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Chinese Physics C> 2017, Vol. 41> Issue(4) : 045102 DOI: 10.1088/1674-1137/41/4/045102

Neutron stars including the effects of chaotic magnetic fields and anomalous magnetic moments

  • 1.

      Physics Department, Nanjing University, Nanjing 210008, China

  • 2.

      Shanghai Institute of Applied Physics, Chinese Academy of Science, Shanghai 201800, China

  • 3.

     Physics Department, Nanjing University, Nanjing 210008, China

  • 4.

     Center of Theoretical Nuclear Physics, National Laboratory of Heavy-Ion Accelerator, Lanzhou 730000, China

  • 5.

     Kavli Institute for Theoretical Physics China, Chinese Academy of Sciences, Beijing 100190, China

  • The relativistic mean field (RMF) FSUGold model extended to include hyperons is employed to study the properties of neutron stars with strong magnetic fields. The chaotic magnetic field approximation is utilized. The effect of anomalous magnetic moments (AMMs) is also investigated. It is shown that the equation of state (EOS) of neutron star matter is stiffened by the presence of the magnetic field, which increases the maximum mass of a neutron star by around 6%. The AMMs only have a small influence on the EOS of neutron star matter, and increase the maximum mass of a neutron star by 0.02Msun. Neutral particles are spin polarized due to the presence of the AMMs.
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    [1] R. Brito, V. Cardoso, and P. Pani, Phys. Rev. D, 89:104045 (2014)
    [2] R. A. Konoplya and R. D. B. Fontana, Phys. Lett. B, 659:375-379 (2008)
    [3] C. Wu and R. L. Xu, Eur. Phys. J. C, 75:391 (2015)
    [4] R. C. Duncan and C. Thompson, Astrophys. J., 392:L9 (1992)
    [5] C. Thompson and R. C. Duncan, Mon. Not. Roy. Astron. Soc., 275:255-300 (1995)
    [6] V. V. Usov, Nature, 357:472-474 (1992)
    [7] G. Vasisht and E. V. Gotthelf, Astrophys. J., 486:L129 (1997)
    [8] P. M. Woods, C. Kouveliotou, J. van Paradijs et al, Astrophys. J., 519:L139 (1999)
    [9] C. Kouveliotou, Nature, 393:235-237 (1998)
    [10] A. Broderick, M. Prakash, and J. M. Lattimer, Astrophys. J., 537:351 (2000)
    [11] J. R. Oppenheimer and G. M. Volkoff, Phys. Rev., 55:374-381 (1939)
    [12] C. Wu and Z. Z. Ren, Phys. Rev. C, 83:025805 (2011)
    [13] L. L. Lopes and D. Menezes, JCAP, 1508:002 (2015)
    [14] A. E. Broderick, M. Prakash, and J. M. Lattimer, Phys. Lett. B, 531:167-174 (2002)
    [15] D. Bandyopadhyay, S. Chakrabarty, and S. Pal, Phys. Rev. Lett., 79:2176-2179 (1997)
    [16] A. Rabhi, H. Pais, P. K. Panda et al, J. Phys. G, 36:115204 (2009)
    [17] D. P. Menezes, M. Benghi Pinto, S. S. Avancini et al, Phys. Rev. C, 80:065805 (2009)
    [18] C. Y. Ryu, K. S. Kim, and M.-K. Cheoun, Phys. Rev. C, 82:025804 (2010)
    [19] A. Rabhi, P. K. Panda, and C. Providencia, Phys. Rev. C, 84:035803 (2011)
    [20] R. Mallick and M. Sinha, Mon. Not. Roy. Astron. Soc., 414:2702-2708 (2011)
    [21] L. L. Lopes and D. P. Menezes, Braz. J. Phys., 42:428-436 (2012)
    [22] R. H. Casali, L. B. Castro, and D. P. Menezes, Phys. Rev. C, 89:015805 (2014)
    [23] D. P. Menezes, M. B. Pinto, L. B. Castro et al, Phys. Rev. C, 89:055207 (2014)
    [24] R. M. S. Schramm and S. Schramm, Phys. Rev. C, 89:045805 (2014)
    [25] Y. F. Yuan and J. L. Zhang, Astrophys. J., 525:950 (1996)
    [26] B. G. Todd-Rutel and J. Piekarewicz, Phys. Rev. Lett., 95:122501 (2005)
    [27] J. Piekarewicz, Phys. Rev. C, 76:064310 (2007)
    [28] F. J. Fattoyev and J. Piekarewicz, Phys. Rev. C, 82:025810 (2010)
    [29] N. K. Glendenning, Phys. Lett. B, 114:392-396 (1982)
    [30] G. J. Mao, A. Iwamoto, and Z. X. Li, Chin. J. Astron. Astrophys., 3:359-374 (2003)
    [31] C. Wu, W. L. Qian, Y. G. Ma et al, Int. J. Mod. Phys. E, 22:1350026 (2013)
    [32] R. L. Xu, C. Wu, and Z. Z. Ren, Int. J. Mod. Phys. E, 23:1450078 (2014)
    [33] S. Chakrabarty, Phys. Rev. D, 54:1306 (1996)
    [34] M. Strickland, V. Dexheimer, and D. P. Menezes, Phys. Rev. D, 86:125032 (2012)
    [35] M. Baldo, I. Bombaci, and G. F. Burgio, Astron. Astrophys., 328:274-282 (1997)
    [36] V. Kalogera and G. Baym, Astrophys. J., 470:L61-L64 (1996)
    [37] V. Dexheimer, R. Negreiros, and S. Schramm, Eur. Phys. J. A, 48:189 (2012)
    [38] J. M. Dong, U. Lombardo, W. Zuo et al, Nucl. Phys. A, 898:32-42 (2013)
    [39] R. O. Gomes, V. Dexheimer, and C. A. Z. Vasconcellos, Astron. Nachr., 335:666 (2014)
    [40] M. Sinha, B. Mukhopadhyay, and A. Sedrakian, Nucl. Phys. A, 898:43-58 (2013)
    [41] K. A. Maslov, E. E. Kolomeitsev, and D.N.Voskresensky, Phys. Rev. C, 92:052801 (2015)

