Effects of equation of state on the outcome of stellar collapse

Details Effects of equation of state on the outcome of stellar collapse Effects of equation of state on the outcome of stellar collapse

May 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...237..903l&link_type=abstract

Astrophysical Journal, Part 1, vol. 237, May 1, 1980, p. 903-911.

Astronomy and Astrophysics

Astrophysics

28

Equations Of State, Gravitational Collapse, Hydrodynamics, Stellar Mass Ejection, Stellar Structure, Density Distribution, Neutrinos, Shock Waves, Stellar Temperature, Transport Properties

Scientific paper

The paper considers the adiabatic hydrodynamics of a collapsing stellar core, neglecting neutrino losses, so that hydrodynamic shocks are the only mechanism for entropy generation and possible mass ejection. Two mechanisms are distinguished depending on the thermal stiffness of the outer core and the strength of the reflected shock: (1) for reasonable values of the thermal stiffness of the outer core, shock heating can produce thermal pressure sufficient for mass ejection, and (2) if the thermal stiffness of the outer core is insufficient, mass ejection requires a large pressure deficit and an inner core soft enough to be deeply compressed, violently rebound, and oscillate. The efficiency of the shock heating mechanism depends on the low density incompressibility, the initial central density, and the density at which the cold equation of state stiffens; a soft outer core requires a large thermal stiffness to thermalize the rapid infall, but then leads to large mass ejection by shock heating.

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