Models of quasiperiodic oscillations related to mass and spin of the GRO J165540 black hole
Abstract
Frequencies of the three quasiperiodic oscillation (QPO) modes observed simultaneously in the accreting black hole GRO J165540 are compared with the predictions of models. Models in which all three QPO signals are produced at the same radius are considered: these include different versions of relativistic precession, epicyclic resonance, tidal disruption, and warped disc models. Models that were originally proposed to interpret only the twin highfrequency QPOs are generalized here to interpret also the lowfrequency QPO in terms of relativistic nodal precession. Inferred values of the black hole mass and spin from each QPO model are compared with the mass measured from optical observations and the spin inferred from Xray spectroscopy techniques. We find that along with the relativistic precession model predicting M = (5.3 ± 0.1) M_{⊙},a = 0.286 ± 0.004, the socalled total precession model (M = (5.5 ± 0.1) M_{⊙},a = 0.276 ± 0.003), and the resonance epicyclic model with beat frequency (M = (5.1 ± 0.1) M_{⊙},a = 0.274 ± 0.003) also satisfy the optical mass test.
 Publication:

Astronomy and Astrophysics
 Pub Date:
 February 2016
 DOI:
 10.1051/00046361/201526095
 arXiv:
 arXiv:1603.07366
 Bibcode:
 2016A&A...586A.130S
 Keywords:

 Xrays: binaries;
 black hole physics;
 accretion;
 accretion disks;
 Astrophysics  High Energy Astrophysical Phenomena
 EPrint:
 Astronomy &