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X-rays from quiescent low-mass X-ray binary transients
Received 6 March 2000 / Accepted 15 June 2000
I argue that it is very unlikely that X-rays from quiescent black-hole low-mass X-ray binary transients are emitted by coronae of companion stars. I show that in a simple model in which these X-rays are emitted by an ADAF filling the inner part of an unsteady, dwarf-nova type disc, the X-ray luminosity is correlated with the orbital period. I predict what values of X-ray luminosities from black-hole transient systems should be observed by Chandra and XMM-Newton .
Key words: stars: binaries: close accretion, accretion disks instabilities X-rays: general
© European Southern Observatory (ESO) 2000
Online publication: August 17, 2000