250 Hz QPO, we arrive at the mass of the black hole. In this method the ratio of frequencies determines the spin (and vice versa), and concrete values of frequencies determine the black-hole mass. Results. Mass of the Kerr black hole in XTE J1650-500 binary system is estimated to be around 5.1 M⊙.