Astronomy and Astrophysics – Astronomy
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640403p&link_type=abstract
American Astronomical Society, AAS Meeting #216, #404.03; Bulletin of the American Astronomical Society, Vol. 41, p.899
Astronomy and Astrophysics
Astronomy
Scientific paper
Hard X-ray (HXR) observations provide the most direct information on the spectrum of the accelerated electrons in solar flares. We describe a new method to obtain the accelerated electron spectra and determine some important parameters of the acceleration mechanism in the framework of the stochastic acceleration of particles by turbulence, which has been successful in explaining many observed features of high energy emission in solar flares. Our method relies on two new important advances. First, HXR observations by Yohkoh, and more recently by the Rueven Ramaty High Energy Solar Spectroscopic Imager (RHESSI), have demonstrated that electron acceleration takes place near the top of a flaring loop or the loop top (LT) source, which, like the more dominant foot point (FP) sources, has distinct nonthermal HXR emission. Second, recently Piana et al. (2007) have shown that the regularized inversion technique can be applied to the RHESSI data in the Fourier domain to obtain electron flux spectral images. We have shown that the resulting spatially resolved electron flux spectra at the LT and FPs can be used to constrain the acceleration model parameters directly. In particular, we obtain the accelerated electron spectra and derive the escape time from and the scattering time of electrons by turbulence in the acceleration region. Results from application of this method to several flares will be presented and their implication for the acceleration mechanism will be discussed.
Chen Qijin
Petrosian Vahe
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