How to Scale Physical Processes Inside Collisionless Shocks in Astrophysics vs Solar Wind Shocks

Details How to Scale Physical Processes Inside Collisionless Shocks in Astrophysics vs Solar Wind Shocks How to Scale Physical Processes Inside Collisionless Shocks in Astrophysics vs Solar Wind Shocks

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh52a..01s&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH52A-01

Astronomy and Astrophysics

Astrophysics

7845 Particle Acceleration, 7851 Shock Waves (4455), 7867 Wave/Particle Interactions (2483, 6984)

Scientific paper

Growing pool of in-situ data on collisionless shocks in solar wind plasmas strongly suggests a comparative analysis of the data with largely hypothetical models of astrophysical shocks, e.g. galactic Supernova cosmic ray shocks. Despite tremendous difference in the energy content the scaling parameters when applied in high-beta limit (at least in downstream) shows a remarkable analogy of plasma turbulence and particle acceleration processes in both limits. Thus solar wind case study may serve as a valuable testbed to validate the astrophysical models.

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