Efficient electron heating in relativistic shocks and gamma ray burst afterglow

Simple item page
dc.creatorGedalin, M.
dc.creatorBalikhin, M. A.
dc.creatorEichler, D.
dc.date2007-09-19
dc.date2007-12-01
dc.date.accessioned2026-07-07T11:19:25Z
dc.date.available2026-07-07T11:19:25Z
dc.descriptionElectrons in shocks are efficiently energized due to the cross-shock potential, which develops because of differential deflection of electrons and ions by the magnetic field in the shock front. The electron energization is necessarily accompanied by scattering and thermalization. The mechanism is efficient in both magnetized and non-magnetized relativistic electron-ion shocks. It is proposed that the synchrotron emission from the heated electrons in a layer of strongly enhanced magnetic field is responsible for gamma ray burst afterglows.
dc.descriptionrevtex4
dc.identifierhttps://arxiv.org/abs/0709.3097
dc.identifierhttp://arxiv.org/abs/0709.3097
dc.identifierPhys.Rev.E77:026403,2008
dc.identifierdoi:10.1103/PhysRevE.77.026403
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/193678
dc.subjectAstrophysics
dc.titleEfficient electron heating in relativistic shocks and gamma ray burst afterglow
dc.typetext

Files

Collections

arXiv