Affiliation:
1. School of Physical Science and Technology, Xinjiang University , Urumqi 830017 , China
2. Xinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi 830011 , China
Abstract
ABSTRACT
Neutrino losses play a crucial role in the evolution of massive stars. We study the neutrino luminosity of stars ranging from 20 to 90 $\rm M_{\odot }$ from Zero Age Main Sequence to Fe Core Collapse (FeCC) with different rotation and metallicity in a neutrino Hertzsprung–Russell diagram. In our simulations, we consider $\rm \omega /\omega _{crit}= 0$ and 0.7 to represent non-rotation and high rotation, respectively, and set the metallicities to 0.014, 0.001, and 0.0001. During hydrogen burning stages, neutrino luminosity primarily originates from CNO cycle, and increases with higher stellar mass while decreasing with increasing metallicity. For the high metallicity models (Z = 0.014) during the helium burning stage, the reduction of the hydrogen envelope caused by a larger mass loss rate leads to a gradual decrease in neutrino luminosity. The rapid rotation results in extra mixing inside massive stars, which increases the neutrino luminosity during main sequence, while decreases the neutrino luminosity during helium burning phase. Simultaneously, the rapid rotation also increases CO core mass, which enhances the neutrino luminosity during C and O burning phase. We also investigate the effect of neutrino magnetic moment (NMM) on the massive stars. We find that the energy loss caused by the NMM does not have effects on the evolutionary destiny of massive stars, and it does not significant change the compactness at the time of FeCC.
Funder
National Natural Science Foundation of China
Natural Science Foundation of Xinjiang Province
Publisher
Oxford University Press (OUP)
Subject
Space and Planetary Science,Astronomy and Astrophysics