Neutrino flow and the collapse of stellar cores

Details Neutrino flow and the collapse of stellar cores Neutrino flow and the collapse of stellar cores

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975nyasa.262...54w&link_type=abstract

(AAS, American Physical Society, and New York Academy of Sciences, Texas Symposium on Relativistic Astrophysics, 7th, Dallas, Te

Astronomy and Astrophysics

Astrophysics

32

Gravitational Collapse, Heavy Nuclei, Neutrinos, Neutron Stars, Scattering Cross Sections, Stellar Cores, Baryons, Elastic Scattering, Electron Energy, Equations Of State, Graphs (Charts), Hot Stars, Stellar Envelopes, Stellar Mass Ejection

Scientific paper

Some preliminary calculations are made which show that a high heavy nucleus scattering cross section makes it possible for the hot neutron star newly formed in stellar collapse to emit enough neutrinos to blow off the iron envelope that would surround the star. In the capture of neutrinos by heavy nuclei, the emitted neutrinos are assumed to have an energy equal to the chemical potential of the electrons. Energy exchange between neutrinos and electrons from elastic scattering is treated by a Fokker-Planck-type equation. Nuclear scattering is assumed to have a cross section proportional to the square of the weight of the heavy nuclei.

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