Outbursts in Black Hole X-Ray Transients

Details Outbursts in Black Hole X-Ray Transients Outbursts in Black Hole X-Ray Transients

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7555h&link_type=abstract

HST Proposal ID #7555

Physics

Hst Proposal Id #7555 Binary Stars

Scientific paper

UV observations of soft X-ray transients {SXTs} will be made using STIS. This is part of an extensive multiwavelength target of opportunity campaign to monitor newly discovered SXTs in outburst and throughout the subsequent decline. Recent work establishes that a high proportion of SXTs harbor black holes, so these observations provide an unrivalled opportunity to obtain high quality data from an accreting black hole. UV data is a keystone of our multiwavelength campaign because the disk regions of interest radiate predominantly in the UV. Emission lines will allow us to probe the kinematics of the inner disk region. We will determine the relative strengths of the reprocessed X-ray flux emitted in the UV, and the UV flux generated by viscous heating in the accretion flow. Multiwavelength observations will probe the physics of the accretion flow throughout the outburst. The observations will yield a detailed quantitative test of the thermal disk instability model for SXT outbursts. FOS work on Nova Muscae 1991 demonstrated the critical importance to this test of recording the UV and optical spectrum during the decline. The new STIS/MAMA capability to perform UV spectroscopy with 125 microsecond time resolution will be exploited: an HST/XTE coordinated echo-mapping experiment will measure the size of the reprocessing regions in the accretion disk, and thus probe morphology changes as the decline proceeds.

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