On the Origin of Hard X-Ray Emissions from the Behind-the-limb Flare on 2014 September 1

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Date
2021
Volume
909
Issue
2
Journal
The astrophysical journal : an international review of spectroscopy and astronomical physics : Part 1
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Publisher
London : Institute of Physics Publ.
Abstract

The origin of hard X-rays and γ-rays emitted from the solar atmosphere during occulted solar flares is still debated. The hard X-ray emissions could come from flaring loop tops rising above the limb or coronal mass ejection shock waves, two by-products of energetic solar storms. For the shock scenario to work, accelerated particles must be released on magnetic field lines rooted on the visible disk and precipitate. We present a new Monte Carlo code that computes particle acceleration at shocks propagating along large coronal magnetic loops. A first implementation of the model is carried out for the 2014 September 1 event, and the modeled electron spectra are compared with those inferred from Fermi Gamma-ray Burst Monitor (GBM) measurements. When particle diffusion processes are invoked, our model can reproduce the hard electron spectra measured by GBM nearly 10 minutes after the estimated on-disk hard X-rays appear to have ceased from the flare site.

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Citation
Wu, Y., Rouillard, A. P., Kouloumvakos, A., Vainio, R., Afanasiev, A. N., Plotnikov, I., et al. (2021). On the Origin of Hard X-Ray Emissions from the Behind-the-limb Flare on 2014 September 1 (London : Institute of Physics Publ.). London : Institute of Physics Publ. https://doi.org//10.3847/1538-4357/abdc20
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CC BY 4.0 Unported