Dense Matter Equation of State: Neutron Star and Strange Star

LI Ang; HU Jinniu; BAO Shishao; SHEN Hong; XU Renxin

doi:10.11804/NuclPhysRev.36.01.001

Volume 36 Issue 1

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LI Ang, HU Jinniu, BAO Shishao, SHEN Hong, XU Renxin. Dense Matter Equation of State: Neutron Star and Strange Star[J]. Nuclear Physics Review, 2019, 36(1): 1-36. doi: 10.11804/NuclPhysRev.36.01.001

Citation:

LI Ang, HU Jinniu, BAO Shishao, SHEN Hong, XU Renxin. Dense Matter Equation of State: Neutron Star and Strange Star[J]. Nuclear Physics Review, 2019, 36(1): 1-36. doi: 10.11804/NuclPhysRev.36.01.001

Dense Matter Equation of State: Neutron Star and Strange Star

doi: 10.11804/NuclPhysRev.36.01.001

1.
College of Physical Science and Technology, Xiamen University, Xiamen 361005, Fujian, China;
2.
School of Physics, Nankai University, Tianjin 300071, China;
3.
School of Physics, Peking University, Beijing 100871, China

Funds: National Natural Science Foundation of China(11873040, 11775119, 11673002, 11675083, 11805115); National Key R&D Program of China(2017YFA0402602)

Received Date: 2018-09-10
Rev Recd Date: 2019-01-27
Publish Date: 2019-03-20

Abstract

The matter state inside neutron stars (NSs) is an exciting problem in nuclear physics, particle physics and astrophysics. The equation of state (EOS) of NSs plays a crucial role in the present multimessenger astronomy, especially after the event of GW170817. Thanks to accruing studies with advanced telescopes and radioactive beam facilities, the unknown EOS of supranuclear matter could soon be understood. We review the current status of the EOS for pulsar-like compact objects, that have been studied with both microscopic many-body approaches and phenomenological models. The appearance of strange baryonic matter and strange quark matter are also discussed. We compare the theoretical predictions with different data coming from both nuclear physics experiments and astrophysical observations. Despite great progresses obtained in dense nuclear matter properties, there are various challenges ahead, such as the model dependence of the constraints extracted from either experimental or observational data, the lack of a consistent and rigorous many-body treatment of all parts of the star, the dependence of many observables on the turbulent dynamics of relevant hot dense system. As LIGO is about to run again and discover more NS merger events, multimessenger observations are expected to finally unravel the mystery of NS structure.
- equation of state,
- dense nuclear matter,
- neutron star,
- strange star,
- nuclear astrophysics

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沈阳化工大学材料科学与工程学院沈阳 110142

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Dense Matter Equation of State: Neutron Star and Strange Star

1. College of Physical Science and Technology, Xiamen University, Xiamen 361005, Fujian, China;

2. School of Physics, Nankai University, Tianjin 300071, China;

3. School of Physics, Peking University, Beijing 100871, China

Funds: National Natural Science Foundation of China(11873040, 11775119, 11673002, 11675083, 11805115); National Key R&D Program of China(2017YFA0402602)

Received Date: 2018-09-10

Rev Recd Date: 2019-01-27

Publish Date: 2019-03-20

Key words:

Abstract: The matter state inside neutron stars (NSs) is an exciting problem in nuclear physics, particle physics and astrophysics. The equation of state (EOS) of NSs plays a crucial role in the present multimessenger astronomy, especially after the event of GW170817. Thanks to accruing studies with advanced telescopes and radioactive beam facilities, the unknown EOS of supranuclear matter could soon be understood. We review the current status of the EOS for pulsar-like compact objects, that have been studied with both microscopic many-body approaches and phenomenological models. The appearance of strange baryonic matter and strange quark matter are also discussed. We compare the theoretical predictions with different data coming from both nuclear physics experiments and astrophysical observations. Despite great progresses obtained in dense nuclear matter properties, there are various challenges ahead, such as the model dependence of the constraints extracted from either experimental or observational data, the lack of a consistent and rigorous many-body treatment of all parts of the star, the dependence of many observables on the turbulent dynamics of relevant hot dense system. As LIGO is about to run again and discover more NS merger events, multimessenger observations are expected to finally unravel the mystery of NS structure.

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Dense Matter Equation of State: Neutron Star and Strange Star

doi: 10.11804/NuclPhysRev.36.01.001

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通讯作者: 陈斌, bchen63@163.com

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