YU Zi1**, DING Wen-Bo2, BAO Tmurbagan3, LIU Ning-Ning4
1The College of Science, Nanjing Forestry University, Nanjing 210037 2Department of Physics, Bohai University, Jinzhou 121000 3College of Physics and Electronic Engineering, Nanyang Normal University, Nanyang 473061 4Department of Basic Course, Nanjing Institute of Technology, Nanjing 211167
PSR J1614-2230 May Include Hyperons
YU Zi1**, DING Wen-Bo2, BAO Tmurbagan3, LIU Ning-Ning4
1The College of Science, Nanjing Forestry University, Nanjing 210037 2Department of Physics, Bohai University, Jinzhou 121000 3College of Physics and Electronic Engineering, Nanyang Normal University, Nanyang 473061 4Department of Basic Course, Nanjing Institute of Technology, Nanjing 211167
摘要In the framework of the relativistic mean field theory, it is found that recently discovered PSR J1614-2230 with mass of 1.97±0.04Mʘ may include hyperons when the weakly interacting light boson (WILB) is considered. To describe PSR J1614−2230 with the equation of state (EOS) including hyperons, the characteristic scale of the WILB (g2/μ2) should lie in the range of 13–46 (24–46) GeV−2 with the weak (strong) hyperon-hyperon (YY) interaction. The measurements of inertial momentum and the total neutrino luminosity of the neutron star could be used to further constrain the characteristic scale of the WILB. Before more stringent constraint on the WILB is given, the mass measurement of the neutron star could not exclude any soft EOS.
Abstract：In the framework of the relativistic mean field theory, it is found that recently discovered PSR J1614-2230 with mass of 1.97±0.04Mʘ may include hyperons when the weakly interacting light boson (WILB) is considered. To describe PSR J1614−2230 with the equation of state (EOS) including hyperons, the characteristic scale of the WILB (g2/μ2) should lie in the range of 13–46 (24–46) GeV−2 with the weak (strong) hyperon-hyperon (YY) interaction. The measurements of inertial momentum and the total neutrino luminosity of the neutron star could be used to further constrain the characteristic scale of the WILB. Before more stringent constraint on the WILB is given, the mass measurement of the neutron star could not exclude any soft EOS.
(Forces in hadronic systems and effective interactions)
引用本文:
YU Zi**;DING Wen-Bo;BAO Tmurbagan;LIU Ning-Ning
. PSR J1614-2230 May Include Hyperons[J]. 中国物理快报, 2011, 28(8): 89701-089701.
YU Zi**, DING Wen-Bo, BAO Tmurbagan, LIU Ning-Ning
. PSR J1614-2230 May Include Hyperons. Chin. Phys. Lett., 2011, 28(8): 89701-089701.
[1] Lattimer J M and Prakash M 2001 Astrophys. J. 550 426
[2] Prakash M et al 1997 Phys. Rep. 280 1
[3] Özel F 2006 Nature 441 1115
[4] Lackey B D et al 2006 Phys. Rev. D 73 024021
[5] Alford M, Blaschke D, Drago A et al 2007 Nature 445 7
[6] Demorest P B, Pennucci T, Ransom S M et al 2010 Nature 467 1081
[7] Pease R 2001 Nature 411 986
[8] Hoyle C D 2003 Nature 421 899
[9] Fayet P 1980 Phys. Lett. B 95 285
[10] Adelberger E G, Heckel B R and Nelson A E 2003 Annu. Rev. Nucl. Phys. Sci. 53 77
[11] Reece M and Wang L T 2009 J. High Enery Phys. 7 051
[12] Jean P et al 2003 Astron. Astrophys. 407 L55
[13] Boehm C, Hooper D, Silk J et al 2004 Phys. Rev. Lett. 92 101301
[14] Wen D H, Li B A and Chen L W 2009 Phys. Rev. Lett. 103 211102
[15] Krivoruchenko M I, Simkovic F, Faessler A 2009 Phys. Rev. D 79 125023
[16] Zhang D R, Yin P L, Wei W et al 2011 Phys. Rev. C 83 035801
[17] Wen D H, Li B A, Chen L W et al 2011 arXiv:1101.1504
[18] Rufa M, Schaffner J, Maruhn J, Stöcker H 1990 Phys. Rev. C 42 2469
[19] Danysz M, 1963 Nucl. Phys. 49 121
Dalitz R H, Davis D H, Fowler P H et al 1989 Proc. R. Soc. A 426 1
[20] Prowse D J 1966 Phys. Rev. Lett. 17 782
[21] Aoki S, Bahk S Y, Chung K S et al 1991 Prog. Theor. Phys. 85 1287
[22] Takahashi H, Ahn J K, Akikawa H et al 2001 Phys. Rev. Lett. 87 212502
[23] Schaffner J and Mishustin I N 1996 Phys. Rev. C 53 1416
[24] Schaffner-Bielich J, Hanauske M, Stöer H et al 2002 Phys. Rev. Lett. 89 171101
[25] Shen H 2002 Phys. Rev. C 65 035802
[26] Qian W L, Su R K and Song H Q 2004 J. Phys. G 30 1893
[27] Bednarek I and Manka R 2005 J. Phys. G 31 1009
[28] Li A, Zuo W, Mi A J et al 2007 Chin. Phys. 16 1934
[29] Yang F and Shen H 2008 Phys. Rev. C 77 025801
[30] Mi A J and You W 2010 Commun. Theor. Phys. 53 133
[31] Yu Z, Liu G Z, Zhu M F et al 2010 Nucl. Phys. A 834 97c
[32] Boguta J and Bodmer A R 1977 Nucl. Phys. A 292 413
[33] Schaffener J, Dover C B, Gal A et al 1993 Phys. Rev. Lett. 71 1328
[34] Schaffner J, Dover C B, Gal A et al 1994 Ann. Phys. 235 35
[35] Sugahara Y and Toki H 1994 Nucl. Phys. A 579 557
[36] Worley A, Krastev P G and Li B A 2008 Astronphys. J. 685 390
[37] Yu Z and Ding W B 2011 Commun. Theor. Phys. 55 643
[38] Yu Z and Ding W B 2011 Chin. Physc. C (in press)
2011, Vol. 28 
