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2024年10月30日

Influence of the weakly interacting light U boson on the properties of massive protoneutron stars

  • Considering the octet baryons in relativistic mean field theory and selecting entropy per baryon S=1, we calculate and discuss the influence of U bosons on the equation of state, mass-radius, moment of inertia and gravitational redshift of massive protoneutron stars (PNSs). The effective coupling constant gU of U bosons and nucleons is selected from 0 to 70 GeV-2. The results indicate that U bosons will stiffen the equation of state (EOS). The influence of U bosons on the pressure is more obvious at low density than high density, while the influence of U bosons on the energy density is more obvious at high density than low density. The U bosons play a significant role in increasing the maximum mass and radius of PNS. When the value of gU changes from 0 to 70 GeV-2, the maximum mass of a massive PNS increases from 2.11M to 2.58M, and the radius of a PNS corresponding to PSR J0348+0432 increases from 13.71 km to 24.35 km. The U bosons will increase the moment of inertia and decrease the gravitational redshift of a PNS. For the PNS of the massive PSR J0348+0432, the radius and moment of inertia vary directly with gU, and the gravitational redshift varies approximately inversely with gU.
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  • [1] P. B. Demorest, T. Pennucci, S. M. Ransom et al, Nature(London), 467:1081(2010)
    [2] J. Antoniadis et al, Science, 340:448(2013)
    [3] C. H. Lenzi and G. Lugones, Astrophys. J, 759:57(2012)
    [4] S. Gandolfi, J. Carlson, and Sanjay Reddy, Phys. Rev. C, 85:032801(2012)
    [5] Ritam Mallick, Phys. Rev. C, 87:025804(2013)
    [6] S. Weissenborn, I. Sagert, G. Pagliara et al, Astrophys. J, 740:L14(2011)
    [7] X. F. Zhao and H. Y. Jia, Chin. Phys. C, 38(1):015101(2014)
    [8] Z. Yu, W. B. Ding, T. Bao et al, Chin. Phys. Lett, 28(8):089701(2011)
    [9] M. Tsuyoshi, Y. Sachiko, and N. Ken'ichiro, Astrophys. J, 777:4(2013)
    [10] X. F. Zhao and H. Y. Jia, Phys. Rev. C, 85:065806(2012)
    [11] I. Bednarek and R. Manka, Phys. Rev. C, 73:045804(2006)
    [12] P. Fayet, Phys. Lett. B, 95:285(1980)
    [13] D. R. Zhang, P. L. Yin, W. Wang et al, Phys. Rev. C, 83:035801(2011)
    [14] P. Jean et al, Astron. Astrophys, 407:L55(2013)
    [15] C. Boehm, D. Hooper, J. Silk et al, Phys. Rev. Lett., 92, 101301(2004)
    [16] E. G. Adelberger, B. R. Heckel, and A. E. Nelson, Annu. Rev. Nucl. Phys. Sci, 53:77(2003)
    [17] M. I. Krivoruchenko, F. imkovic, and Amand Faessler, Phys. Rev. D, 79:125023(2009)
    [18] M. Reece and L. T. Wang, J. High Energy Phys, 07(2009) 051
    [19] N. K. Glendenning, Phys. Lett. B, 114:392(1982)
    [20] P. Madappa, B. Ignazio, P. Manju et al, Phys. Reps, 280:1-77(1997)
    [21] N. K. Glendenning, Compact Star:Nuclear Physics, Particle Physics, and General Relativity (New York:Springer, 2000), P. 145-272
    [22] Y. Fujii, Nature, 234:5(1971)
    [23] Z. Hao and L. W. Chen, Phy. Rev. D, 85:043013(2012)
    [24] D. H. Wen, B. A. Li, and L. W. Chen, Phys. Rev. Lett., 103:211102(2009)
    [25] H. Davoudiasl, H. S. Lee, and W. J. Marciano, Phys. Rev. D, 85:115019(2012)
    [26] D. Babusci, I. Balwiera-Pytko, G. Bencivenni et al, Phys. Lett. B, 736:459-464(2014)
    [27] J. R. Oppenheimer and G. M. Volkoff, Phys. Rev., 55:374(1939)
    [28] F. J. Fattoyev and J. Piekarewicz, Phys. Rev. C, 82:025810(2010)
    [29] D. L. Benjamin, N. Mohit, and J. O. Benjamin, Phys. Rev. D, 73:024021(2006)
    [30] J. M. Lattimer and Y. Lim, Astrophys. J, 777:51(2013)
    [31] S. Banik, M. Hempel, and D.Bandyopadhyay, Astrophys. J. Suppl. Ser, 214:22(2014)
    [32] C. H. Lenzi and G. Lugones, Astrophys. J, 759:57(2012)
    [33] X. F. Zhao, Phys. Rev. C, 92:055802(2015)
    [34] N. K. Glendenning, Phys. Lett. B 114:392(1982)
    [35] S. Weissenborn, D. Chatterjee, and J. Schaffner-Bielich, Nucl. Phys. A, 881:62-77(2012)
    [36] D. J. Millener, C. B. Dover, and A. Gal, Phys. Rev. C, 38:2700(1988)
    [37] J. Schaffner, C. Greiner, and H. Stcker, Phys. Rev. C, 46:322(1992)
    [38] C. J. Batty, E. Friedman, and A. Gal, Phys. Reps, 287:385(1997)
    [39] B. J. Schaffner and A. Gal, Phys. Rev. C, 62:034311(2000)
    [40] S. Aoki, S. Y. Bahk, and K. S. Chung, Phys. Lett. B, 355:45(1995)
    [41] P. Khaustov, D. E. Alburger, P. D. Barnes et al, Phys. Rev. C, 61:054603(2000)
    [42] N. K. Glendenning and S. A. Moszkowski, Phys. Rev. Lett., 67:2414(1991)
    [43] S. Pal, M. Hanauske, I. Zakout et al, Phys. Rev. C, 60:015802(1999)
    [44] A. Drago, A. Lavabno, and G. Pagloara, Phys. Rev. D, 89:043014(2014)
    [45] F. Ozel, D. Psaltis, S. Pansom et al, Astrophys. J, 724:L199-L202(2010)
    [46] V. Dexheimer and S. Schramm, Astrophys. J, 683:943-948(2008)
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Bin Hong, Huan-Yu Jia, Xue-Ling Mu and Xia Zhou. Influence of the weakly interacting light U boson on the properties of massive protoneutron stars[J]. Chinese Physics C, 2016, 40(6): 065101. doi: 10.1088/1674-1137/40/6/065101
Bin Hong, Huan-Yu Jia, Xue-Ling Mu and Xia Zhou. Influence of the weakly interacting light U boson on the properties of massive protoneutron stars[J]. Chinese Physics C, 2016, 40(6): 065101.  doi: 10.1088/1674-1137/40/6/065101 shu
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Received: 2015-11-30
Revised: 2016-01-25
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    Supported by National Natural Science Foundation of China (11175147)

