Adiabatic stellar core collapse - Propagation of the shock

Details Adiabatic stellar core collapse - Propagation of the shock Adiabatic stellar core collapse - Propagation of the shock

Sep 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...240..658v&link_type=abstract

Astrophysical Journal, Part 1, vol. 240, Sept. 1, 1980, p. 658-671.

Astronomy and Astrophysics

Astrophysics

16

Adiabatic Conditions, Gravitational Collapse, Shock Wave Propagation, Stellar Mass, Stellar Structure, Equations Of State, Stellar Models, Supernovae

Scientific paper

Lichtenstadt, Sack, and Bludman (1980) have pointed out the importance of thermal stiffness, the postshock adiabatic index which determines how much shock-dissipated energy goes into pressure, in determining whether or not core collapse of massive stars will result in an explosion. The present paper shows how the thermal stiffness enters into the equation of state and how it affects the shock propagation. The present numerical models confirm the findings of Lichtenstadt et al. that, with a large thermal stiffness, an explosion can occur without an inner core rebound following bounce. The effect of different inner core masses at bounce is examined and it is found that a smaller inner core, resulting from small decrease in the adiabatic index during infall, can nullify the explosive effects of a large thermal stiffness.

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