Accretion disk coronae and Cygnus X-1

Details Accretion disk coronae and Cygnus X-1 Accretion disk coronae and Cygnus X-1

Nov 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...218..247l&link_type=abstract

Astrophysical Journal, Part 1, vol. 218, Nov. 15, 1977, p. 247-252.

Astronomy and Astrophysics

Astrophysics

156

Binary Stars, Stellar Atmospheres, Stellar Mass Accretion, Stellar Winds, X Ray Stars, Energy Levels, Solar Corona, Stellar Mass Ejection, Stellar Models, Stellar Radiation

Scientific paper

It is plausible that an accretion disk pumps energy into an outer tenuous layer of its atmosphere to form a high-temperature corona analogous to the solar corona. General features of such a corona, not specific to any model, are discussed, and order-of-magnitude estimates are made for the physical parameters of a corona on the Cygnus X-1 disk. It is shown that a corona with a strong 'wind' (mass loss flux) can produce hard (exceeding 100 keV) X-rays if it is cooled by inverse Compton scattering. An observational test for the presence of such a corona is suggested.

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