Simulating neutron stars with a flexible enthalpy-based equation of state parametrization in spectre
Creators
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1.
California Institute of Technology
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2.
University of New Hampshire
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3.
Cornell University
Abstract
Numerical simulations of neutron star mergers represent an essential step toward interpreting the full complexity of multimessenger observations and constraining the properties of supranuclear matter. Currently, simulations are limited by an array of factors, including computational performance and input physics uncertainties, such as the neutron star equation of state. In this work, we expand the range of nuclear phenomenology efficiently available to simulations by introducing a new analytic parametrization of cold, beta-equilibrated matter that is based on the relativistic enthalpy. We show that the new enthalpy parametrization can capture a range of nuclear behavior, including strong phase transitions. We implement the enthalpy parametrization in the spectre code, simulate isolated neutron stars, and compare performance to the commonly used spectral and polytropic parametrizations. We find comparable computational performance for nuclear models that are well represented by either parametrization, such as simple hadronic equations of state. We show that the enthalpy parametrization further allows us to simulate more complicated hadronic models or models with phase transitions that are inaccessible to current parametrizations.
Copyright and License
© 2023 American Physical Society.
Acknowledgement
I. L. thanks Tianqi Zhao for helpful conversations in preparing this manuscript. The authors thank Reed Essick, Ingo Tews, Phil Landry, and Achim Schwink for access to 𝜒-EFT conditioned Gaussian process draws. charm++/converse [48] was developed by the Parallel Programming Laboratory in the Department of Computer Science at the University of Illinois at Urbana-Champaign. This project made use of python libraries including scipy and numpy [121,122]. Figures were produced using matplotlib [123] and paraview [124]. Computations were performed with the Wheeler cluster at Caltech, which is supported by a grant from the Sherman Fairchild Foundation and Caltech. This work was supported in part by the Sherman Fairchild Foundation at Caltech and Cornell, as well as by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech and by NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell. I. L. and K. C. acknowledge support from the Department of Energy under Award No. DE-SC0023101. F. F. gratefully acknowledges support from the Department of Energy, Office of Science, Office of Nuclear Physics, under Contract No. DE-AC02-05CH11231, from NASA through Grant No. 80NSSC22K0719, and from the NSF through Grant No. AST-2107932. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants No. PHY-0757058 and No. PHY-0823459.
Files
PhysRevD.107.123017.pdf
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Additional details
Related works
- Is new version of
- Discussion Paper: arXiv:2301.13818 (arXiv)
Funding
- Sherman Fairchild Foundation
- California Institute of Technology
- National Science Foundation
- PHY-2011961
- National Science Foundation
- PHY-2011968
- National Science Foundation
- OAC-1931266
- National Science Foundation
- PHY-1912081
- National Science Foundation
- OAC-1931280
- United States Department of Energy
- DE-SC0023101
- United States Department of Energy
- DE-AC02-05CH11231
- National Aeronautics and Space Administration
- 80NSSC22K0719
- National Science Foundation
- AST-2107932
- National Science Foundation
- PHY-0757058
- National Science Foundation
- PHY-0823459
Dates
- Submitted
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2023-01-31
- Accepted
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2023-05-08