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Accretion Disk Coronae

Published online by Cambridge University Press:  14 August 2015

Max Kuperus
Max Kuperus*
Affiliation:
Sterrekundig Instituut, P.O. Box 80 000, 3508 TA Utrecht, The Netherlands

Summary

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Accretion disk coronae around compact objects are the result of strong magnetic activity in the inner regions of accretion disks. Part of the accreting energy is dissipated in te corona and can be observed as hard X-ray emission with a time variability caused by the coronal structures. The interaction of disk coronae with neutron stars and black holes may cause quaslperiodlc oscillations respectively flare type emission.

Type
Joint Commission Meeting
Information
Highlights of Astronomy , Volume 8: Highlights of Astronomy. As presented at the XXth General Assembly of the IAU, 1988 , 1989 , pp. 535 - 538
Copyright
Copyright © Kluwer 1989

References

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