The physics of stellar core collapse

Details The physics of stellar core collapse The physics of stellar core collapse

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988ap%26ss.143...15b&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 143, no. 1, April 1988, p. 15-44.

Physics

15

Energy Transfer, Gravitational Collapse, Relativistic Theory, Stellar Cores, Stellar Mass, Stellar Physics, Electron Capture, Electron Scattering, Equations Of State, High Energy Interactions

Scientific paper

The processes governing the hydrodynamics developing during the infall of the core of a massive star at the end of its hydrostatic evolutionary epoch are explored both semianalytically and numerically, with special attention given to the factors responsible for reducing the mass of the inner core. These factors are found to be mainly associated with the general relativistic effects and with the production, equilibration, and transport of electron neutrinos, nu(e)s. It is shown that the neutrino-electron scattering plays the dominant role in the matter-nu(e) equilibration, with the result that the equilibration is nearly complete by trapping. It is shown that, as a result of the processes examined, the inner core mass becomes greatly reduced by the time of core turn-around. However, it is noted that the effect of the small inner core mass on the subsequent dynamical history of the core is not known.

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