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- W3021444531 abstract "Two neutron star evolution simulations are presented. The v e and v e transport is calculated with the Flux-limited Neutrino Diffusion Theory (FNDT) transport code[1, 2, 3]. The transport is spectral and monochromatic. The evolution of two protoneutron star models is simulated for 30 and 10 sec, respectively. In the first stellar model, without nuclei in its baryonic composition, the neutrino flows deposit a substantial amount of energy, about 3 1049 erg, during the first tenths of a second at matter densities around and below 5 1010 g cm -3. Initially, this causes the star to expand. In the second model nuclei are added to the composition of the star in the relevant regions to investigate the qualitative effect of the modified opacities on the deposition. It is found that the inclusion of nuclei impedes the expansion. Nevertheless, the energy deposition slows down the contraction of the atmosphere in both models considerably, and over many seconds. After about 1 sec a Rayleigh-Taylor unstable density inversion develops at the edge of the dense inner core at p ≈ 1013 g cm 3 in both models. This density inversion is unstable against convection as well. Both the energy deposition in the outer regions of the star and the density inversion at the edge of the inner core may have some effect on the working of the delayed-explosion mechanism [3]." @default.
- W3021444531 created "2020-05-13" @default.
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- W3021444531 date "1992-01-01" @default.
- W3021444531 modified "2023-09-27" @default.
- W3021444531 title "Neutrino driven neutron star formation." @default.
- W3021444531 hasPublicationYear "1992" @default.
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