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Title: Equation of state effects in the core collapse of a 20 M star

Abstract

Uncertainties in our knowledge of the properties of dense matter near and above nuclear saturation density are among the main sources of variations in multimessenger signatures predicted for core-collapse supernovae (CCSNe) and the properties of neutron stars (NSs). We construct 97 new finite-temperature equations of state (EOSs) of dense matter that obey current experimental, observational, and theoretical constraints and discuss how systematic variations in the EOS parameters affect the properties of cold nonrotating NSs and the core collapse of a 20–M progenitor star. The core collapse of the 20–M progenitor star is simulated in spherical symmetry using the general-relativistic radiation-hydrodynamics code GR1D where neutrino interactions are computed for each EOS using the NuLib library. We conclude that the effective mass of nucleons at densities above nuclear saturation density is the largest source of uncertainty in the CCSN neutrino signal and dynamics even though it plays a subdominant role in most properties of cold NS matter. Meanwhile, changes in other observables affect the properties of cold NSs, while having little effect in CCSNe. To strengthen our conclusions, we perform six octant three-dimensional CCSN simulations varying the effective mass of nucleons at nuclear saturation density. Here, we conclude that neutrino heating and,more » thus, the likelihood of explosion is significantly increased for EOSs where the effective mass of nucleons at nuclear saturation density is large.« less

Authors:
ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [3]; ORCiD logo [4]
  1. Stockholm Univ. (Sweden); California Institute of Technology (CalTech), Pasadena, CA (United States)
  2. Michigan State Univ., East Lansing, MI (United States)
  3. OCS Labs LLC, Pasadena, CA (United States)
  4. Stockholm Univ. (Sweden)
Publication Date:
Research Org.:
Stockholm Univ. (Sweden); California Institute of Technology (CalTech), Pasadena, CA (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States); Univ. of California, Oakland, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC); National Science Foundation (NSF)
OSTI Identifier:
1604342
Grant/Contract Number:  
AC02-05CH11231; AST-1333520; PHY-1151197; PHY-1404569; OAC-1550514
Resource Type:
Accepted Manuscript
Journal Name:
Physical Review C
Additional Journal Information:
Journal Volume: 100; Journal Issue: 5; Journal ID: ISSN 2469-9985
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; 73 NUCLEAR PHYSICS AND RADIATION PHYSICS; nuclear matter; equation of state; core collapse; supernovae; neutron stars; equations of state of nuclear matter; novae & supernovae; nuclear astrophysics; nuclear matter in neutron stars; neutron stars & pulsars; astrophysical & cosmological simulations

Citation Formats

Schneider, Andre S., Roberts, L. F., Ott, C. D., and O'Connor, Evan. Equation of state effects in the core collapse of a 20–M⊙ star. United States: N. p., 2019. Web. doi:10.1103/PhysRevC.100.055802.
Schneider, Andre S., Roberts, L. F., Ott, C. D., & O'Connor, Evan. Equation of state effects in the core collapse of a 20–M⊙ star. United States. doi:https://doi.org/10.1103/PhysRevC.100.055802
Schneider, Andre S., Roberts, L. F., Ott, C. D., and O'Connor, Evan. Thu . "Equation of state effects in the core collapse of a 20–M⊙ star". United States. doi:https://doi.org/10.1103/PhysRevC.100.055802. https://www.osti.gov/servlets/purl/1604342.
@article{osti_1604342,
title = {Equation of state effects in the core collapse of a 20–M⊙ star},
author = {Schneider, Andre S. and Roberts, L. F. and Ott, C. D. and O'Connor, Evan},
abstractNote = {Uncertainties in our knowledge of the properties of dense matter near and above nuclear saturation density are among the main sources of variations in multimessenger signatures predicted for core-collapse supernovae (CCSNe) and the properties of neutron stars (NSs). We construct 97 new finite-temperature equations of state (EOSs) of dense matter that obey current experimental, observational, and theoretical constraints and discuss how systematic variations in the EOS parameters affect the properties of cold nonrotating NSs and the core collapse of a 20–M⊙ progenitor star. The core collapse of the 20–M⊙ progenitor star is simulated in spherical symmetry using the general-relativistic radiation-hydrodynamics code GR1D where neutrino interactions are computed for each EOS using the NuLib library. We conclude that the effective mass of nucleons at densities above nuclear saturation density is the largest source of uncertainty in the CCSN neutrino signal and dynamics even though it plays a subdominant role in most properties of cold NS matter. Meanwhile, changes in other observables affect the properties of cold NSs, while having little effect in CCSNe. To strengthen our conclusions, we perform six octant three-dimensional CCSN simulations varying the effective mass of nucleons at nuclear saturation density. Here, we conclude that neutrino heating and, thus, the likelihood of explosion is significantly increased for EOSs where the effective mass of nucleons at nuclear saturation density is large.},
doi = {10.1103/PhysRevC.100.055802},
journal = {Physical Review C},
number = 5,
volume = 100,
place = {United States},
year = {2019},
month = {11}
}

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