Search for Non-Thermal Emission in a Quiescent Black-Hole X-ray Binary

Details Search for Non-Thermal Emission in a Quiescent Black-Hole X-ray Binary Search for Non-Thermal Emission in a Quiescent Black-Hole X-ray Binary

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sptz.prop20669b&link_type=abstract

Spitzer Proposal ID #20669

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Scientific paper

Accretion flow in X-ray binaries, particularly during quiescence, has been claimed to produce evidence for the existence of event horizons (Garcia et al. 2001) and other direct tests of strong-field relativity (Cui, Zhang & Chen 1998). However, the basic physical processes are still poorly understood. Traditionally it has been thought that the quiescent flux is dominated by the secondary star. However, light curve models show that the secondary star alone cannot account for the quiescent flux. Flux from accretion disks have been included in such models, but these are not always successful in explaining the light curve morphology. Alternatively, some of the flux may be due to the presence of synchrotron emission which most likely originates from jets. If non-thermal emission is present in X-ray binaries during quiescence it may provide the best constraint on the quiescent accretion flow. This proposal seeks to observe a quiescent black-hole X-ray binary to determine if non-thermal emission is present.

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