Volume 586, February 2016
|Number of page(s)||6|
|Published online||05 February 2016|
Models of quasi-periodic oscillations related to mass and spin of the GRO J1655-40 black hole
Institute of Physics and Research Centre for Theoretical Physics and Astrophysics, Faculty of Philosophy and Science, Silesian University in Opava, Bezručovo nám.13, 74601 Opava, Czech Republic
Received: 13 March 2015
Accepted: 3 December 2015
Frequencies of the three quasi-periodic oscillation (QPO) modes observed simultaneously in the accreting black hole GRO J1655-40 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 high-frequency QPOs are generalized here to interpret also the low-frequency 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 X-ray spectroscopy techniques. We find that along with the relativistic precession model predicting M = (5.3 ± 0.1) M⊙,a = 0.286 ± 0.004, the so-called 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.
Key words: X-rays: binaries / black hole physics / accretion, accretion disks
© ESO, 2016
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.