X-ray Spectral and timing properties of the black hole x-ray transient Swift J1753.5-0127
arXiv:astro-ph/0701489 · doi:10.1086/512799
Abstract
We have carried out detailed analysis on the black hole candidate (BHC) X- ray transient Swift J1753.5-0127 observed by the Rossi X-Ray Timing Explorer (RXTE) during its outburst in 2005 {2006. The spectral analysis shows that the emissions are dominated by the hard X-rays, thus revealing the low/hard state of the source during the outburst. The peak luminosity is found lower than the typical value of balancing the mass flow and evaporation of the inner edge of disk (Meyer-Hofmeister 2004). As a result, the disk is prevented from extending inward to produce strong soft X-rays, corresponding to the so-called high/soft state. These are the typical characteristics for a small subset of BHCs, i.e. those soft X-ray transients stay at the low/hard state during the outburst. In most observational time, the QPO frequencies are found to vary roughly linearly with the fluxes and the spectral indices, while the deviation from this relationship at the peak luminosity might provide the first observational evidence of a partially evaporated inner edge of the accretion disk. The anti-correlation between the QPO frequency and spectral color suggests that the global disk oscillation model proposed by Titarchuk & Osherovich (2000) is not likely at work.
Accepted by ApJ, 24 pages, 13 figures, 3 tables
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- Accretion Flow Properties of Swift J1753.5-0127 during its 2005 outburst
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- The X-ray Spectrum Of The Black Hole Candidate Swift J1753.5-0127
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- Swift J1753.5-0127 : Understanding the accretion geometry through frequency resolved spectroscopy
- Long-Term Monitoring of the Black Hole Candidate Swift J1753.5-0127 with INTEGRAL/SPI