X-ray spectra of Accretion Disk Coronae

Details X-ray spectra of Accretion Disk Coronae X-ray spectra of Accretion Disk Coronae

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.8803r&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #88.03; Bulletin of the American Astronomical Society, Vol. 32, p.1561

Astronomy and Astrophysics

Astronomy

Scientific paper

The CHANDRA and XMM satellites open up the possibility of detailed spectroscopy of Low Mass X-ray Binaries. Accretion disk coronae can be formed by photoionization and Compton heating by photons from near the neutron star, or the accretion flow may take the form of a low density Advection Dominated Accretion flow. In either case, a wind may drastically modify the structure. X-ray spectral lines and recombination contiua provide several clear signatures of different kinds of coronae.

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