Can a Single Reconnecting Current Sheet Model of a CME or a Flare Accelerate the Required Electron Fluxes Needed to Explain Non-Thermal X-ray Events Accompanying these Events?

Details Can a Single Reconnecting Current Sheet Model of a CME or a Flare Accelerate the Required Electron Fluxes Needed to Explain Non-Thermal X-ray Events Accompanying these Events? Can a Single Reconnecting Current Sheet Model of a CME or a Flare Accelerate the Required Electron Fluxes Needed to Explain Non-Thermal X-ray Events Accompanying these Events?

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aspc..415..435s&link_type=abstract

The Second Hinode Science Meeting: Beyond Discovery-Toward Understanding ASP Conference Series, Vol. 415, proceedings of a meeti

Astronomy and Astrophysics

Astronomy

Scientific paper

Non-thermal hard X-ray bursts are a common phenomena during solar flares and CME eruptions (Kane & Donnelly 1971; Lin & Hudson 1971; Brown 1971; Hudson & McKenzie 2001; Hudson 2002; Hudson et al. 2006). However, often overlooked are the number of non-thermal electrons needed to explain the observed hard X-rays and the substantial fraction of flare or CME energy carried by these electrons. Because the non-thermal electrons per sec required to produce the non-thermal hard X-ray bursts represents between ≈ 1.6× 1026 erg s-1 and 3.2× 1028 erg s-1-1 needed to explain the hard X-ray bursts and find the standard model incapable of producing the needed electron fluxes using reasonable solar parameters. We thus conclude that if the standard model is to maintain its usefulness an alternative mechanism(s) must accelerate the electrons. Various possibilities are considered.

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