Bulletin of the American Physical Society
APS April Meeting 2011
Volume 56, Number 4
Saturday–Tuesday, April 30–May 3 2011; Anaheim, California
Session B6: Plasma Physics of Cosmic Rays in Galaxies |
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Sponsoring Units: DPP DAP Chair: Ellen Zweibel, University of Wisconsin-Madison Room: Terrace A-F |
Saturday, April 30, 2011 10:45AM - 11:21AM |
B6.00001: PIC Simulations of Cosmic Ray Acceleration Invited Speaker: |
Saturday, April 30, 2011 11:21AM - 11:57AM |
B6.00002: Cosmic Rays in Galaxies Invited Speaker: |
Saturday, April 30, 2011 11:57AM - 12:33PM |
B6.00003: Plasma Physics of Cosmic Ray Acceleration Invited Speaker: For more than 30 years, first-order Fermi particle acceleration in collisionless shocks has remained the mechanism of choice for producing cosmic rays and other superthermal particle populations in various astrophysical environments. The high efficiency, and therefore nonlinear nature, of the mechanism has presented challenges and surprises for modelers over the years and I will briefly describe some of these. In particular, I will focus on magnetic field amplification and particle escape; two phenomena that highlight the difficult plasma physics involved and which are undergoing active current research. While collisionless shocks, with associated particle acceleration, are believed to exist on scales from the Earth bow shock to galaxy clusters, supernova remnants (SNRs) offer perhaps the best place to study the mechanism. This is the case because several SNRs show extremely broadband continuum emission from radio to TeV gamma rays, sometimes accompanied with thermal X-ray emission. Other aspects, such as the morphology and observed evolution of some young remnants, offer unique clues to fundamental properties of the underlying plasma physics of both the remnant and the coupled acceleration mechanism. I will show how the consistent modeling of SNR observations can result in important constraints on the underlying acceleration mechanism. [Preview Abstract] |
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