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




TekijätWu Yihong, Rouillard Alexis P, Kouloumvakos Athanasios, Vainio Rami, Afanasiev Alexandr N, Plotnikov Illya, Murphy Ronald J, Mann Gottfried J, Warmuth Alexander

KustantajaIOP PUBLISHING LTD

Julkaisuvuosi2021

JournalAstrophysical Journal

Tietokannassa oleva lehden nimiASTROPHYSICAL JOURNAL

Lehden akronyymiASTROPHYS J

Artikkelin numeroARTN 163

Vuosikerta909

Numero2

Sivujen määrä16

ISSN0004-637X

DOIhttps://doi.org/10.3847/1538-4357/abdc20

Rinnakkaistallenteen osoitehttps://research.utu.fi/converis/portal/detail/Publication/55574206


Tiivistelmä
The origin of hard X-rays and gamma-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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Last updated on 2024-26-11 at 15:30