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

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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https://hal-insu.archives-ouvertes.fr/insu-03672451
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Submitted on : Thursday, May 19, 2022 - 12:27:57 PM
Last modification on : Monday, July 4, 2022 - 8:43:24 AM

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yihong Wu, Alexis P. Rouillard, Athanasios Kouloumvakos, Rami Vainio, Alexandr N. Afanasiev, et al.. On the Origin of Hard X-Ray Emissions from the Behind-the-limb Flare on 2014 September 1. The Astrophysical Journal, 2021, 909, ⟨10.3847/1538-4357/abdc20⟩. ⟨insu-03672451⟩

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