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《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2006, Vol. 30> Issue(10) : 956-960 

Properties of Proto-Neutron Star and Effect of Three-Body Forces

  •  Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China2 Graduate University of Chinese Academy of Sciences, Beijing 100049, China3 School of Physics and Technology, Lanzhou University, Lanzhou 730000, China

  • Within the Brueckner-Hartree-Fock framework, the equation of state and the properties of newborn neutron stars are investigated by adopting a realistic nucleon-nucleon interaction AV18 supplemented with a microscopic three-body force or a phenomenological three-body force. The maximum mass of newborn neutron star and the proton fraction in the newborn beta-stable neutron-star matter are calculated. The neutrino-trapping and the three-body force effects are discussed, and the interplay between the effects of the trapped neutrino and the three-body force are especially explored. It is shown that neutrino trapping considerably affects the proton abundance and the equation of state of the newborn neutron star in both cases with and without the three-body forces. The effect of neutrino trapping remarkably enhances the proton abundance, and the contribution of the three-body force makes the equation of state of the newborn neutron star much stiffer at high densities and consequently increases the proton abundance strongly. The trapped neutrinos significantly reduce the influence of the three-body force on the proton abundance in newborn neutron stars.
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    [1] . Burrows A, Lattimer J M. Astrophys. J., 1986, 307: 1782. Prakash M et al. Phys. Rep., 1997, 280: 13. Pons J A et al. Astrophys. J., 1999, 513: 7804. Lattimer J M, Prakash M. Phys. Rep., 2000, 333: 1215. Arnett W D, Bowers R L. Astrophys. J., 1977, 33(Suppl.): 4156. Bombaci I. Neutron Star Structure and Nuclear Equation of State. In Nuclear Methods and the Nuclear Equation ofState. Baldo M Ed. Singapore: World Scienti c, 1999. 3817. Lattimer J M, Prakash M. Astrophys. J., 2001, 550: 4268. Engvik L et al. Astrophys. J., 1996, 469: 7949. Bednarek I, Manka R. Nucl. Phys., 2003, A719: 322c10. SUN Bao-Xi, JIA Huan-Yu, MENG Jie et al. HEP NP,2000, 24(Suppl.): 69(in Chinese)(孙宝玺, 贾焕玉, 孟杰等. 高能物理与核物理, 2000, 24(增刊)69); JIA Huan-Yu, Lü Hong-Feng, MENG Jie. HEP NP, 2002, 26: 1050 (in Chinese)(贾焕玉, 昌洪风, 孟杰.高能物理与核物理, 2002, 26: 1050); JIA Huan-Yu, MENG Jie, ZHAO En-Guang et al. HEP NP, 2003, 27: 200 (in Chinese)(贾焕玉, 孟杰, 赵恩广‘等. 高能物理与核物理, 2003, 27: 200)BAN S F et al. Phys. Rev., 2004, 69: 04580511. SHEN H. Phys. Rev., 2002, C65: 03580212. ZHOU X R et al. Phys. Rev., 2004, C69: 01880113. Bombaci I et al. Nucl. Phys., 1995, A583: 62314. Menezes D P, Providencia C. Phys. Rev., 2004, C69: 04580115. Mornas L. Eur. Phys. J., 2005, A24: 29316. Santos AMS, Menezes D P. Phys. Rev., 2004, C69: 04580317. Panda P K, Menezes D P, Providencia C. Phys. Rev., 2005,C69: 02520718. Vidana I et al. Astron. Astrophys., 2003, 399: 687; Nucl.Phys., 2003, A719: 17319. Tolman R C. Proc. Natl. Acad. Sci. U.S.A., 1934, 20: 3;Oppenheimer J R, Volkov G M. Phys. Rev., 1939, 55: 37420. ZUO W, Bombaci I, Lombardo U. Phys. Rev., 1999, C60: 024605; ZUO Wei et al. HEP NP, 2002, 26: 703(in Chinese)(左维等. 高能物理与核物理, 2002; 26: 703)21. SONG H Q, Baldo M, Giansiracusa G et al. Phys. Rev.Lett., 1998, 81: 158422. Baldo M, Fiasconaro A, SONG H Q et al. Phys. Rev., 2002,C65: 01730323. Wiringa R B, Stoks V G J, Schiavilla R. Phys. Rev., 1995,C51: 2824. Grange P et al. Phys. Rev., 1989, C40: 104025. ZUO Wei et al. Nucl. Phys., 2002, A706: 41826. Baldo M. The Nuclear Many-Body Theory and the NuclearEquation of State. In Nuclear Methods and the NuclearEquation of State. Baldo M Ed. Singapore: WorldScienti c, 1999. 127. Bethe G E et al. Nucl. Phys., 1979, B348: 34528. ZUO W et al. Euro. Phys. J., 2002, A14: 469; ZUO Weiet al. HEP NP, 2002, 26: 1238(in Chinese)(左维等. 高能物理与核物理, 2002; 26: 1238)

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ZUO Wei, LI Ang, LUO Pei-Yan and YONG Gao-Chan. Properties of Proto-Neutron Star and Effect of Three-Body Forces[J]. Chinese Physics C, 2006, 30(10): 956-960.
ZUO Wei, LI Ang, LUO Pei-Yan and YONG Gao-Chan. Properties of Proto-Neutron Star and Effect of Three-Body Forces[J]. Chinese Physics C, 2006, 30(10): 956-960. shu
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Received: 2005-11-28
Revised: 2006-02-20
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Properties of Proto-Neutron Star and Effect of Three-Body Forces

    Corresponding author: ZUO Wei,
  • Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China2 Graduate University of Chinese Academy of Sciences, Beijing 100049, China3 School of Physics and Technology, Lanzhou University, Lanzhou 730000, China
  • Received Date: 2005-11-28
  • Accepted Date: 2006-02-20
  • Available Online: 2006-10-05

Abstract: Within the Brueckner-Hartree-Fock framework, the equation of state and the properties of newborn neutron stars are investigated by adopting a realistic nucleon-nucleon interaction AV18 supplemented with a microscopic three-body force or a phenomenological three-body force. The maximum mass of newborn neutron star and the proton fraction in the newborn beta-stable neutron-star matter are calculated. The neutrino-trapping and the three-body force effects are discussed, and the interplay between the effects of the trapped neutrino and the three-body force are especially explored. It is shown that neutrino trapping considerably affects the proton abundance and the equation of state of the newborn neutron star in both cases with and without the three-body forces. The effect of neutrino trapping remarkably enhances the proton abundance, and the contribution of the three-body force makes the equation of state of the newborn neutron star much stiffer at high densities and consequently increases the proton abundance strongly. The trapped neutrinos significantly reduce the influence of the three-body force on the proton abundance in newborn neutron stars.

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