Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999bha..proge...7b&link_type=abstract
Presented at the KITP Program: Black Hole Astrophysics, May 4, 1999, Kavli Institute for Theoretical Physics, University of Cali
Astronomy and Astrophysics
Astrophysics
Scientific paper
Magnetic reconnection describes the environment in which magneticenergy is dissipated into a combination of flow and particle energy in thepresence of a magnetic topology change. Here aspects of magnetic reconnectionphysicsand its role in astrophysical sources (solar flares, AGN) are addressed.Ways to enhance the rate , the generalized relativisticrate, as well as the particle acceleration processes occuring in reconnectionsites are presented. In general, nature seems to require fast reconnectionspeeds up to at least 0.1 V_A,but the energy conversion processes can vary widely from system to system.The presence or absence of slow shocks bounding inflows andoutflows and turbulence and/or fast shocksin the outflows play a role in determining how the magnetic energy is dissipatedinto particles and flow energy. The presence or absence of these likely dependon the various inflow boundary conditions and inflow parameters.Solar flares provide a good example of this. Reconnection and its slow shocksare a likely candidate for direct X-ray emission in Seyfert coronae.
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