Flares in accretion disk coronae

Details Flares in accretion disk coronae Flares in accretion disk coronae

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003adspr..32.1087s&link_type=abstract

Advances in Space Research, Volume 32, Issue 6, p. 1087-1096.

Astronomy and Astrophysics

Astrophysics

8

Scientific paper

We discuss the possibility of applying the theory of large solar-type flares to astrophysical phenomena accompanied by fast plasma ejection, powerful fluxes of heat and radiation, impulsive acceleration of electrons and ions to high energies. A new analytical 2D model for a magnetosphere of a compact star with an accretion disk is constructed for a case when. the magnetic axis of the star does not coincide with the rotation axis. In the simplest approximation, this model allows us to estimate the value of magnetic field and its gradient in the corona of the disk. On the basis of these data, we use the well-tested models of a super-hot turbulent-current layer (SHTCL) to evaluate an ability to release a free magnetic energy from such layers in the accretion disk coronae. We conclude that the magnetic reconnection in accretion disk coronae is a powerful mechanism which may explain the observed transient X-ray emission from compact stars, in particular the neutron stars.

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