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Equation of state effects in core-collapse supernovae

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arxiv 1812.02002 v2 pith:MXVDMU7N submitted 2018-12-05 nucl-th astro-ph.HEnucl-ex

Hannah Yasin , Sabrina Schäfer , Almudena Arcones , Achim Schwenk This is my paper · ORCID
classification nucl-thastro-ph.HEnucl-ex
keywords statecontractioneffectiveequationequationsnuclearcore-collapsedifferent
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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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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. From Multimessenger Inference to Simulations: A Ranked Ensemble of Finite-Temperature Equations of State

    astro-ph.HE 2026-08 conditional novelty 7.0 of 10

    The paper constructs a 12-member ensemble of finite-temperature neutron star equations of state that spans the posterior from multimessenger and nuclear-physics constraints and releases simulation-ready tables.

  2. On the Nucleon Effective Mass in Neutron Stars Cooling

    hep-th 2026-07 conditional novelty 6.0 of 10

    Using the Landau instead of the Dirac effective nucleon mass in neutron-star cooling calculations cools massive stars faster, changing predicted surface temperatures by ~0.03–0.06 dex.

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