Determination of the equation of state from nuclear experiments and neutron star observations

被引：26
作者：
Tsang, Chun Yuen [1 ,2 ]
Tsang, ManYee Betty [1 ,2 ]
Lynch, William G. [1 ,2 ]
Kumar, Rohit [1 ]
Horowitz, Charles J. [1 ,3 ,4 ]
机构：
[1] Michigan State Univ, Facil Rare Isotope Beams, E Lansing, MI 48824 USA
[2] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA
[3] Indiana Univ, Ctr Explorat Energy & Matter, Bloomington, IN USA
[4] Indiana Univ, Dept Phys, Bloomington, IN USA
来源：
NATURE ASTRONOMY | 2024年 / 8卷 / 03期
基金：
美国国家科学基金会;
关键词：
MATTER; PHYSICS; FLOW;
D O I：
10.1038/s41550-023-02161-z
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
With recent advances in neutron star observations, major progress has been made in determining the pressure of neutron star matter at high density. This pressure is constrained by the neutron star deformability, as determined from gravitational waves emitted in a neutron star merger, and measurements of the radii of two neutron stars made using the Neutron Star Interior Composition Explorer X-ray observatory on the International Space Station. Previous studies have relied on nuclear theory calculations to provide the equation of state at low density. Here we use a combination of 15 constraints composed of three astronomical observations and 12 nuclear experimental constraints that extend over a wide range of densities. Bayesian inference is then used to obtain a comprehensive nuclear equation of state. This data-centric result provides benchmarks for theoretical calculations and modelling of nuclear matter and neutron stars. Furthermore, it provides insights into the composition of neutron stars and their cooling due to neutrino radiation. Nuclear experiments become the latest 'messenger' to help with unravelling the mysteries of neutron stars. Combining information from astronomical observations and laboratory experiments reveals how nucleons interact in both nuclei and stars.
引用
收藏
页码：328 / 336
页数：9
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