http://arxiv.org/abs/1511.02820
We present a new calculation of neutrino emissivities and energy spectra from a presupernova, a massive star going through the advanced stages of nuclear burning in the months before becoming a supernova. The contributions from beta decay and electron capture, pair annihilation, plasmon decay, and the photoneutrino process are modeled in detail, using updated tabulated nuclear rates. We also use realistic conditions of temperature, density, electron fraction and nuclear isotopic composition of the star from the state of the art stellar evolution code MESA. It is found that beta processes contribute substantially to the neutrino flux above realistic detection thresholds of few MeV, at selected positions and times in the evolution of the star.
K. Patton and C. Lunardini
Tue, 10 Nov 15
32/62
Comments: 15 pages, 4 figures
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