Physics
Scientific paper
May 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990cophr..12..275k&link_type=abstract
Comput. Phys. Rep., Vol. 12, No. 4, p. 275 - 287
Physics
5
Accretion Disks: Magnetohydrodynamics, Accretion Disks: Close Binaries, Accretion Disks: Compact Objects
Scientific paper
Accretion disks in close binary systems originate when mass overflow occurs from the primary star onto the compact star. When the compact star is a neutron star or a black hole the inner parts of the thin disk extend to the Alfvén radius respectively a few times the Schwarzschild radius. In the Keplerian rotating highly turbulent inner parts of the accretion disk magnetic fields are strongly amplified and expelled from the disk thus leading to the formation of a magnetically structured accretion disk corona. The magnetic energy supplied to the corona is radiated by inverse Compton scattering of soft X-ray photons produced in the disk by the viscous heating of the accreting matter. The interaction of the inner parts of an accretion disk with the magnetosphere around a neutron star leads to channeled accretion onto the magnetic poles, resulting in the phenomenon of X-ray pulsars. The interaction of disk coronal structures with the relatively weak magnetic fields of old fast spinning neutron stars leads to a new form of interaction around the so called beat frequency that can be used as a model for quasiperiodic oscillations in low-mass X-ray binaries.
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