1. Seed Population for Particle Acceleration... Anywhere in the Universe Shock heating based on many factors: 1. 1. v shock : shock speed 2. 2.  Bn : magnetic field angle to shock normal 3. 3.  : ratio of thermal and magnetic pressure 4. 4. M A : Alfvenic mach number 5. 5. Mass to charge ratio 6. 6. Plasma waves/instabilities 7. 7. Compression ratio 8. 8. Equilibration between species: T e /T p Ions studied seem to vary by shock Mass proportional heating in Supernova Remnant (SNR) Greater than mass proportional heating in Interplanetary shocks

2. Decreasing heating with increasing beta Heating in collisionless shocks Higher M/Q more heating 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