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Coronal X‐Ray Emission from the Stellar Companions to Transiently Accreting Black Holes
Observations of soft X-ray transients (SXTs) in quiescence have found that the binaries harboring black holes are fainter than those that contain a neutron star. Narayan and collaborators postulated that the faint X-ray emission from black hole binaries was powered by an advection dominated accretion flow (ADAF). We explore an alternative explanation for the quiescent X-ray emission from the black hole systems: coronal emission from the rapidly rotating optical companion. This is commonlydoi:10.1086/309464 fatcat:5bhxm7aksveorakcvgleqdvbs4