Solar flare particle heating via low-β reconnection

Details Solar flare particle heating via low-β reconnection Solar flare particle heating via low-β reconnection

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007hia....14...89k&link_type=abstract

Highlights of Astronomy, Volume 14, p. 89-89

Astronomy and Astrophysics

Astronomy

Solar Flares, Acceleration Of Particles

Scientific paper

Observations give tight constraints on the temporal and spatial scales of particle heating in solar flares, and on the required efficiency. Electrons are accelerated into a quasi-thermal population of a few tens of keV. X- and γ-rays imply tails in electron and ion distributions reaching tens of MeV and above. Simple estimates indicate that all available electrons are accelerated at least once to moderate energies, pointing to an initial process resembling bulk heating rather than acceleration of a small or localized population. In the absence of effective collisions, wave-particle interactions are the prime candidate. Here we address the outstanding questions, (i) what process can heat the entire reconnecting plasma to the above energies, and (ii) what provides the free energy for wave-particle interactions? We propose a process in which initially the ions are heated and provide the free energy for electron heating and tail formation.

Affiliated with

Also associated with

No associations

Rating

Solar flare particle heating via low-β reconnection 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 Solar flare particle heating via low-β reconnection, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Solar flare particle heating via low-β reconnection will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-974512