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Influence of the weakly interacting light U boson on the properties of massive protoneutron stars

    Corresponding author: Huan-Yu Jia,
  • 1. Institute for Modern Physics, Southwest Jiaotong University, Chengdu 610031, China
Fund Project:  Supported by National Natural Science Foundation of China (11175147)

Abstract: Considering the octet baryons in relativistic mean field theory and selecting entropy per baryon S=1, we calculate and discuss the influence of U bosons on the equation of state, mass-radius, moment of inertia and gravitational redshift of massive protoneutron stars (PNSs). The effective coupling constant gU of U bosons and nucleons is selected from 0 to 70 GeV-2. The results indicate that U bosons will stiffen the equation of state (EOS). The influence of U bosons on the pressure is more obvious at low density than high density, while the influence of U bosons on the energy density is more obvious at high density than low density. The U bosons play a significant role in increasing the maximum mass and radius of PNS. When the value of gU changes from 0 to 70 GeV-2, the maximum mass of a massive PNS increases from 2.11M to 2.58M, and the radius of a PNS corresponding to PSR J0348+0432 increases from 13.71 km to 24.35 km. The U bosons will increase the moment of inertia and decrease the gravitational redshift of a PNS. For the PNS of the massive PSR J0348+0432, the radius and moment of inertia vary directly with gU, and the gravitational redshift varies approximately inversely with gU.

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