TY - GEN

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.

UR - http://www.scopus.com/inward/record.url?scp=85069715604&partnerID=8YFLogxK

U2 - 10.1063/1.5117809

DO - 10.1063/1.5117809

M3 - Conference contribution

AN - SCOPUS:85069715604

T3 - AIP Conference Proceedings

BT - Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy

A2 - Li, Bao-An

A2 - Li, Ang

A2 - Xu, Furong

PB - American Institute of Physics Inc.

T2 - Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy 2019

Y2 - 3 January 2019 through 7 January 2019

ER -