Effect of σ*,φ Mesons on the Neutron Star Matter at Finite Temperature

ZHAO Xian-Feng; WANG Shun-Jin; ZHANG Hua; JIA Huan-Yu

Chinese Physics C> 2007, Vol. 31> Issue(6) : 532-537

Effect of σ*,φ Mesons on the Neutron Star Matter at Finite Temperature

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

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Within the RMF approach, considering the contribution of σ*,φ mesons and baryon octet {n,p,Λ,Σ^－,Σ⁰,Σ⁺,Ξ^－,Ξ⁰}, some properties of neutron star matter have been investigated in the temperature region between 5—15MeV. It is found that when the contributions of σ*,φ mesons are included, (1) the critical baryon density decreases (but for the Λ hyperon, the effect is not obvious), but the number of hyperons increases; (2) the equation of state becomes soft at higher energy density; (3) the maximum mass decreases while the corresponding radius increases; (4) the central density, the central energy density, and the central pressure all become smaller. At T=5MeV and 10MeV and for Σ⁰,Ξ⁰,Σ⁺, the σ*,φ mesons make critical baryon density greatly decrease; but at T=15MeV, 20MeV, and 25MeV, the effect is not obvious. However, for Λ,Σ^－,Ξ^－ hyperons, at all the above temperatures, the effect is not obvious.

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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. Scha ner J, Dover C B, Gal A et al. Phys. Rev. Lett., 1993,71: 13285. Scha ner J, Dover C B, Gal A et al. Ann. Phys.(N.Y.),1994, 235: 356. TAN Yu-Hong, SUN Bao-Xi, LI Lei et al. Commun. Theor.Phys., 2004, 41: 4417. JIA Huan-Yu, MENG Jie, ZHAO En-Guang et al. HEP NP, 2003, 27(3): 200(in Chinese)(贾焕玉,孟杰.赵恩广等.高能物理与核物理,2003, 27(3):200)8. Glendenning N K, Moszkowski S A. Phys. Rev. Lett., 1991,67: 24149. Scha ner J, Greiner C, Stocker H. Phys. Rev., 1992, C46:32210. Scha ner 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. Glendenning 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. Burrows A, Lattimer J M. Astrophys. J., 1986, 307: 186

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[14]	LI Wen-Fei , ZHANG Feng-Shou , CHEN Lie-Wen . Study on Mass and Radius of Neutron Star Using Asymmetry Equation of State of Nuclear Matter. Chinese Physics C, 2001, 25(9): 877-883.
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[16]	Liu Jueping , Jin Yaping . Finite Temperature QCD Sum Rule and the ρ-Meson. Chinese Physics C, 1995, 19(12): 1108-1113.
[17]	Gao Shouen , Hut Yuan , Zheng Guotong , Su Rukeng . η-meson in the Pseudoscalar Coupling at Finite Temperature. Chinese Physics C, 1994, 18(2): 148-153.
[18]	Zheng Cuotong , Su Rukeng . One ρ-Meson Exchange Potential at Finite Temperature. Chinese Physics C, 1994, 18(6): 525-533.
[19]	ZHENG Guo-Tong , SU Ru-Keng . One η-Meson Exchange Potential of Nucleon-Nucleon at Finite Temperature. Chinese Physics C, 1992, 16(2): 131-136.
[20]	BI Pin-Zhen . KAONS CONDENSATION AT FINITE TEMPEATURE. Chinese Physics C, 1989, 13(3): 219-221.

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ZHAO Xian-Feng, WANG Shun-Jin, ZHANG Hua and JIA Huan-Yu. Effect of σ*,φ Mesons on the Neutron Star Matter at Finite Temperature[J]. Chinese Physics C, 2007, 31(6): 532-537.

ZHAO Xian-Feng, WANG Shun-Jin, ZHANG Hua and JIA Huan-Yu. Effect of σ*,φ Mesons on the Neutron Star Matter at Finite Temperature[J]. Chinese Physics C, 2007, 31(6): 532-537. shu

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Received: 2006-08-31
Revised: 2007-01-12

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沈阳化工大学材料科学与工程学院沈阳 110142

Effect of σ*,φ Mesons on the Neutron Star Matter at Finite Temperature

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: 2006-08-31

Accepted Date: 2007-01-12

Available Online: 2007-06-05

Abstract: Within the RMF approach, considering the contribution of σ*,φ mesons and baryon octet {n,p,Λ,Σ^－,Σ⁰,Σ⁺,Ξ^－,Ξ⁰}, some properties of neutron star matter have been investigated in the temperature region between 5—15MeV. It is found that when the contributions of σ*,φ mesons are included, (1) the critical baryon density decreases (but for the Λ hyperon, the effect is not obvious), but the number of hyperons increases; (2) the equation of state becomes soft at higher energy density; (3) the maximum mass decreases while the corresponding radius increases; (4) the central density, the central energy density, and the central pressure all become smaller. At T=5MeV and 10MeV and for Σ⁰,Ξ⁰,Σ⁺, the σ*,φ mesons make critical baryon density greatly decrease; but at T=15MeV, 20MeV, and 25MeV, the effect is not obvious. However, for Λ,Σ^－,Ξ^－ hyperons, at all the above temperatures, the effect is not obvious.

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Effect of σ*,φ Mesons on the Neutron Star Matter at Finite Temperature

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