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

Jeremy W. Holt, Yeunhwan Lim

Research output: Chapter in Book/Report/Conference proceedingConference contributionpeer-review

4 Scopus citations

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 languageEnglish
Title of host publicationXiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy
EditorsBao-An Li, Ang Li, Furong Xu
PublisherAmerican Institute of Physics Inc.
ISBN (Electronic)9780735418691
DOIs
StatePublished - 17 Jul 2019
EventXiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy 2019 - Xiamen, China
Duration: 3 Jan 20197 Jan 2019

Publication series

NameAIP Conference Proceedings
Volume2127
ISSN (Print)0094-243X
ISSN (Electronic)1551-7616

Conference

ConferenceXiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy 2019
Country/TerritoryChina
CityXiamen
Period3/01/197/01/19

Bibliographical note

Publisher Copyright:
© 2019 Author(s).

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