We review the purely leptonic neutrino emission processes, contributing to the energy loss rate of the stellar plasma. We perform a complete analysis up to the first order in the electromagnetic coupling constant. In particular the radiative electromagnetic corrections, at order α, to the process e + e - →νν at finite density and temperature have been computed. This process gives one of the main contributions to the cooling of stellar interior in the late stages of star evolution. As a result of the analysis we find that the corrections affect the energy loss rate, computed at tree level, by a factor (-4-1)% in the temperature and density region where the pair annihilation is the most efficient cooling mechanism. © 2003 Elsevier Science B.V. All rights reserved.
NEUTRINO ENERGY LOSS RATE IN A STELLAR PLASMA / Esposito, S.; Mangano, G.; Miele, Gennaro; Picardi, I.; Pisanti, Ofelia. - In: NUCLEAR PHYSICS. B. - ISSN 0550-3213. - 658:1-2(2003), pp. 217-253. [10.1016/S0550-3213(03)00151-2]
NEUTRINO ENERGY LOSS RATE IN A STELLAR PLASMA
ESPOSITO S.;MANGANO G.;MIELE, GENNARO;PICARDI I.;PISANTI, OFELIA
2003
Abstract
We review the purely leptonic neutrino emission processes, contributing to the energy loss rate of the stellar plasma. We perform a complete analysis up to the first order in the electromagnetic coupling constant. In particular the radiative electromagnetic corrections, at order α, to the process e + e - →νν at finite density and temperature have been computed. This process gives one of the main contributions to the cooling of stellar interior in the late stages of star evolution. As a result of the analysis we find that the corrections affect the energy loss rate, computed at tree level, by a factor (-4-1)% in the temperature and density region where the pair annihilation is the most efficient cooling mechanism. © 2003 Elsevier Science B.V. All rights reserved.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
