Electron Heating at SNR Collisionless Shocks

Details Electron Heating at SNR Collisionless Shocks Electron Heating at SNR Collisionless Shocks

Apr 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apjs..127..409l&link_type=abstract

The Astrophysical Journal Supplement Series, Volume 127, Issue 2, pp. 409-413.

Astronomy and Astrophysics

Astronomy

12

Shock Waves, Ism: Supernova Remnants

Scientific paper

The hot gas in supernova remnants is heated by collisionless shocks, generally propagating in low density (~1 atom cm-3 media), where the shock transition occurs on a length scale much shorter than the typical particle mean free path to Coulomb collisions. Conservation laws for energy, momentum, and particle numbers across the shock predict postshock particle temperatures proportional to their masses, that is, electron temperature << ion temperature. Electrons and ions will, of course, equilibrate by Coulomb collisions, but collisionless processes might bring about faster equilibration. I review theoretical and observational work on this important point and speculate on reasons for discrepancies where they exist.

Affiliated with

Also associated with

No associations

Rating

Electron Heating at SNR Collisionless Shocks does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Electron Heating at SNR Collisionless Shocks, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Electron Heating at SNR Collisionless Shocks will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-751634