Bibcode
van der Klis, M.; Fender, R.; Wijnands, R.; Linares, M.; Altamirano, D.; Méndez, M.; Casella, P.; Belloni, T.; Motta, S.; Muñoz-Darias, T.; Soleri, P.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society, Volume 429, Issue 2, p.1244-1257
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2
2013
Citations
40
Refereed citations
40
Description
We present our monitoring campaign of the outburst of the black hole
candidate Swift J1753.5-0127, observed with the Rossi X-ray Timing
Explorer and the Swift satellites. After ˜4.5 yr since its
discovery, the source had a transition to the hard intermediate state.
We performed spectral and timing studies of the transition showing that,
unlike the majority of the transient black holes, the system did not go
to the soft states but it returned to the hard state after a few months.
During this transition Swift J1753.5-0127 features properties which are
similar to those displayed by the black hole Cygnus X-1. We compared
Swift J1753.5-0127 to one dynamically confirmed black hole and two
neutron stars showing that its power spectra are in agreement with the
binary hosting a black hole. We also suggest that the prolonged period
at low flux that followed the initial flare is reminiscent of that
observed in other X-ray binaries, as well as in cataclysmic variables.
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Accreting black-holes and neutron stars in X-ray binaries provide an ideal laboratory for exploring the physics of compact objects, yielding not only confirmation of the existence of stellar mass black holes via dynamical mass measurements, but also the best opportunity for probing high-gravity environments and the physics of accretion; the most
Montserrat
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