Angular and energy distributions of energetic electrons in solar flares: results with RHESSI
Abstract
X-ray spectroscopy of solar flares is the key tool in diagnostics of high-energy particles in the low solar atmosphere However an observed X-ray spectrum is the convolution of radiation propagation effects as well as the instrumental response Specifically Compton back-scattering from the photosphere can account for 30-90 of the observed flux at energies 30-50 keV Starting with RHESSI Hard X-ray spectra and using recently developed inversion tools we compute the spectra of energetic electrons The angular and energy distribution of energetic electrons can be viewed as acceleration and propagation model fingerprints The electron spectra inferred from RHESSI solar flare spectra put new tighter observational constrains on possible acceleration propagation models
- Publication:
-
36th COSPAR Scientific Assembly
- Pub Date:
- 2006
- Bibcode:
- 2006cosp...36.1013K