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dc.contributor.authorZiebell, Luiz Fernandopt_BR
dc.contributor.authorYoon, Peter H.pt_BR
dc.contributor.authorGaelzer, Rudipt_BR
dc.contributor.authorPavan, Joelpt_BR
dc.date.accessioned2015-03-26T01:58:39Zpt_BR
dc.date.issued2014pt_BR
dc.identifier.issn0004-637Xpt_BR
dc.identifier.urihttp://hdl.handle.net/10183/114543pt_BR
dc.description.abstractThe plasma emission is the radiation mechanism responsible for solar type II and type III radio bursts. The first theory of plasma emission was put forth in the 1950s, but the rigorous demonstration of the process based upon first principles had been lacking. The present Letter reports the first complete numerical solution of electromagnetic weak turbulence equations. It is shown that the fundamental emission is dominant and unless the beam speed is substantially higher than the electron thermal speed, the harmonic emission is not likely to be generated. The present findings may be useful for validating reduced models and for interpreting particle-in-cell simulations.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofThe astrophysical journal. Bristol. Vol. 795, no. 2 (Nov. 2014), L32, 5 p.pt_BR
dc.rightsOpen Accessen
dc.subjectPlasmas astrofisicospt_BR
dc.subjectRadiation mechanisms: non-thermalen
dc.subjectSolar winden
dc.subjectSimulação de plasmaspt_BR
dc.subjectSun: radio radiationen
dc.subjectTurbulência em plasmaspt_BR
dc.subjectRadiação solar em radio-frequênciapt_BR
dc.subjectTurbulenceen
dc.titlePlasma emission by weak turbulence processespt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000955419pt_BR
dc.type.originEstrangeiropt_BR


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