On the Origin of Hard X-Ray Emissions from the Behind-the-limb Flare on 2014 September 1
dc.bibliographicCitation.firstPage | 163 | |
dc.bibliographicCitation.issue | 2 | |
dc.bibliographicCitation.journalTitle | The astrophysical journal : an international review of spectroscopy and astronomical physics : Part 1 | eng |
dc.bibliographicCitation.volume | 909 | |
dc.contributor.author | Wu, Yihong | |
dc.contributor.author | Rouillard, Alexis P. | |
dc.contributor.author | Kouloumvakos, Athanasios | |
dc.contributor.author | Vainio, Rami | |
dc.contributor.author | Afanasiev, Alexandr N. | |
dc.contributor.author | Plotnikov, Illya | |
dc.contributor.author | Murphy, Ronald J. | |
dc.contributor.author | Mann, Gottfried J. | |
dc.contributor.author | Warmuth, Alexander | |
dc.date.accessioned | 2023-04-19T04:39:11Z | |
dc.date.available | 2023-04-19T04:39:11Z | |
dc.date.issued | 2021 | |
dc.description.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. | eng |
dc.description.version | publishedVersion | eng |
dc.identifier.uri | https://oa.tib.eu/renate/handle/123456789/12011 | |
dc.identifier.uri | http://dx.doi.org/10.34657/11044 | |
dc.language.iso | eng | |
dc.publisher | London : Institute of Physics Publ. | |
dc.relation.doi | https://doi.org/10.3847/1538-4357/abdc20 | |
dc.relation.essn | 1538-4357 | |
dc.relation.issn | 0004-637X | |
dc.rights.license | CC BY 4.0 Unported | |
dc.rights.uri | https://creativecommons.org/licenses/by/4.0 | |
dc.subject.ddc | 520 | |
dc.subject.other | Solar coronal mass ejection shocks | eng |
dc.subject.other | Solar x-ray emission | eng |
dc.subject.other | Solar particle emission | eng |
dc.subject.other | Solar electromagnetic emission | eng |
dc.title | On the Origin of Hard X-Ray Emissions from the Behind-the-limb Flare on 2014 September 1 | eng |
dc.type | Article | eng |
dc.type | Text | eng |
tib.accessRights | openAccess | |
wgl.contributor | AIP | |
wgl.subject | Physik | ger |
wgl.type | Zeitschriftenartikel | ger |
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