Equation of state effects in core-collapse supernovae. (arXiv:1812.02002v1 [nucl-th])

<a href="http://arxiv.org/find/nucl-th/1/au:+Yasin_H/0/1/0/all/0/1">Hannah Yasin</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Schafer_S/0/1/0/all/0/1">Sabrina Schäfer</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Arcones_A/0/1/0/all/0/1">Almudena Arcones</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Schwenk_A/0/1/0/all/0/1">Achim Schwenk</a>

We investigate the impact of different properties of the nuclear equation of

state in core-collapse supernovae, with a focus on the proto-neutron-star

contraction and its impact on the shock evolution. To this end, we introduce a

range of equations of state that vary the nucleon effective mass,

incompressibility, symmetry energy, and nuclear saturation point. This allows

us to point to the different effects in changing these properties from the

Lattimer and Swesty to the Shen et al. equations of state, the two most

commonly used equations of state in simulations. In particular, we trace the

contraction behavior to the effective mass, which determines the thermal

nucleonic contributions to the equation of state. Larger effective masses lead

to lower pressures at nuclear densities and a lower thermal index. This results

in a more rapid contraction of the proto-neutron star and consequently higher

neutrino energies, which aids the shock evolution to a faster explosion.

We investigate the impact of different properties of the nuclear equation of

state in core-collapse supernovae, with a focus on the proto-neutron-star

contraction and its impact on the shock evolution. To this end, we introduce a

range of equations of state that vary the nucleon effective mass,

incompressibility, symmetry energy, and nuclear saturation point. This allows

us to point to the different effects in changing these properties from the

Lattimer and Swesty to the Shen et al. equations of state, the two most

commonly used equations of state in simulations. In particular, we trace the

contraction behavior to the effective mass, which determines the thermal

nucleonic contributions to the equation of state. Larger effective masses lead

to lower pressures at nuclear densities and a lower thermal index. This results

in a more rapid contraction of the proto-neutron star and consequently higher

neutrino energies, which aids the shock evolution to a faster explosion.

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