Magnetic Reconnection in the Accretion Disk Corona of Compact Stars

Details Magnetic Reconnection in the Accretion Disk Corona of Compact Stars Magnetic Reconnection in the Accretion Disk Corona of Compact Stars

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aspc..289..315o&link_type=abstract

The Proceedings of the IAU 8th Asian-Pacific Regional Meeting, Volume I, held 2-5 July 2002 at National Center of Sciences, Hito

Astronomy and Astrophysics

Astronomy

Scientific paper

We present a new model of the magnetosphere for a compact star surrounded by an accretion disk. It is assumed that the magnetic axis of the star does not coincide with the rotation axis. The shape of the accretion disk, the magnetic field strength, and its gradient inside the disk corona are estimated. From these results, we describe an analytical model of a reconnecting current sheet and estimate its characteristics as well as the total power released by current sheets in the disk corona. It is shown that magnetic reconnection quantitatively explains the observed X-ray emission from compact stars.

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