Relativistic Reconnection in Astrophysics

Details Relativistic Reconnection in Astrophysics Relativistic Reconnection in Astrophysics

Mar 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003head....7.2015l&link_type=abstract

American Astronomical Society, HEAD meeting #7, #20.15; Bulletin of the American Astronomical Society, Vol. 35, p.635

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We analyze the dynamics of the steady-state Sweet--Parker-type reconnection in relativistic regime when energy density in the inflowing region is dominated by magnetic field. The structure of reconnection layer (its thickness, inflow and outflow velocities) depends on the ratio of two large dimensionless parameters of the problem - magnetization parameter σ >> 1 (the ratio of the magnetic to particle energy-densities in the inflowing region) and the Lundquist number S. The inflow velocity may be relativistic (for S< σ ) or non-relativistic (for S > σ ), while the outflowing plasma is moving always relativisticly. Applications of relativistic reconnection to pulsar winds, AGNs, GRBs, and magnetars are discussed.

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