Emissivity of Neutrinos in Supernova in a Left–right Symmetric Model

Abstract

We calculate the emissivity due to neutrino-pair production in e + e − annihilation in the context of a left-right symmetric model in a way that can be used in supernova calculations. We also present some simple estimates which show that such process can act as an efficient energy-loss mechanism in the shocked supernova core. We find that the emissivity is dependent of the mixing angle φ of the model in the allowed range for this parameter.

Role of neutrino form factors in the energy loss rates of the pair annihilation process

“…) are dominant, the bremstrahlung ( ) and recombination processes ( ) play a smaller role in astrophysics and cosmology. The energy loss rates of these processes have already been calculated at various temperature values and matter densities in different models [18][19][20][21][22][23][24][25][26][27][28][29].…”

The Role of the Neutrino Form Factors in the Energy Loss Rates of Pair Annihilation Process

“…While the three thermal neutrino processes which are plasmon decay (γ plasmon → ν e + ν e ), photo neutrino production (e − + γ → e − + ν e + ν e ) and pair annihilation (e − +e + → ν e +ν e ) are most dominant, the bremstrahlung (e − +Z → e − +Z +ν e +ν e ) and recombination processes (e − continuum → e − bound + ν e + ν e ) play smaller role in astrophysics and cosmology. The energy loss rate of these process has been already calculated at various values of the temperature and matter density for different model [18][19][20][21][22][23][24][25][26][27][28][29].…”

Stellar energy loss rates beyond the standard model

“…However although large values of temperatures and densities seems to characterize well the final stage of stellar evolution, the former are dominant. Under these conditions, we can identify four main mechanisms of neutrino pair production relevant for the neutrino luminosity [4][5][6][7][8][9][10][11]:…”