X-rays from quiescent low-mass X-ray binary transients

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 s how that in a simple model in which these X-rays are emitted by an ADAF fil ling the inner part of an unsteady, dwarf-nova type disc, the X-ray luminos ity is correlated with the orbital period. I predict what values of X-ray l uminosities from black-hole transient systems should be observed by Chandra and XMM-Newton.