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dc.contributor.authorBirn, Joachim
dc.contributor.authorBattaglia, Marina
dc.contributor.authorFletcher, Lyndsay
dc.contributor.authorHesse, Michael
dc.contributor.authorNeukirch, Thomas
dc.date.accessioned2017-10-24T15:30:07Z
dc.date.available2017-10-24T15:30:07Z
dc.date.issued2017-10-20
dc.identifier.citationBirn , J , Battaglia , M , Fletcher , L , Hesse , M & Neukirch , T 2017 , ' Can substorm particle acceleration be applied to solar flares? ' , Astrophysical Journal , vol. 848 , no. 2 , 116 . https://doi.org/10.3847/1538-4357/aa8ad4en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 251204574
dc.identifier.otherPURE UUID: ca4b4260-425b-4552-9e72-1ab4a0d2ff5c
dc.identifier.otherScopus: 85032838627
dc.identifier.otherORCID: /0000-0002-7597-4980/work/38124085
dc.identifier.otherWOS: 000413339200016
dc.identifier.urihttp://hdl.handle.net/10023/11912
dc.description.abstractUsing test particle studies in the electromagnetic fields of three-dimensional magnetohydrodynamic (MHD) simulations of magnetic reconnection, we study the energization of charged particles in the context of the standard two-ribbon flare picture in analogy to the standard magnetospheric substorm paradigm. In particular, we investigate the effects of the collapsing field ("collapsing magnetic trap") below a reconnection site, which has been demonstrated to be the major acceleration mechanism that causes energetic particle acceleration and injections observed in Earth's magnetotail associated with substorms and other impulsive events. We contrast an initially force-free, high-shear field (low beta) with low and moderate shear, finite-pressure (high-beta) arcade structures, where beta represents the ratio between gas (plasma) and magnetic pressure. We demonstrate that the energization affects large numbers of particles, but the acceleration is modest in the presence of a significant shear field. Without incorporating loss mechanisms, the effect on particles at different energies is similar, akin to adiabatic heating, and thus is not a likely mechanism to generate a power-law tail onto a (heated or not heated) Maxwellian velocity distribution.
dc.format.extent14
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2017, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.3847/1538-4357/aa8ad4en
dc.subjectAcceleration of particlesen
dc.subjectSun: coronaen
dc.subjectSun: flaresen
dc.subjectSun: magnetic fieldsen
dc.subjectSun: particle emissionen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleCan substorm particle acceleration be applied to solar flares?en
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews.School of Mathematics and Statisticsen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aa8ad4
dc.description.statusPeer revieweden


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