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Impulsive and Long Duration High-Energy Gamma-ray Emission From the Very Bright 2012 March 7 Solar Flares

dc.contributor.authorAJELLO, Marco
dc.contributor.authorALBERT, A.
dc.contributor.authorALLAFORT, A.
dc.contributor.authorBALDINI, Luca
dc.contributor.authorBARBIELLINI, Guido
dc.contributor.authorBASTIERI, D.
dc.contributor.authorBELLAZZINI, R.
dc.contributor.authorBISSALDI, E.
dc.contributor.authorBONAMENTE, E.
dc.contributor.authorJ. BRANDT, T.
dc.contributor.authorBREGEON, J.
dc.contributor.authorBRIGIDA, M.
hal.structure.identifierLaboratoire Leprince-Ringuet [LLR]
dc.contributor.authorBRUEL, Pascal
dc.contributor.authorBUEHLER, R.
dc.contributor.authorBUSON, S.
dc.contributor.authorA. CALIANDRO, G.
dc.contributor.authorA. CAMERON, R.
dc.contributor.authorCARAVEO, P. A.
dc.contributor.authorCECCHI, C.
dc.contributor.authorCHARLES, E.
dc.contributor.authorCHEKHTMAN, A.
dc.contributor.authorCHIANG, J.
dc.contributor.authorCHIARO, G.
dc.contributor.authorCIPRINI, S.
dc.contributor.authorCLAUS, R.
hal.structure.identifierLaboratoire Univers et Particules de Montpellier [LUPM]
dc.contributor.authorCOHEN-TANUGI, J.
dc.contributor.authorCONRAD, J.
dc.contributor.authorD'AMMANDO, F.
dc.contributor.authorDE PALMA, F.
dc.contributor.authorD. DERMER, C.
dc.contributor.authorDO COUTO E SILVA, E.
dc.contributor.authorS. DRELL, P.
dc.contributor.authorDRLICA-WAGNER, A.
dc.contributor.authorFAVUZZI, C.
dc.contributor.authorB. FOCKE, W.
dc.contributor.authorFRANCKOWIAK, A.
dc.contributor.authorFUKAZAWA, Y.
dc.contributor.authorGARGANO, F.
dc.contributor.authorGASPARRINI, D.
dc.contributor.authorGERMANI, S.
dc.contributor.authorGIGLIETTO, N.
dc.contributor.authorGIOMMI, P.
dc.contributor.authorGIORDANO, F.
dc.contributor.authorGIROLETTI, M.
dc.contributor.authorGLANZMAN, T.
dc.contributor.authorGODFREY, G.
dc.contributor.authorE. GROVE, J.
dc.contributor.authorHADASCH, D.
dc.contributor.authorHAYASHIDA, M.
hal.structure.identifierLaboratoire Leprince-Ringuet [LLR]
dc.contributor.authorHORAN, D.
dc.contributor.authorINOUE, Y.
dc.contributor.authorS. JACKSON, M.
dc.contributor.authorJOGLER, T.
dc.contributor.authoŕ OHANNESSON, G.J
hal.structure.identifierInstitut de recherche en astrophysique et planétologie [IRAP]
dc.contributor.authorKNÖDLSEDER, Jürgen
dc.contributor.authorKOCEVSKI, D.
dc.contributor.authorLATRONICO, L.
dc.contributor.authorLOPARCO, F.
dc.contributor.authorLOVELLETTE, N.
dc.contributor.authorLUBRANO, P.
dc.contributor.authorMAYER, M.
dc.contributor.authorN. MAZZIOTTA, M.
dc.contributor.authorF. MICHELSON, P.
dc.contributor.authorMIZUNO, T.
dc.contributor.authorA. MOISEEV, A.
dc.contributor.authorE. MONZANI, M.
dc.contributor.authorMORSELLI, A.
dc.contributor.authorV. MOSKALENKO, I.
dc.contributor.authorMURGIA, S.
dc.contributor.authorMURPHY, R.
dc.contributor.authorNAKAMORI, T.
dc.contributor.authorNEMMEN, R.
dc.contributor.authorOHNO, M.
dc.contributor.authorOHSUGI, T.
dc.contributor.authorOMODEI, N.
dc.contributor.authorORIENTI, M.
dc.contributor.authorORLANDO, E.
dc.contributor.authorPANEQUE, D.
