Use of RHESSI observations to determine the orign and the fate of non-thermal flare electrons

dc.creatorMachado, Marcos Emilio
dc.creatorMandrini, Cristina Hemilse
dc.date.accessioned2017-07-24T16:30:10Z
dc.date.accessioned2018-11-06T13:26:36Z
dc.date.available2017-07-24T16:30:10Z
dc.date.available2018-11-06T13:26:36Z
dc.date.created2017-07-24T16:30:10Z
dc.date.issued2004-12
dc.identifierMachado, Marcos Emilio; Mandrini, Cristina Hemilse; Use of RHESSI observations to determine the orign and the fate of non-thermal flare electrons; Elsevier; Advances in Space Research; 34; 2; 12-2004; 451-455
dc.identifier0273-1177
dc.identifierhttp://hdl.handle.net/11336/21156
dc.identifierCONICET Digital
dc.identifierCONICET
dc.identifier.urihttp://repositorioslatinoamericanos.uchile.cl/handle/2250/1875389
dc.description.abstractMost analyses of the characteristics of hard X-ray emission from solar flares have relied on observations of the spectral, temporal and spatial intensity distribution obtained by different instruments and, in the majority of cases, different events. The Reuven Ramaty High Energy Spectroscopic Imager gives us the possibility of combining all three fundamental parameters in a single set of observations from the same instrument. In this paper, we describe a method to compute the distribution of hard X-ray emission in flare loops, which can be used to determine the characteristics of electron energization, transport and thermalization during short lived impulsive peaks
dc.languageeng
dc.publisherElsevier
dc.relationinfo:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1016/j.asr.2004.01.007
dc.relationinfo:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0273117704000390
dc.rightshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.rightsinfo:eu-repo/semantics/restrictedAccess
dc.titleUse of RHESSI observations to determine the orign and the fate of non-thermal flare electrons
dc.typeArtículos de revistas
dc.typeArtículos de revistas
dc.typeArtículos de revistas


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