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

Jul 8, 2021, 5:56 PM
4m
Virtual

Virtual

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Working Group 2: Particle acceleration Working Group 2: Particle acceleration

Speaker

Yihong Wu

Description

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.

Email yhwyihongwu@gmail.com

Primary author

Yihong Wu

Co-authors

Dr Alexis Rouillard (Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse III (UPS), France) Dr Athanasios Kouloumvakos (Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse III (UPS), France) Dr Rami Vainio (University of Turku, Turku, Finland) Dr Alexandr Afanasiev (University of Turku, Turku, Finland) Dr Illya Plotnikov (Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse III (UPS), France) Dr Ronald Murphy (Space Science Division, Naval Research Laboratory, Washington DC 20375, USA) Dr Gottfried Mann (Leibniz-Institut für Astrophysik Potsdam (AIP), Potsdam, Germany) Dr Alexander Warmuth (Leibniz-Institut für Astrophysik Potsdam (AIP), Potsdam, Germany)

Presentation materials