dc.contributor.authorH. PANETTA, J.
dc.contributor.authorS. PERKINS, J.
dc.contributor.authorPESCE-ROLLINS, M.
dc.contributor.authorPETROSIAN, V.
hal.structure.identifierLaboratoire Univers et Particules de Montpellier [LUPM]
dc.contributor.authorPIRON, F.
dc.contributor.authorPIVATO, G.
dc.contributor.authorPORTER, T.A.
dc.contributor.authorRAIN ' O, S.
dc.contributor.authorRANDO, R.
dc.contributor.authorRAZZANO, M.
dc.contributor.authorROTH, M.
dc.contributor.authorSCHULZ, A.
dc.contributor.authorSGRO, C.
dc.contributor.authorSPANDRE, G.
dc.contributor.authorSPINELLI, P.
dc.contributor.authorTAKAHASHI, H.
dc.contributor.authorG. THAYER, J.
dc.contributor.authorB. THAYER, J.
dc.contributor.authorJ. THOMPSON, D.
dc.contributor.authorTIBALDO, L.
dc.contributor.authorTINIVELLA, M.
dc.contributor.authorTOSTI, G.
dc.contributor.authorVANDENBROUCKE, J.
hal.structure.identifierLaboratoire Univers et Particules de Montpellier [LUPM]
dc.contributor.authorVASILEIOU, V.
dc.contributor.authorVIANELLO, G.
dc.contributor.authorVITALE, V.
dc.contributor.authorWERNER, M.
dc.contributor.authorYANG, Z.
hal.structure.identifierCentre d'Etudes Nucléaires de Bordeaux Gradignan [CENBG]
dc.contributor.authorHOU, X.
hal.structure.identifierCentre d'Etudes Nucléaires de Bordeaux Gradignan [CENBG]
dc.contributor.authorLOTT, B.
hal.structure.identifierLaboratoire Univers et Particules de Montpellier [LUPM]
dc.contributor.authorNUSS, E.
dc.date.issued2014
dc.identifier.issn0004-637X
dc.description.abstractEnThe Fermi Large Area Telescope (LAT) observed two bright X-class solar ares on 2012 March 7, and detected gamma-rays up to 4 GeV. We detected gamma-rays both during the impulsive and temporally-extended emission phases, with emission above 100 MeV lasting for approximately 20 hours. Accurate localization of the gamma-ray production site(s) coincide with the solar active region from which X-ray emissions associated with these ares originated. Our analysis of the > 100 MeV gamma-ray emission shows a relatively rapid monotonic decrease in ux during the rst hour of the impulsive phase, and a much slower, almost monotonic decrease in ux for the next 20 hours. The spectra can be adequately described by a power law with a high energy exponential cuto , or as resulting from the decay of neutral pions produced by accelerated protons and ions with an isotropic power-law energy distribution. The required proton spectrum has a number index 3, with minor variations during the impulsive phase, while during the temporally extended phase the spectrum softens monotonically, starting with index 4. The > 30 MeV proton ux and spectra observed near the Earth by the GOES satellites also show a monotonic ux decrease and spectral softening during the extended phase, but with a harder spectrum, with index 3. Based on the Fermi -LAT and GOES observations of the ux and spectral evolution of these bright ares, we explore the relative merits of prompt and continuous acceleration scenarios, hadronic and leptonic emission processes, and acceleration at the solar corona by the fast Coronal Mass Ejections (CME) as explanations for the observations. We conclude that the most likely scenario is continuous acceleration of protons in the solar corona which penetrate the lower solar atmosphere and produce pions that decay into gamma-rays.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subjectSun: X-rays
dc.subjectSun: flares
dc.subjectgamma rays
dc.title.enImpulsive and Long Duration High-Energy Gamma-ray Emission From the Very Bright 2012 March 7 Solar Flares
dc.typeArticle de revue
dc.identifier.doi10.1088/0004-637X/789/1/20
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Phénomènes cosmiques de haute energie [astro-ph.HE]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Phénomènes cosmiques de haute energie [astro-ph.HE]
dc.identifier.arxiv1304.5559
bordeaux.journalThe Astrophysical Journal
bordeaux.page20
bordeaux.volume789
bordeaux.peerReviewedoui
hal.identifierin2p3-01071503
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//in2p3-01071503v1
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