An energetic pre-flare
From RHESSI Wiki
Mbattaglia (Talk | contribs) |
Mbattaglia (Talk | contribs) (→Simultaenous fitting of RHESSI and AIA data) |
||
| Line 7: | Line 7: | ||
== Simultaenous fitting of RHESSI and AIA data == | == Simultaenous fitting of RHESSI and AIA data == | ||
| - | + | This idea of this method, developed by Motorina & Kontar 2015 [http://adsabs.harvard.edu/abs/2015Ge%26Ae..55..995M] | |
| - | + | ||
| - | + | ||
== The pre-impulsive phase of SOL2012-07-19T05:58 == | == The pre-impulsive phase of SOL2012-07-19T05:58 == | ||
Revision as of 09:35, 12 February 2019
Contents |
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]
