Reconnection Acceleration in Force Free Fields

Details Reconnection Acceleration in Force Free Fields Reconnection Acceleration in Force Free Fields

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..apr.p3004c&link_type=abstract

American Physical Society, April Meeting, 2003, April 5-8, 2003 Philadelphia, Pennsylvania, MEETING ID: APR03, abstract #P3.004

Physics

Scientific paper

The free energy in force-free fields, FFF, nabla × B = α B, in the low β intergalactic medium, IGM, is likely to be 10^6 larger than that within galaxies, as indicated by the synchrotron emission, SE from giant radio lobes, GRLs, and by SE and Faraday rotation in galaxy clusters. GRLs have minimum total energy (already close to galactic black hole energies) when the SE electrons, relativistic γ ˜ 10^5, have the same total energy as the FFF. These electrons alone then have more energy than the extra galactic cosmic rays, EGCRs, in the IGM. The lack of shocks at the boundaries of over pressured GRLs and the need for high acceleration efficiency suggests acceleration insitu from the reconnection of the FFF. The free energy of the FFF can only be converted to work by ot J_allel. Reconnection by an irreversible, non-linear instability, not yet fully understood, is the most likely explanation. Laboratory plasma experiments, e.g., interruptions, and simulations are contributing to understanding e acceleration. The typical CR power law spectrum results from a tangled field reconnection model where the fractional energy gain is proportional to a rigidity dependent fractional number loss of particles from the acceleration region by flux wandering. Supported by UC and the DOE.

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