Electron Capture in Early Gravitational Collapse -- Nuclear Equation of State

Details Electron Capture in Early Gravitational Collapse -- Nuclear Equation of State Electron Capture in Early Gravitational Collapse -- Nuclear Equation of State

1997-07-19

arxiv.org/abs/astro-ph/9707218v1

Astronomy and Astrophysics

Astrophysics

4 pages + 1 page of figures. To be published in the Conference proceedings of "SN1987A: Ten years later", meeting held in Chil

Scientific paper

We present the spectra of pre trapping neutrinos emitted from a core collapse supernova (having main sequence masses 15 and 25 $M_{\sun}$) within 1 kpc which can be detected by terrestrial detectors. The neutrino spectrum depends on the abundance of nuclei and free protons which undergo electron capture which in turn is determined by nuclear properties of the stellar core. The ambient temperature in the early pre-trapping phase is not so high as to wipe out shell and pairing effects. We present results from Relativistic Mean Field (RMF) calculations, which we use to predict properties of the neutron rich nuclei which dominate the stellar composition at this stage of stellar collapse and compare the RMF results with the Baron et al (BCK) equation of state.

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