Gravitational radiation from type-II supernovae: The effect of the high-density equation of state

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Abstract
Odd-parity gravitational perturbations of detailed spherically symmetric type-II supernova models, which include realistic equations of state and neutrino transport, are studied in the linearized Einstein theory. To investigate the parameters affecting gravitational-wave production during core collapse, we have performed simulations in which we vary the equation of state at supernuclear densities, the free proton mass fraction, and the precollapse iron core. These variations span much of the range of conditions currently thought to occur during stellar collapse and lead to the production of core-bounce shock waves that vary from the very strong to those that stall almost immediately. We find little difference in the gravitational radiation output among any of these models, though models that use stiffer equations of state or higher-mass iron cores give somewhat more radiation output.

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