Hot and dense matter equation of state probability distributions for astrophysical simulations
Abstract
We add an ensemble of nuclei to the equation of state for homogeneous nucleonic matter to generate a new set of models suitable for astrophysical simulations of core-collapse supernovae and neutron star mergers. We implement empirical constraints from (i) nuclear mass measurements, (ii) proton-proton scattering phase shifts, and (iii) neutron star observations. Our model is also guided by microscopic many-body theory calculations based on realistic nuclear forces, including the zero-temperature neutron matter equation of state from quantum Monte Carlo simulations and thermal contributions to the free energy from finite-temperature many-body perturbation theory. We ensure that the parameters of our model can be varied while preserving thermodynamic consistency and the connection to experimental or observational data, thus providing a probability distribution of the astrophysical hot and dense matter equation of state. Furthermore, we compare our results with those obtained from other available equations of state. While our probability distributions indeed represent a large number of possible equations of state, we cannot yet claim to have fully explored all of the uncertainties, especially with regard to the structure of nuclei in the hot and dense medium.
- Authors:
-
[2];
- Univ. of Tennessee, Knoxville, TN (United States)
- Univ. of Tennessee, Knoxville, TN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
- Texas A & M Univ., College Station, TX (United States)
- Publication Date:
- Research Org.:
- Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), Nuclear Physics (NP); USDOE Office of Science (SC), Advanced Scientific Computing Research (ASCR). Scientific Discovery through Advanced Computing (SciDAC); National Science Foundation (NSF)
- OSTI Identifier:
- 1877461
- Grant/Contract Number:
- AC05-00OR22725; AC02-05CH11231; SC0018232; PHY1652199
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Physical Review. C
- Additional Journal Information:
- Journal Volume: 105; Journal Issue: 3; Journal ID: ISSN 2469-9985
- Publisher:
- American Physical Society (APS)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 73 NUCLEAR PHYSICS AND RADIATION PHYSICS; Asymmetric nuclear matter; Equations of state of nuclear matter; Nuclear astrophysics; Nuclear density functional theory; Symmetry energy
Citation Formats
Du, Xingfu, Steiner, Andrew W., and Holt, Jeremy W. Hot and dense matter equation of state probability distributions for astrophysical simulations. United States: N. p., 2022.
Web. doi:10.1103/physrevc.105.035803.
Du, Xingfu, Steiner, Andrew W., & Holt, Jeremy W. Hot and dense matter equation of state probability distributions for astrophysical simulations. United States. https://doi.org/10.1103/physrevc.105.035803
Du, Xingfu, Steiner, Andrew W., and Holt, Jeremy W. Mon .
"Hot and dense matter equation of state probability distributions for astrophysical simulations". United States. https://doi.org/10.1103/physrevc.105.035803. https://www.osti.gov/servlets/purl/1877461.
@article{osti_1877461,
title = {Hot and dense matter equation of state probability distributions for astrophysical simulations},
author = {Du, Xingfu and Steiner, Andrew W. and Holt, Jeremy W.},
abstractNote = {We add an ensemble of nuclei to the equation of state for homogeneous nucleonic matter to generate a new set of models suitable for astrophysical simulations of core-collapse supernovae and neutron star mergers. We implement empirical constraints from (i) nuclear mass measurements, (ii) proton-proton scattering phase shifts, and (iii) neutron star observations. Our model is also guided by microscopic many-body theory calculations based on realistic nuclear forces, including the zero-temperature neutron matter equation of state from quantum Monte Carlo simulations and thermal contributions to the free energy from finite-temperature many-body perturbation theory. We ensure that the parameters of our model can be varied while preserving thermodynamic consistency and the connection to experimental or observational data, thus providing a probability distribution of the astrophysical hot and dense matter equation of state. Furthermore, we compare our results with those obtained from other available equations of state. While our probability distributions indeed represent a large number of possible equations of state, we cannot yet claim to have fully explored all of the uncertainties, especially with regard to the structure of nuclei in the hot and dense medium.},
doi = {10.1103/physrevc.105.035803},
journal = {Physical Review. C},
number = 3,
volume = 105,
place = {United States},
year = {Mon Mar 14 00:00:00 EDT 2022},
month = {Mon Mar 14 00:00:00 EDT 2022}
}
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