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Post Info TOPIC: SWIFT J1753.5-0127
Blobrana


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Date:
2MAXI J1753-013
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ATel 10110: Radio detections of the brightening black hole candidate Swift J1753.5-0127 made with the Arcminute Microkelvin Imager Large Array



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Blobrana


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RE: SWIFT J1753.5-0127
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ATel 10081: X-ray/UV re-brightening of Swift J1753.5-0127 observed with Swift



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2MAXI J1753-013
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ATel 10075: Optical brightening of Swift J1753.5-0127 observed with the Faulkes Telescope North



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Blobrana


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SWIFT J175328.5-012704
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Title: Expanding hot flow in the black hole binary SWIFT J1753.5-0127: evidence from optical timing
Author: A. Veledina, P. Gandhi, R. Hynes, J. J. E. Kajava, S. S. Tsygankov, M. G. Revnivtsev, M. Durant, J. Poutanen

We describe the evolution of optical and X-ray temporal characteristics during the outburst decline of the black hole X-ray binary SWIFT J1753.5-0127. The optical/X-ray cross-correlation function demonstrates a single positive correlation at the outburst peak, then it has multiple dips and peaks during the decline stage, which are then replaced by the precognition dip plus peak structure in the outburst tail. Power spectral densities and phase lags show a complex evolution, revealing the presence of intrinsically connected optical and X-ray quasi-periodic oscillations. For the first time, we quantitatively explain the evolution of these timing properties during the entire outburst within one model, the essence of which is the expansion of the hot accretion flow towards the tail of the outburst. The pivoting of the spectrum produced by synchrotron Comptonization in the hot flow is responsible for the appearance of the anti-correlation with the X-rays and for the optical quasi-periodic oscillations. Our model reproduces well the cross-correlation and phase lag spectrum during the decline stage, which could not be understood with any model proposed before.

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Blobrana


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RE: SWIFT J1753.5-0127
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ATel 9758: Optical/UV follow-up observations of Swift J1753.5-0127



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Blobrana


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ATel 9741: Detection of a very red source at the position of SWIFT J1753.5-0127



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ATel 9739: Follow-up optical observations of Swift J1753.5-0127 as it fades into quiescence



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Blobrana


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ATel 9735: Swift J1753.5-0127 no longer detected by Swift



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Blobrana


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Posts: 131433
Date:
SWIFT J175328.5-012704
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ATel 9708: Swift J1753.5-0127 is heading to quiescence after an 11-year outburst



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Blobrana


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Posts: 131433
Date:
RE: SWIFT J1753.5-0127
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Title: A 420 day X-ray/optical modulation and extended X-ray dips in the short-period transient Swift J1753.5-0127
Authors: A. W. Shaw, P. A. Charles, A. J. Bird, R. Cornelisse, J. Casares, F. Lewis, T. Muņoz-Darias, D. M. Russell, C. Zurita

We have discovered a ~420d modulation, with associated X-ray dips, in RXTE-ASM/MAXI/Swift-BAT archival light-curves of the short-period (3.2h) black-hole X-ray transient, Swift J1753.5-0127. This modulation only appeared at the end of a gradual rebrightening, approximately 3 years after the initial X-ray outburst in mid-2005. The same periodicity is present in both the 2-20 keV and 15-50 keV bands, but with a ~0.1 phase offset (~40d). Contemporaneous photometry in the optical and near-IR reveals a weaker modulation, but consistent with the X-ray period. There are two substantial X-ray dips (very strong in the 15-50 keV band, weaker at lower energies) that are separated by an interval equal to the X-ray period. This likely indicates two physically separated emitting regions for the hard X-ray and lower energy emission. We interpret this periodicity as a property of the accretion disc, most likely a long-term precession, where the disc edge structure and X-ray irradiation is responsible for the hard X-ray dips and modulation, although we discuss other possible explanations, including Lense-Thirring precession in the inner disc region and spectral state variations. Such precession indicates a very high mass ratio LMXB, which even for a ~10 solar mass BH requires a brown dwarf donor (~0.02 solar masses), making Swift J1753.5-0127 a possible analogue of millisecond X-ray pulsars. We compare the properties of Swift J1753.5-0127 with other recently discovered short-period transients, which are now forming a separate population of high latitude BH transients located in the galactic halo.

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