Neutron star equation of state in density dependent relativistic Hartree-Fock theory*

中国物理C, 2009, 33(z1): 73-75.

^1, , ^2,

1.School of Physics, and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China

2.School of Physics, and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China;Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100080, China;Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator, Lanzhou 730000, China;Department of Physics, University of Stellenbosch, Stellenbosch, South Africa

基金项目: 国家重点基础研究发展规划(973计划)(2007CB815000) 国家自然科学基金(10435010;10775004;10221003)

Neutron star equation of state in density dependent relativistic Hartree-Fock theory*

SUN Bao-Yuan ^1, , MENG Jie ^2,

1.School of Physics, and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China

2.School of Physics, and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China;Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100080, China;Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator, Lanzhou 730000, China;Department of Physics, University of Stellenbosch, Stellenbosch, South Africa

Keywords： neutron stars

The equation of state of neutron stars is studied in the newly developed density dependent relativistic Hartree-Fock (DDRHF) theory with the effective interaction PKO1 and applied to describe the properties of neutron stars. The results are compared with the recent observational data of compact stars and those calculated with the relativistic mean field (RMF) effective interactions. The maximum mass of neutron stars calculated with PKO1 is about 2.45 M☉, which consists with high pulsar mass from PSR B1516+02B recently reported. The influence of Fock terms on the cooling of neutron stars is discussed as well.

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