Rate of energy-loss due to pair, plasma and photo neutrino processes in stellar environment

다국어 초록 (Multilingual Abstract)

Neutrinos are critical probes of many processes involved in stellar evolution. Stellar cores have the complex nuclear network, and at the end of helium burning, a star will enter an advanced stage of nuclear burning which proceeds at high temperature and density such that photons are no longer the dominant energy produced. The emission of neutrinos balances this energy generation by thermonuclear reactions at centres of massive stars. At lowest densities and temperature; the neutrino emission is strong, whereas, at high temperature, pair annihilation process dominates. In this work, the rate of neutrino energy-loss for stellar progenitor models of mass 15 M⊙, and 40 M⊙ both with and without rotation are computed and analysed. The variations in the evolution track of these models are responsible for diferent and independent values of thermal neutrino energy. As expected, the Pair. Photo and Plasma processes increase with temperature and density. In the 15 M⊙ model, the nuclei are fully ionised and the temperature increases to T ≥ 109 K such that pair neutrino possesses the highest value as compared to other processes We observed that thermal neutrino processes involving lesser temperature range are higher in 40 M⊙ rotating model. The plasma and photo energy loss as functions of density varies due to contraction of the stars.
The stars are contracted more with an increase in degrees of rotation, so also the neutrino energy loss difer as contraction causes change in range of densities. These fndings provides details about the heating and cooling of the models considered.

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