Dense matter equation of state and neutron star properties from nuclear theory and experiment

Jeremy W. Holt; Yeunhwan Lim

doi:10.1063/1.5117809

Dense matter equation of state and neutron star properties from nuclear theory and experiment

Jeremy W. Holt, Yeunhwan Lim

Department of Physics

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

The equation of state of dense matter determines the structure of neutron stars, their typical radii, and maximum masses. Recent improvements in theoretical modeling of nuclear forces from the low-energy effective field theory of QCD has led to tighter constraints on the equation of state of neutron-rich matter at and somewhat above the densities of atomic nuclei, while the equation of state and composition of matter at high densities remains largely uncertain and open to a multitude of theoretical speculations. In the present work we review the latest advances in microscopic modeling of the nuclear equation of state and demonstrate how to consistently include also empirical nuclear data into a Bayesian posterior probability distribution for the model parameters. Derived bulk neutron star properties such as radii, moments of inertia, and tidal deformabilities are computed, and we discuss as well the limitations of our modeling.

Original language	English
Title of host publication	Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy
Editors	Bao-An Li, Ang Li, Furong Xu
Publisher	American Institute of Physics Inc.
ISBN (Electronic)	9780735418691
DOIs	https://doi.org/10.1063/1.5117809
Publication status	Published - 2019 Jul 17
Event	Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy 2019 - Xiamen, China Duration: 2019 Jan 3 → 2019 Jan 7

Publication series

Name	AIP Conference Proceedings
Volume	2127
ISSN (Print)	0094-243X
ISSN (Electronic)	1551-7616

Conference

Conference	Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy 2019
Country/Territory	China
City	Xiamen
Period	19/1/3 → 19/1/7

Bibliographical note

Funding Information:
Work supported by the National Science Foundation under grant No. PHY1652199. Portions of this research were conducted with the advanced computing resources provided by Texas A&M High Performance Research Computing.

Publisher Copyright:
© 2019 Author(s).

All Science Journal Classification (ASJC) codes

Physics and Astronomy(all)

Access to Document

10.1063/1.5117809

Cite this

Holt, J. W., & Lim, Y. (2019). Dense matter equation of state and neutron star properties from nuclear theory and experiment. In B-A. Li, A. Li, & F. Xu (Eds.), Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy [020019] (AIP Conference Proceedings; Vol. 2127). American Institute of Physics Inc.. https://doi.org/10.1063/1.5117809

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abstract = "The equation of state of dense matter determines the structure of neutron stars, their typical radii, and maximum masses. Recent improvements in theoretical modeling of nuclear forces from the low-energy effective field theory of QCD has led to tighter constraints on the equation of state of neutron-rich matter at and somewhat above the densities of atomic nuclei, while the equation of state and composition of matter at high densities remains largely uncertain and open to a multitude of theoretical speculations. In the present work we review the latest advances in microscopic modeling of the nuclear equation of state and demonstrate how to consistently include also empirical nuclear data into a Bayesian posterior probability distribution for the model parameters. Derived bulk neutron star properties such as radii, moments of inertia, and tidal deformabilities are computed, and we discuss as well the limitations of our modeling.",

author = "Holt, {Jeremy W.} and Yeunhwan Lim",

note = "Funding Information: Work supported by the National Science Foundation under grant No. PHY1652199. Portions of this research were conducted with the advanced computing resources provided by Texas A&M High Performance Research Computing. Publisher Copyright: {\textcopyright} 2019 Author(s).; Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy 2019 ; Conference date: 03-01-2019 Through 07-01-2019",

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doi = "10.1063/1.5117809",

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Holt, JW & Lim, Y 2019, Dense matter equation of state and neutron star properties from nuclear theory and experiment. in B-A Li, A Li & F Xu (eds), Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy., 020019, AIP Conference Proceedings, vol. 2127, American Institute of Physics Inc., Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy 2019, Xiamen, China, 19/1/3. https://doi.org/10.1063/1.5117809

Dense matter equation of state and neutron star properties from nuclear theory and experiment. / Holt, Jeremy W.; Lim, Yeunhwan.

Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy. ed. / Bao-An Li; Ang Li; Furong Xu. American Institute of Physics Inc., 2019. 020019 (AIP Conference Proceedings; Vol. 2127).

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

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T1 - Dense matter equation of state and neutron star properties from nuclear theory and experiment

AU - Holt, Jeremy W.

AU - Lim, Yeunhwan

N1 - Funding Information: Work supported by the National Science Foundation under grant No. PHY1652199. Portions of this research were conducted with the advanced computing resources provided by Texas A&M High Performance Research Computing. Publisher Copyright: © 2019 Author(s).

PY - 2019/7/17

Y1 - 2019/7/17

N2 - The equation of state of dense matter determines the structure of neutron stars, their typical radii, and maximum masses. Recent improvements in theoretical modeling of nuclear forces from the low-energy effective field theory of QCD has led to tighter constraints on the equation of state of neutron-rich matter at and somewhat above the densities of atomic nuclei, while the equation of state and composition of matter at high densities remains largely uncertain and open to a multitude of theoretical speculations. In the present work we review the latest advances in microscopic modeling of the nuclear equation of state and demonstrate how to consistently include also empirical nuclear data into a Bayesian posterior probability distribution for the model parameters. Derived bulk neutron star properties such as radii, moments of inertia, and tidal deformabilities are computed, and we discuss as well the limitations of our modeling.

AB - The equation of state of dense matter determines the structure of neutron stars, their typical radii, and maximum masses. Recent improvements in theoretical modeling of nuclear forces from the low-energy effective field theory of QCD has led to tighter constraints on the equation of state of neutron-rich matter at and somewhat above the densities of atomic nuclei, while the equation of state and composition of matter at high densities remains largely uncertain and open to a multitude of theoretical speculations. In the present work we review the latest advances in microscopic modeling of the nuclear equation of state and demonstrate how to consistently include also empirical nuclear data into a Bayesian posterior probability distribution for the model parameters. Derived bulk neutron star properties such as radii, moments of inertia, and tidal deformabilities are computed, and we discuss as well the limitations of our modeling.

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Dense matter equation of state and neutron star properties from nuclear theory and experiment

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Bibliographical note

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