npsm 새물리 New Physics : Sae Mulli

pISSN 0374-4914 eISSN 2289-0041


Research Paper

New Physics: Sae Mulli 2016; 66: 1571-1577

Published online December 30, 2016

Copyright © New Physics: Sae Mulli.

Nuclear Equation of State and the Structure of Neutron Stars

Yeunhwan LIM*1, Taehyun KIM2, Yongseok OH†3

1 Cyclotron Institute, Texas A&M University, College Station, TX 77843, U.S.A.
2 Department of Physics, Kyungpook National University, Daegu 41566, Korea
3 Department of Physics, Kyungpook National University, Daegu 41566, Korea and Asia Pacific Center for Theoretical Physics, Pohang 37673, Korea

Correspondence to:*, †

Received: November 6, 2016; Revised: December 12, 2016; Accepted: December 12, 2016

This is an open-access article distributed under the terms of the Creative Commons Attribution Non-Commercial License ( which permits unrestricted non-commercial use, distribution, and reproduction in any medium, provided the original work is properly cited.


Starting from the binding energies of finite or isolated nuclei, to investigate ways to study inhomogeneous nuclear matter, \textit{i.e.}, nuclei with a free gas of neutrons, we review and discuss a general method to solve the nuclear equation of state for neutron stars by finding the solution for uniform nuclear matter. We also discuss a way to develop the nuclear equation of state in the presence of hyperons. The mass-radius relations of neutron stars are compared with the results of X-ray burst analyses to probe the validities of various models for the nuclear equation of state in neutron star physics.

Keywords: Neutron star, Nuclear equation of state, Nuclear properties, Nuclear matter

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