Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992phdt........10m&link_type=abstract
Ph.D. Thesis Tel-Aviv Univ. (Israel).
Astronomy and Astrophysics
Astronomy
Accretion Disks, Astronomical Photometry, Early Stars, Flare Stars, Massive Stars, Neutron Stars, Variable Stars, X Ray Binaries, Black Holes (Astronomy), Celestial Mechanics, Roche Limit, Spectroscopy, Stellar Luminosity, Stellar Spectra, X Ray Telescopes
Scientific paper
Massive X-ray binaries comprise a neutron star or black hole and an early-type star; their X-radiation is generated by the accretion of matter from the early-type star onto its companion. The X-ray spectra of such systems is usually hard, with exponentially fitted kT values exceeding about 15 keV. In many cases, the X-ray emission is pulsed, owing to the funneling of accreted matter towards the magnetic poles of the neutron star, whose magnetic axis is not aligned with its rotation axis. The systems are divided into two groups according to the luminosity class of the massive star: supergiant X-ray binaries (SXRB), with a spectral type earlier than B2; and Be X-ray binaries. The optical radiation of the system is dominated by the early-type star. Seven systems which could be readily observed from the Wise Observatory were monitored photometrically in the U, B, V, R, and I bands and in the Halpha radiation. The aim was to seek correlations between the changes in the X-ray and in the optical radiation and to detect long-term changes in system luminosities and orbital periods. The main conclusion is that a permanent or transient accretion disk may exist in Be binaries; a permanent disk may be associated with a highly eccentric system in which Roche-lobe overflows recur around periastron, or in close systems in which the neutron star moves within the flattened envelope of the Be star; a transient disk may form in large systems during the active phases of the Be star, when a large amount of matter is ejected from it.
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