An energetic pre-flare

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Introduction

How much energy is released in a flare? Which fractions of this energy are converted into accelerated particles and hot plasma, respectively. RHESSI observations have been used to answer these questions in many different ways - add a few references here - . While RHESSI observations have considerably improved our understanding of flare energetics, they have a limitation. Due to the typically steep power-law shape of the accelerated electron spectrum, the total energy is dominated by low energetic electrons, whose signatures are found at photon energies for which the interpretation of the spectrum can be ambiguous and/or to which RHESSI is not sensitive (Kontar et al. 2011, for a review). One way to overcome this, is to include data from SDO/AIA. This way, the lower energies are much better constrained. We used this method to analyze the pre-impulsive phase of the well known event SOL2012-07-19T05:58. Up to 20 minutes before the impulsive phase, two X-ray sources could be imaged, one below and one above what was interpreted as the magnetic reconnection region.

Simultaenous fitting of RHESSI and AIA data

This idea of this method, developed by Motorina & Kontar 2015 [1] is that any mean electron flux distribution can be described via a differential emission measure. And any observed count spectrum can be forward fitted with such a model. Hence, RHESSI and AIA data are combined into one dataset and a single temperature response matrix is computed. This combined data set is then forward fitted with a model DEM, where the chosen model is not any DEM, but it in fact represents the κ distribution. Figure 1: Illustration of the method of simultaneous RHESSI and AIA data fitting. In this case (see also ), two components (dark blue and green), one dominated by low-temperature emission from the corona and one dominated by flare emission

The pre-impulsive phase of SOL2012-07-19T05:58

This event presented something rarely seen with RHESSI: two HXR sources in the corona, one below and one above the presumed magnetic reconnection site. Both sources could be imaged over ~15 minutes during the pre-impulsive phase of the event, as shown in Figure 2. Using the method described above we analyzed the time evolution of the electron spectrum in both sources.

Figure 2: Overview of the event. On the top left, GOES and RHESSI lightcurves are shown and the analyzed time interval is indicated. An AIA 131 image it presented to the right with RHESSI contours (red: 7-8 keV, blue: 13-14 keV, yellow: 16-20 keV, green: 38-44 keV) overlaid. The bottom row shows the time evolution of the


Energy losses==

Conclusion

We show that considerable electron energization takes place in magnetic reconnection outflow regions up to 40 minutes before the peak of a solar flare. The spectrum of accelerated electrons in the magnetic reconnection outflows is consistent with a kappa-distribution with a power-law tail spectral index between −5 and −6 above 2 keV. The observations also show efficient heating of the reconnection outflows to temperatures of 6–8 MK, suggesting that the successful flare acceleration models should account for both heating and the formation of power-law tails. Both sources show time evolution at scales longer than the energy loss suggesting quasi-stationary energy release of energy. The dominant means of energy loss out of the acceleration region is by free-streaming, low energetic electrons. This not only implies that considerable electron acceleration can take place in flare phases other than the main, impulsive, flare phase, but also demonstrates the importance that the pre-impulsive phase plays in overall flare energetics.

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