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《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2005, Vol. 29> Issue(6) : 565-569 

Pesponse of the Neutron Star Properties to the Equation of State at Low Density

  •  School of Physics,Peking University,Beijing 1008712 Institute of Theoretical Physics,Chinese Academy of Science,Beijing 1000803 Center of Theoretical Nuclear Physics,National Laboratory of Heavy Ion Accelerator,Lanzhou 730000

  • Using the RMF theory to describe the neutron liquid region in the neutron star and the Fermi gas model or FMT, BPS,and BBP model to describe the crust of the neutron star (referred as Fermi gas+RMF and RMF* respectively),the properties of the neutron star are calculated and compared with those from the RMF theory. Although the EOS at low density has negligible influence on the maximum mass of the neutron star, and its corresponding central density, energy density, and pressure, it changes the mass-radius relationship of neutron stars considerably. The differences of the neutron star radius corresponding to maximum mass between the RMF theory and RMF* calculations are 0.23-0.33 km.
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ZHU Zhao-Huan, BAN Shu-Fang, LI Jun and MENG Jie. Pesponse of the Neutron Star Properties to the Equation of State at Low Density[J]. Chinese Physics C, 2005, 29(6): 565-569.
ZHU Zhao-Huan, BAN Shu-Fang, LI Jun and MENG Jie. Pesponse of the Neutron Star Properties to the Equation of State at Low Density[J]. Chinese Physics C, 2005, 29(6): 565-569. shu
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Received: 2005-01-26
Revised: 1900-01-01
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Pesponse of the Neutron Star Properties to the Equation of State at Low Density

    Corresponding author: MENG Jie,
  • School of Physics,Peking University,Beijing 1008712 Institute of Theoretical Physics,Chinese Academy of Science,Beijing 1000803 Center of Theoretical Nuclear Physics,National Laboratory of Heavy Ion Accelerator,Lanzhou 730000
  • Received Date: 2005-01-26
  • Accepted Date: 1900-01-01
  • Available Online: 2005-06-05

Abstract: Using the RMF theory to describe the neutron liquid region in the neutron star and the Fermi gas model or FMT, BPS,and BBP model to describe the crust of the neutron star (referred as Fermi gas+RMF and RMF* respectively),the properties of the neutron star are calculated and compared with those from the RMF theory. Although the EOS at low density has negligible influence on the maximum mass of the neutron star, and its corresponding central density, energy density, and pressure, it changes the mass-radius relationship of neutron stars considerably. The differences of the neutron star radius corresponding to maximum mass between the RMF theory and RMF* calculations are 0.23-0.33 km.

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