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《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2007, Vol. 31> Issue(4) : 345-349 

Effect of f0(975) and φ(1020) Mesons on Neutron Star Mater

  •  College of Physics Science and Technology, Sichuan University, Chengdu 610065, China2 Department of Basic Courses of Emei Campus, Southwest Jiaotong University, Emeishan 614202, China3 Institute for Modern Physics, Southwest Jiaotong University, Chengdu 610031, China

  • In the RMF approach, considering the contributions of the σ* and φ mesons and the hyperons in the baryon octet {N,P,Λ,∑－,∑0,∑+,Ξ－,Ξ0}, the properties of neutron star matter have been investigated. It is found that with the contributions of the σ* and φ mesons, the critical baryon density of hyperon appearance decreases, the number of hyperons increases, the transition density ρ0H of hyperon stars decreases, the equation of state turns soft, the maximum mass of neutron star decreases and the corresponding radius increases, the central density, the central energy density and the central pressure are all reduced.
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    [1] . Lattimer J M, Prakash M. Science, 2004, 304: 5362. Glendenning N K. Astrophys. J., 1985, 293: 4703. Glendenning N K. Compact Stars: Neuclear Physics, ParticlePhysics and General Relativety. New York: Springer-Verlag, New York, Inc, 1997. 180-2464. Schaffner J, Dover C B, Gal A et al. Phys. Rev. Lett., 1993,71: 13285. Schaffner J, Dover C B, Gal A et al. Ann. Phys.(N.Y.),1994, 235: 356. Takahashi H et al. Phys. Rev. Lett., 2001, 87:212502-1.07. TAN Yu-Hong, SUN Bao-Xi, LI Lei et al. Commun.Theor.Phys., 2004, 41: 4418. Glendening N K, Moszkowski S A. Phys. Rev. Lett., 1991,67: 24149. Schaffner J, Greiner C, Stcker H. Phys. Rev., 1992, C46:32210. Schaffner J, Mishustin I N. Phys. Rev., 1996, C53: 141611. Dover C B, Gal A. Ann. Phys. (N.Y), 1983, 146: 30912. Fukuda T et al. Phys. Rev., 1998, C58: 130613. Ellis J, Kapusta J I, Olive K A. Nucl. Phys., 1991, B348:34514. Glendening N K, Von-Ei D, Haft M et al. Phys. Rev.,1993, C48: 88915. Mare#353; J, Friedman E, Gal A et al. Nucl. Phys., 1995, A594:31116. Bart S et al. Phys. Rev. Lett., 1999, 83: 523817. Dabrowski J. Phys. Rev., 1999, C60: 02520518. Harada T. Nucl. Phys., 2000, A672: 18119. JIA Huan-Yu, SUN Bao-Xi, MENG Jie et al. Chin. Phys.Lett., 2001, 18(12): 1571

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ZHAO Xian-Feng, WANG Shun-Jin, ZHANG Hua and JIA Huan-Yu. Effect of f0(975) and φ(1020) Mesons on Neutron Star Mater[J]. Chinese Physics C, 2007, 31(4): 345-349.
ZHAO Xian-Feng, WANG Shun-Jin, ZHANG Hua and JIA Huan-Yu. Effect of f0(975) and φ(1020) Mesons on Neutron Star Mater[J]. Chinese Physics C, 2007, 31(4): 345-349. shu
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Received: 2006-05-19
Revised: 2006-11-20
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Effect of f0(975) and φ(1020) Mesons on Neutron Star Mater

    Corresponding author: ZHAO Xian-Feng,
  • College of Physics Science and Technology, Sichuan University, Chengdu 610065, China2 Department of Basic Courses of Emei Campus, Southwest Jiaotong University, Emeishan 614202, China3 Institute for Modern Physics, Southwest Jiaotong University, Chengdu 610031, China
  • Received Date: 2006-05-19
  • Accepted Date: 2006-11-20
  • Available Online: 2007-04-05

Abstract: In the RMF approach, considering the contributions of the σ* and φ mesons and the hyperons in the baryon octet {N,P,Λ,∑－,∑0,∑+,Ξ－,Ξ0}, the properties of neutron star matter have been investigated. It is found that with the contributions of the σ* and φ mesons, the critical baryon density of hyperon appearance decreases, the number of hyperons increases, the transition density ρ0H of hyperon stars decreases, the equation of state turns soft, the maximum mass of neutron star decreases and the corresponding radius increases, the central density, the central energy density and the central pressure are all reduced.

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