Neutrinos and supernova collapse

Details Neutrinos and supernova collapse Neutrinos and supernova collapse

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980stin...8115922c&link_type=abstract

Presented at the 1980 Intern. Dumand Symp., Honolulu, Hawaii, 24 Jul - 2 Aug. 1980

Physics

Gravitational Collapse, Neutrinos, Stellar Mass Ejection, Supernovae, Capture Effect, Electron Capture, Supernova Remnants

Scientific paper

The neutrino emission resulting from stellar collapse and supernova formation was reviewed. The electron capture and consequent neutronization of the collapsing stellar matter at the end of evolution determines both the initial adiabat of core collapse as well as the trapped lepton fraction. The initial lepton fraction, Y = .48 supplies the pressure for neutral support of the star at the Chandrasekhar limit. High trapping values, Y = .4, lead to soft core collapses, low values to harder collapses. The neutrino emission from initial electron capture is relatively small. A strong core-bounce shock releases both electron neutrinos as well as thermal neutrinos. Subsequent neutrino emission and cooling can sometimes lead to an unstable buoyancy gradient in the core in which case unstable core overturn is expected. Calculations showed the importance of the largest possible eddy or equivalently the lowest mode of overturn. Models of low lepton trapping ratio lead to high entropy creation by the reflected shock and the stabilization of the core matter against overturn.

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