The Pre-flare Phase: Key to Understanding Energy and Mass Transport in Flare Loops

Details The Pre-flare Phase: Key to Understanding Energy and Mass Transport in Flare Loops The Pre-flare Phase: Key to Understanding Energy and Mass Transport in Flare Loops

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.2.85b&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

In the classical solar flare scenario, the chromosphere is heated by an incident beam of supra-thermal electrons that were accelerated in the corona, then precipitated downward along the field lines of a magnetic loop. The hot chromospheric plasma expands and fills the magnetic loops. This process has been termed chromospheric evaporation. The classical scenario causes characteristic emission in soft- and hard X-rays, both from the corona and the chromosphere. The time evolution of this emission follows a specific pattern known as the Neupert effect.
Recent observations indicate that this scenario is only applicable for about half of the observed flares (Veronig et al. 2002). The early rise phase of many events is dominated by increasing soft X-ray emission up to minutes before the onset of the hard X-ray emission. This pre-heating clearly contradicts the classical Neupert scenario and indicates that other mechanisms of energy transport such as thermal conduction have to be at work. It also implies that the pre-flare energy release is dominated by heating, not acceleration. While energy transport by thermal conduction and subsequent chromospheric evaporation has been studied in some detail for the decay phase of solar flares, we present the first comprehensive study of the early phases of 4 pre-heating events. We analyze the time evolution of those events in imaging and spectroscopy using data from the RHESSI satellite and demonstrate how this can improve our understanding of heating and evaporation processes in coronal loops and the initiation of particle acceleration.

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