Physics – Plasma Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh22a..07k&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SH22A-07
Physics
Plasma Physics
[7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7807] Space Plasma Physics / Charged Particle Motion And Acceleration, [7811] Space Plasma Physics / Discontinuities
Scientific paper
Observations provide tight constraints on the temporal and spatial scales of particle heating and acceleration in solar flares, and on the required efficiency. Electrons are quickly heated beyond tens of keV, and while observational signatures for ion heating are difficult to come by, both are known to exhibit significant energetic tails reaching tens of MeV and above. Moreover, simple estimates indicate that virtually all available electrons are brought to moderately high energies, while electrons and ions share much of the magnetic energy released - pointing to a process resembling bulk heating rather than acceleration of a small or localized population. Recently, we proposed a two-stage process in which the counter-streaming ion beams of kinetic, low-beta reconnection are responsible for the primary ion heating to thermal speeds of approximately the Alfvén speed, and simultaneously contribute to the turbulence that leads to highly energetic ion tails, bulk electron heating, and electron tail generation. Here, we show details of the underlying linear mode properties, and discuss results of large-scale simulations that shed light on the temporal and spatial scales of acceleration into the MeV range and beyond.
Krauss-Varban Dietmar
Welsch Brian Thomas
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