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

Yeunhwan Lim; Jeremy W. Holt

doi:10.3390/galaxies10050099

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

Yeunhwan Lim, Jeremy W. Holt

Department of Physics

Research output: Contribution to journal › Article › peer-review

Abstract

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.).

Original language	English
Article number	99
Journal	Galaxies
Volume	10
Issue number	5
DOIs	https://doi.org/10.3390/galaxies10050099
Publication status	Published - 2022 Oct

Bibliographical note

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.

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics

Access to Document

10.3390/galaxies10050099

Cite this

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

abstract = "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.).",

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

note = "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: {\textcopyright} 2022 by the authors.",

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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.).

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