HEAD 2003 Meeting
Session 20. Magnetars and Young Neutron Stars III
Poster, Sunday-Wednesday, March 23, 2003, Duration of Meeting

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[20.15] Relativistic Reconnection in Astrophysics

M. Lyutikov (McGill University, CITA)

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 \sigma \gg 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< \sigma) or non-relativistic (for S > \sigma), 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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Bulletin of the American Astronomical Society, 35#2
© 2003. The American Astronomical Soceity.