Particle acceleration and the decay of soft X-ray non-thermal line broadcasting in solar flares

Details Particle acceleration and the decay of soft X-ray non-thermal line broadcasting in solar flares Particle acceleration and the decay of soft X-ray non-thermal line broadcasting in solar flares

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..154..157a&link_type=abstract

Solar Physics, vol. 154, no. 1, p. 157-175

Astronomy and Astrophysics

Astronomy

2

Gamma Ray Bursts, Gamma Ray Spectra, Line Shape, Line Spectra, Magnetohydrodynamic Turbulence, Mathematical Models, Nonthermal Radiation, Particle Acceleration, Solar Flares, Solar X-Rays, Wave-Particle Interactions, X Ray Astronomy, X Ray Spectra, Bessel Functions, Energy Distribution, Gamma Ray Spectrometers, Photosphere, Solar Atmosphere, Solar Magnetic Field, Solar Maximum Mission, Spectrum Analysis, X Ray Spectroscopy

Scientific paper

The relationship between the production of gamma-ray emitting particles and non-thermal soft X-ray line broadening is investigated. A model of particle acceleration via the stochastic interaction with magnetohydrodynamic (MHD) turbulence is assumed and the time development of the wave energy density derived under the condition of energy conservation between waves and particles. The inferred numbers and energy distribution of accelerated protons for four gamma-ray flares are used to define the wave energy density and its temporal development. The presence of Alfven wave turbulence is considered as the source of the non-thermal motions in the ambient plasma. These motions are observed as excess widths in the soft X-ray line emission from these events. The decay of the waves via the particle acceleration process is compared with the observed decays of this non-thermal line broadening. Our results show that both the gamma-ray emission and excess soft X-ray line widths in these flares can be explained by the single physical phenomenon of Alfven wave turbulence.

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