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Astron. Astrophys. 360, 575-582 (2000)

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

J.-P. Lasota

Institut d'Astrophysique de Paris, 98bis Boulevard Arago, 75014 Paris, France (lasota@iap.fr)

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

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© European Southern Observatory (ESO) 2000

Online publication: August 17, 2000