TY - JOUR

T1 - Neutron Star Radii, Deformabilities, and Moments of Inertia from Experimental and Ab Initio Theory Constraints of the 208Pb Neutron Skin Thickness

AU - Lim, Yeunhwan

AU - Holt, Jeremy W.

N1 - Funding Information:
This research was funded by Ewha Womans University Research Grant of 2021(1-2021-0520-001-1), the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIT) (No. 2021R1A2C2094378), the US National Science Foundation Grant No. PHY1652199 and the U.S. Department of Energy National Nuclear Security Administration Grant No. DE-NA0003841.
Publisher Copyright:
© 2022 by the authors.

PY - 2022/10

Y1 - 2022/10

N2 - Recent experimental and ab initio theory investigations of the (Formula presented.) Pb neutron skin thickness have the potential to inform the neutron star equation of state. In particular, the strong correlation between the (Formula presented.) Pb neutron skin thickness and the pressure of neutron matter at normal nuclear densities leads to modified predictions for the radii, tidal deformabilities, and moments of inertia of typical (Formula presented.) neutron stars. In the present work, we study the relative impact of these recent analyses of the (Formula presented.) Pb neutron skin thickness on bulk properties of neutron stars within a Bayesian statistical analysis. Two models for the equation of state prior are employed in order to highlight the role of the highly uncertain high-density equation of state. From our combined Bayesian analysis of nuclear theory, nuclear experiment, and observational constraints on the dense matter equation of state, we find at the 90% credibility level (Formula presented.) km for the radius of a (Formula presented.) neutron star, (Formula presented.) km for the radius of a (Formula presented.) neutron star, (Formula presented.) for the tidal deformability of a (Formula presented.) neutron star, and (Formula presented.) for the moment of inertia of PSR J0737-3039A whose mass is (Formula presented.).

AB - Recent experimental and ab initio theory investigations of the (Formula presented.) Pb neutron skin thickness have the potential to inform the neutron star equation of state. In particular, the strong correlation between the (Formula presented.) Pb neutron skin thickness and the pressure of neutron matter at normal nuclear densities leads to modified predictions for the radii, tidal deformabilities, and moments of inertia of typical (Formula presented.) neutron stars. In the present work, we study the relative impact of these recent analyses of the (Formula presented.) Pb neutron skin thickness on bulk properties of neutron stars within a Bayesian statistical analysis. Two models for the equation of state prior are employed in order to highlight the role of the highly uncertain high-density equation of state. From our combined Bayesian analysis of nuclear theory, nuclear experiment, and observational constraints on the dense matter equation of state, we find at the 90% credibility level (Formula presented.) km for the radius of a (Formula presented.) neutron star, (Formula presented.) km for the radius of a (Formula presented.) neutron star, (Formula presented.) for the tidal deformability of a (Formula presented.) neutron star, and (Formula presented.) for the moment of inertia of PSR J0737-3039A whose mass is (Formula presented.).

KW - chiral effective field theory

KW - neutron stars

KW - nuclear equation of state

UR - http://www.scopus.com/inward/record.url?scp=85140581388&partnerID=8YFLogxK

U2 - 10.3390/galaxies10050099

DO - 10.3390/galaxies10050099

M3 - Article

AN - SCOPUS:85140581388

SN - 2075-4434

VL - 10

JO - Galaxies

JF - Galaxies

IS - 5

M1 - 99

ER -