The neutrino radiation for a hot neutron star formation and the envelope outburst problem

Details The neutrino radiation for a hot neutron star formation and the envelope outburst problem The neutrino radiation for a hot neutron star formation and the envelope outburst problem

Jan 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978ap%26ss..53..131n&link_type=abstract

Astrophysics and Space Science, vol. 53, no. 1, Jan. 1978, p. 131-153.

Astronomy and Astrophysics

Astronomy

53

Gravitational Collapse, Light Curve, Neutrinos, Neutron Stars, Star Formation, Stellar Envelopes, Black Holes (Astronomy), Coherent Scattering, Scattering Cross Sections, Stellar Luminosity

Scientific paper

Through use of the equations of neutrino heat conductivity, the neutrino light curve is calculated for the spherically symmetrical collapse of an iron-oxygen star of two solar masses up to the formation of a hot hydrostatically equilibrium neutron star. The total energy, radiated in the form of muon and electron neutrinos, is 5.8 times 10 to the 53rd power ergs. The mean neutrino particle energy is about 12 MeV for all the time the collapse proceeds. The maximum neutrino luminosity value is equal to 3 times 10 to the 53rd power ergs/sec. For the collapse of a star of 10 solar masses, the luminosity maximum takes place at the moment of the formation of a black hole inside the collapsing star. The set of calculations, allowing for the deposition of momentum by means of neutrino-nuclear coherent scattering, leads to the conclusion that the envelope outburst is only possible if the scattering cross-section is 50 times larger than the value experimentally accepted.

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