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Seed Population for Particle Acceleration ... Anywhere in the Universe

Seed Population for Particle Acceleration ... Anywhere in the Universe. Shock heating based on many factors: v shock : shock speed  Bn : magnetic field angle to shock normal  : ratio of thermal and magnetic pressure M A : Alfvenic mach number Mass to charge ratio

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Seed Population for Particle Acceleration ... Anywhere in the Universe

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  1. Seed Population for Particle Acceleration ... Anywhere in the Universe Shock heating based on many factors: • vshock: shock speed • Bn: magnetic field angle to shock normal • : ratio of thermal and magnetic pressure • MA: Alfvenic mach number • Mass to charge ratio • Plasma waves/instabilities • Compression ratio • Equilibration between species: Te/Tp Ions studied seem to vary by shock • Mass proportional heating in Supernova Remnant (SNR) • Greater than mass proportional heating in Interplanetary shocks

  2. Heating in collisionless shocks Higher M/Q more heating Decreasing heating with increasing beta No apparent trend with Mach number

  3. Summary for heavy ion heating • Shock heating often has a strong M/Q dependence • Perpendicular shocks impart a larger fraction of energy to heavies • The heating rate does not depend on Mach number, but upstream proton  • Trends can be applied to other astrophysical shocks to predict magnetic field Would like to acknowledge ACE SWICS, MAG, SWEPAM. J. Raines for analysis support

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