Other
Scientific paper
Mar 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.3801s&link_type=abstract
American Astronomical Society, HEAD meeting #10, #38.01
Other
Scientific paper
Collisionless shocks are an essential ingredient of the observed emission from nonthermal astrophysical sources. Such shocks are expected to produce and amplify magnetic fields, thermalize flow energy, and accelerate nonthermal electrons and cosmic rays. The physics of these processes remains to be clarified through both observations and theory. Supernova remnants are the prototypical laboratories for studying collisionless shocks for nonrelativistic flows. In cases where supernova remnants contain pulsar wind nebulae (PWN), highly relativistic shocks can be studied as well. I will present a summary of recent progress in theoretical modeling of collisionless shocks, focusing on the first-principles simulations of shocks using particle-in-cell codes. Such simulations allow self-consistent calculations of the structure of shocks and the generated turbulence. I will discuss the internal structure of the shocks in different regimes of magnetization and composition, concentrating on the conditions necessary for particle acceleration. I will present simulations which show ab-initio Fermi acceleration of particles from the thermal pool to powerlaw distributions, setting constraints on the shock acceleration efficiency and geometry. For relativistic shocks in PWN, the results imply the magnetic geometry in the shock region consistent with equatorial current sheet that underwent reconnection. Other shock simulation results that will be discussed include the amplification of upstream magnetic field by the accelerated particles through streaming instabilities, and the electron-ion temperature equilibration in relativistic and nonrelativistic shocks.
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