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- W2105268719 abstract "Evolutionary sequences of stellar models that began with helium burning have been followed into the hydrodynamic phase of neutronization and thermal disintegration of nuclei. The thermal history is calculated with some care, and the rate of electron capture (and of other processes that change lepton number) is numerically integrated. The helium star (M/sub ..cap alpha../ = 8 M/sub mass/ which perhaps corresponds to a total mass of M = 24 M/sub solar/), develops a neutron star core (neutron/proton ratio approximately 50) that is hot (T approximately 5 x 10/sup 100/K at a density rho/sub c/ approx. = 1.0 x 10/sup 12/ g/cm/sup 3/). At the end of the last calculated time step, about 1.1 M/sub solar/ had accreted into the neutron star core, and although the core velocities were subsonic, a shock front had developed outside the neutronization region. 9 references. (auth)" @default.
- W2105268719 created "2016-06-24" @default.
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- W2105268719 date "1975-10-01" @default.
- W2105268719 modified "2023-09-27" @default.
- W2105268719 title "THE APPROACH TO GRAVITATIONAL COLLAPSE" @default.
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- W2105268719 doi "https://doi.org/10.1111/j.1749-6632.1975.tb31419.x" @default.
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