Accretion Disk Coronae

  • Max Kuperus
Part of the International Astronomical Union / Union Astronomique Internationale book series (IAUH, volume 8)

Summary

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 quasiperiodic oscillations respectively flare type emission.

Keywords

Black Hole Neutron Star Accretion Disk Rotate Neutron Star Open Field Line 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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References

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Copyright information

© International Astronomical Union 1989

Authors and Affiliations

  • Max Kuperus
    • 1
  1. 1.Sterrekundig InstituutUtrechtThe Netherlands

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