Astronomy and Astrophysics – Astrophysics
Scientific paper
1997-04-24
(1997) ApJ, 484, L79
Astronomy and Astrophysics
Astrophysics
15 pages TeX and 2 .eps figures, accepted to Ap.J.Lett
Scientific paper
10.1086/310763
Observations show that magnetic reconnection and its slow shocks occur in solar flares. The basic magnetic structures are similar for long duration event (LDE) flares and faster compact impulsive (CI) flares, but the former require less non-thermal electrons than the latter. Slow shocks can produce the required non-thermal electron spectrum for CI flares by Fermi acceleration if electrons are injected with large enough energies to resonate with scattering waves. The dissipation region may provide the injection electrons, so the overall number of non-thermal electrons reaching the footpoints would depend on the size of the dissipation region and its distance from the chromosphere. In this picture, the LDE flares have converging inflows toward a dissipation region that spans a smaller overall length fraction than for CI flares. Bright loop-top X-ray spots in some CI flares can be attributed to particle trapping at fast shocks in the downstream flow, the presence of which is determined by the angle of the inflow field and velocity to the slow shocks.
No associations
LandOfFree
Distinguishing Solar Flare Types by Differences in Reconnection Regions 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 Distinguishing Solar Flare Types by Differences in Reconnection Regions, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Distinguishing Solar Flare Types by Differences in Reconnection Regions will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-268387