Seed Population for Particle Acceleration ... Anywhere in the Universe
3
Seed Population for Particle Acceleration ... Anywhere in the Universe Shock heating based on many factors: 1. v shock : shock speed 2. Bn : magnetic field angle to shock normal 3. : ratio of thermal and magnetic pressure 4. M A : Alfvenic mach number 5. Mass to charge ratio 6. Plasma waves/instabilities 7. Compression ratio 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
description
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 - PowerPoint PPT Presentation
Transcript of Seed Population for Particle Acceleration ... Anywhere in the Universe
Seed Population for Particle Acceleration ... Anywhere in the Universe
Shock heating based on many factors:1. vshock: shock speed2. Bn: magnetic field angle to shock
normal3. : ratio of thermal and magnetic
pressure4. MA: Alfvenic mach number5. Mass to charge ratio6. Plasma waves/instabilities7. Compression ratio8. Equilibration between species: Te/Tp
Ions studied seem to vary by shockMass proportional heating in Supernova Remnant (SNR)Greater than mass proportional heating in Interplanetary shocks
Decreasing heating with increasing beta
Heating in collisionless shocks
Higher M/Q more heating
No apparent trend with Mach
number
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
