Radiative corrections to neutrino energy loss rate in stellar interiors

Abstract

We consider radiative electromagnetic corrections, at order α, to the process $e^{+}{e}^{-}\to \nu \bar{\nu }$ at finite density and temperature. This process represents one of the main contributions to the cooling of stellar environments in the late stages of star evolution. We find that these corrections affect the energy loss rate by a factor $(-4÷1)$ with respect to the tree level estimate, in the temperature and density ranges where the neutrino pair production via e^+ e^- annihilation is the most efficient cooling mechanism.

arXiv commentLaTeX, 13 pages, 9 figure files; major revision due to a numerical error now corrected

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• Standard and Non-Standard Plasma Neutrino Emission Revisited
• Precision Rates for Nucleon Weak Interactions in Primordial Nucleosynthesis and He-4 Abundance
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• Emissivity of neutrinos in supernova in a left-right symmetric model
• Stellar energy loss rates in the pair-annihilation process beyond the standard model
• Neutrino Energy Loss Rates in 3-3-1 Models