Publikationsdatum:
2019-06-28
Beschreibung:
It is suggested that optically small gamma-ray flares result from gradual pre-flare acceleration of protons over approximately 1,000 s by a series of magnetohydrodynamic shocks in the low corona. A fraction of the accelerated protons are trapped in the corona where they form a seed population for future acceleration. If the shock acceleration is sufficiently rapid proton energies may exceed the gamma-ray production threshold and trigger gamma-ray emission. This occurs without the total flare energy being necessarily large. Magnetic field geometry is an important parameter.
Schlagwort(e):
SOLAR PHYSICS
Materialart:
SH-1.3-2
,
19th Intern. Cosmic Ray Conf - Vol. 4; p 82-85; NASA-CP-2376-VOL-4
Format:
application/pdf
