Journal
ASTROPHYSICAL JOURNAL
Volume 735, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/735/2/103
Keywords
methods: numerical; Sun: corona; Sun: flares
Categories
Funding
- NASA [NNX09AB18G-R, NAG5-12820, NNM07AA02C]
- STFC [ST/H000429/1, PP/D002907/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/D002907/1, ST/H000429/1] Funding Source: researchfish
- UK Space Agency [ST/J001732/1] Funding Source: researchfish
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In this work, we model both the thermal and non-thermal components of solar flares. The model we use, HyLoop, combines a hydrodynamic equation solver with a non-thermal particle tracking code to simulate the thermal and non-thermal dynamics and emission of solar flares. In order to test the effects of pitch-angle distribution on flare dynamics and emission, a series of flares is simulated with non-thermal electron beams injected at the loop apex. The pitch-angle distribution of each beam is described by a single parameter and allowed to vary from flare to flare. We use the results of these simulations to generate synthetic hard and soft X-ray emissions (HXR and SXR). The light curves of the flares in Hinode's X-ray Telescope passbands show a distinct signal that is highly dependent on pitch-angle distribution. The simulated HXR emission in the 3-6 keV bandpass shows the formation and evolution of emission sources that correspond well to the observations of pre-impulsive flares. This ability to test theoretical models of thermal and non-thermal flare dynamics directly with observations allows for the investigation of a wide range of physical processes governing the evolution of solar flares. We find that the initial pitch-angle distribution of non-thermal particle populations has a profound effect on loop top HXR and SXR emission and that apparent motion of HXR is a natural consequence of non-thermal particle evolution in a magnetic trap.
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