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Chinese Physics C> 2014, Vol. 38> Issue(1) : 015101 DOI: 10.1088/1674-1137/38/1/015101

Transition density of the large mass hyperon star

  • The difference between the transition density of a larger mass hyperon star (for example, the neutron star PSR J1614-2230) and that of a smaller mass hyperon star is investigated in the framework of the relativistic mean field theory. We see that the transition density ρ0H increases with the increase of xω (i.e. the mass of the neutron star). For the nucleons parts, the neutrons make the main contribution to the transition density as the baryon density ρ=ρ0H. With the increase of the xω (i.e. the mass of the neutron star), the relative particle number density of neutrons decreases while that of protons increases. For the parts of hyperons, the Λ and Ξ- make the main contributions to the transition density as the baryon density ρ=ρ0H. The relative particle number density of Λ decreases while that of Ξ- increases with the increase of the xω (i.e. the mass of the neutron star). For the hyperons Σ-, Σ0 and Σ-, the total contributions are less than 16 per cent.
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    [1] Glendenning N K. Compact Stars: Nuclear Physics, Particle Physics, and General Relativity. 2nd ed. Springer, 2000[2] Glendenning N K. Astrophy, 1985, 293: 470-493[3] JIA Huan-Yu, SUN Bao-Xi, MENG Jie et al. Chin. Phys. Lett., 2001, 18: 1571-1574[4] ZHAO Xian-Feng, ZHANG Hua. Chin. Phys. C (HEP NP), 2010, 34: 1704-1708[5] Demorest P B, Pennucci T, Ransom S M et al. Nature, 2010, 467: 1081-1083[6] Massot #278;, Margueron J, Chanfray G. Europhysics Letters, 2012, 97(3): 39002[7] Weissenborn S, Chatterjee D, Schaffner-Bielich J. Phys. Rev. C, 2012, 85(6): 065802[8] Masuda K, Hatsuda T, Takatsuka T. Ap. J, 2012, 764(1): 12[9] Whittenbury D L, Carroll J D, Thomas A W, Tsushima K, Stone J R. eprint arXiv: 1204.2614(2012)[10] Mallick R. Phys. Rev. C, 2013, 87(2): 025804[11] Bednarek I, Haensel P, Zdunik J L, Bejger M, Mańka R. Astronomy Astrophysics, 2012, 543: A157[12] Katayama T, Miyatsu T, Saito K. Ap.J S, 2012, 203(2): 22[13] Weissenborn S, Chatterjee D, Schaffner-Bielich J. Nucl. Phys. A, 2012, 881: 62-77[14] JIANG Wei-Zhou, LI Bao-An, CHEN Lie-Wen. Ap. J., 2012, 756: 56[15] Chamel N, Fantina A F, Pearson J M, Goriely S. eprint arXiv: 1205.0983(2012)[16] ZHAO Xian-Feng, JIA Huan-Yu. Phys. Rev. C, 2012, 85: 065806[17] Schaffner J, Mishustin I N. Phys. Rev. C, 1996, 53: 1416-1429[18] Glendenning N K, Moszkowski S A. Phys. Rev. Lett., 1991, 67: 2414-2417[19] TAN Yu-Hong, SUN Bao-Xi, LI Lei et al. Theor. Phys., 2004, 41: 441-446[20] Dover C B, Millener D J, Gal A. Phys. Rep., 1989, 184: 1-97[21] Friedman E, Gal A. Phys. Rep., 2007, 452: 89-153[22] Batty C J, Friedman E, Gal A. Phys. Lett. B, 1994, 335: 273-278[23] Bart S, Chrien R E, Franklin W A et al. Phys. Rev. Lett., 1999, 83: 5238-5241[24] Khaustov P, Alburger D E, Barnes P D et al. Phys. Rev. C, 2000, 61: 054603[25] Fukuda T, Higashi A, Matsuyama Y et al. Phys. Rev. C, 1998, 58: 1306-1309[26] Dover C B, Gal A. Ann. Phys., 1983, 146: 309-348

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ZHAO Xian-Feng and JIA Huan-Yu. Transition density of the large mass hyperon star[J]. Chinese Physics C, 2014, 38(1): 015101. doi: 10.1088/1674-1137/38/1/015101
ZHAO Xian-Feng and JIA Huan-Yu. Transition density of the large mass hyperon star[J]. Chinese Physics C, 2014, 38(1): 015101.  doi: 10.1088/1674-1137/38/1/015101 shu
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Received: 2012-12-03
Revised: 1900-01-01
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Transition density of the large mass hyperon star

    Corresponding author: ZHAO Xian-Feng,
  • Received Date: 2012-12-03
  • Accepted Date: 1900-01-01
  • Available Online: 2014-01-05

Abstract: The difference between the transition density of a larger mass hyperon star (for example, the neutron star PSR J1614-2230) and that of a smaller mass hyperon star is investigated in the framework of the relativistic mean field theory. We see that the transition density ρ0H increases with the increase of xω (i.e. the mass of the neutron star). For the nucleons parts, the neutrons make the main contribution to the transition density as the baryon density ρ=ρ0H. With the increase of the xω (i.e. the mass of the neutron star), the relative particle number density of neutrons decreases while that of protons increases. For the parts of hyperons, the Λ and Ξ- make the main contributions to the transition density as the baryon density ρ=ρ0H. The relative particle number density of Λ decreases while that of Ξ- increases with the increase of the xω (i.e. the mass of the neutron star). For the hyperons Σ-, Σ0 and Σ-, the total contributions are less than 16 per cent.

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