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Equation of State Effects in Core-Collapse Supernovae
H Yasin1, S Schäfer1,2, A Arcones1,3
1Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany.
Physical Review Letters
|March 24, 2020
Summary
Investigating nuclear equation of state properties reveals that larger nucleon effective masses accelerate proto-neutron-star contraction. This rapid contraction enhances neutrino energies, aiding core-collapse supernova shock evolution for faster explosions.
Area of Science:
- Nuclear Physics
- Astrophysics
- Computational Physics
Background:
- Core-collapse supernovae are crucial astrophysical events.
- The nuclear equation of state (EoS) governs supernova dynamics.
- Proto-neutron star contraction significantly impacts shock evolution.
Purpose of the Study:
- To investigate how variations in nuclear EoS properties affect core-collapse supernovae.
- To specifically analyze the influence on proto-neutron star contraction and shock evolution.
- To differentiate the effects of varying nucleon effective mass, incompressibility, symmetry energy, and nuclear saturation point.
Main Methods:
- Simulations using a range of nuclear equations of state.
- Comparison between Lattimer and Swesty EoS and Shen et al. EoS.
- Analysis of how specific EoS parameters influence proto-neutron star behavior.
Main Results:
- Nucleon effective mass is identified as a key factor in proto-neutron star contraction.
- Larger effective masses lead to lower pressures and a lower thermal index.
- This results in more rapid contraction and higher neutrino energies.
Conclusions:
- Variations in nuclear EoS properties, particularly effective mass, have a direct impact on supernova outcomes.
- Rapid proto-neutron star contraction driven by effective mass aids shock propagation.
- The study provides insights into mechanisms driving faster supernova explosions.
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