Abstract
Neutrinos are the principle carriers of energy in massive stars, beginning from core carbon burning and continuing through core collapse and after the core bounce. In fact, it may be possible to detect neutrinos from nearby pre-supernova stars. Therefore, it is of great interest to understand the neutrino energy spectra from these stars. Leading up to core collapse, beginning around core silicon burning, nuclei become dominant producers of neutrinos, particularly at high neutrino energy, so a systematic study of nuclear neutrino spectra is desirable. We have done such a study, and we present our sd-shell model calculations of nuclear neutrino energy spectra for nuclei in the mass number range A = 21 – 35. Our study includes neutrinos produced by charged lepton capture, charged lepton emission, and neutral current nuclear deexcitation. Previous authors have tabulated the rates of charged current nuclear weak interactions in astrophysical conditions, but the present work expands on this not only by providing neutrino energy spectra, but also by including the heretofore untabulated neutral current de-excitation neutrino pairs.
Highlights
Neutrinos from nearby (
In the final phases before collapse, when the star begins to fuse silicon into iron, nuclei become the dominant sources of neutrinos, at high energy [4, 5]
Reference [5] presented expected presupernova neutrino spectra and detector signals from simulation results. They used the technique of reference [6] to compute the nuclear component of the spectra from published nuclear weak rate tables. This method consists of treating each nucleus at each temperature-density point as having a single transition from parent to daughter with an effective Q-value chosen to reproduce the published average neutrino energy
Summary
There has been recent work to produce realistic neutrino spectra from presupernova cores. In the final phases before collapse, when the star begins to fuse silicon into iron, nuclei become the dominant sources of neutrinos, at high energy [4, 5].
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