Regularized Mean and Accelerated Electron Flux Spectra in Solar Flares Eduard P. Kontar University of Glasgow Michele Piana, Anna Maria Massone (INFM,

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Regularized Mean and Accelerated Electron Flux Spectra in Solar Flares Eduard P. Kontar University of Glasgow Michele Piana, Anna Maria Massone (INFM, UdR di Genova), A. Gordon Emslie (The University of Alabama in Huntsville), and John C. Brown (University of Glasgow) COSPAR, July 2004

From X-rays to electron spectrum To find an electron spectrum is to solve a least square problem: X-ray spectrum is a convolution of a electron flux and cross-section: COSPAR, July 2004 and contains valuable information on electron spectrum via a system of linear equations: where But this problem is ill-posed and has no unique solution ! Additional constraints are needed to find a meaningful solution

Tikhonov regularization (Tikhonov,1963) Constrained minimum problem can be solved using Lagrange multiplier method: COSPAR, July 2004 subject to The solution of this problem is well-behaved and unique ! The constraints naturally follow from the physics of the problem, For example, thick-target mean electron flux is related to injected spectrum (Brown and Emslie,1988): Leading to the following constraint:

Mean Electron Spectrum:2002-Apr-14 22:25 UT flare COSPAR, July 2004

Mean Electron Spectrum: Temporal evolution COSPAR, July 2004 Temporal evolution of the Regularized Mean Electron Spectrum (20s time intervals) RHESSI Lightcurves 3-12keV; 12-25keV; 25-50keV; keV

Accelerated (injected) Electron Spectrum COSPAR, July 2004 Temporal evolution of the Regularized Accelerated Electron Spectrum (20s time intervals) Accelerated (injected) electron spectrum for a thick-target model:

The gap in electron spectrum or albedo ? Electron spectral index Using regularization approach electron flux spectrum has been inferred (Piana, 2003) August 20, 2002 M-class flare at 8:26 UT shows very flat spectra (spectral index 1.2) in the range keV Monte-Carlo modelled albedo correction (Bai & Ramaty, 1978) Without correction the spectral index is too small to be explained by collisional losses COSPAR, July 2004

Conclusions Regularized inversion gives us model-independent (without assumptions on functional shape of the spectra) mean electron flux independent and can detect features not predicted by current models. Provides us with information about high energy part of the spectrum above maximum photon energy. In case of collisional transport of electrons, accelerated electron spectrum can be obtained.