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Fei Wu, Chen Wu and Zhong-Zhou Ren. Neutron stars including the effects of chaotic magnetic fields and anomalous magnetic moments[J]. Chinese Physics C, 2017, 41(4): 045102. doi: 10.1088/1674-1137/41/4/045102
Fei Wu, Chen Wu and Zhong-Zhou Ren. Neutron stars including the effects of chaotic magnetic fields and anomalous magnetic moments[J]. Chinese Physics C, 2017, 41(4): 045102.  doi: 10.1088/1674-1137/41/4/045102 shu
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Received: 2016-09-25
Revised: 2016-11-09
Fund

    Supported by National Natural Science Foundation of China (11535004, 11375086, 11120101005, 11175085, 11235001), 973 National Major State Basic Research and Development of China (2013CB834400), and Science and Technology Development Fund of Macau (068/2011/A)

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Neutron stars including the effects of chaotic magnetic fields and anomalous magnetic moments

    Corresponding author: Fei Wu,
    Corresponding author: Chen Wu,
    Corresponding author: Zhong-Zhou Ren,
  • 1.  Physics Department, Nanjing University, Nanjing 210008, China
  • 2.  Shanghai Institute of Applied Physics, Chinese Academy of Science, Shanghai 201800, China
  • 3. Physics Department, Nanjing University, Nanjing 210008, China
  • 4. Center of Theoretical Nuclear Physics, National Laboratory of Heavy-Ion Accelerator, Lanzhou 730000, China
  • 5. Kavli Institute for Theoretical Physics China, Chinese Academy of Sciences, Beijing 100190, China
  • Received Date: 2016-09-25
  • Accepted Date: 2016-11-09
  • Available Online: 2017-04-05
Fund Project:  Supported by National Natural Science Foundation of China (11535004, 11375086, 11120101005, 11175085, 11235001), 973 National Major State Basic Research and Development of China (2013CB834400), and Science and Technology Development Fund of Macau (068/2011/A)

Abstract: The relativistic mean field (RMF) FSUGold model extended to include hyperons is employed to study the properties of neutron stars with strong magnetic fields. The chaotic magnetic field approximation is utilized. The effect of anomalous magnetic moments (AMMs) is also investigated. It is shown that the equation of state (EOS) of neutron star matter is stiffened by the presence of the magnetic field, which increases the maximum mass of a neutron star by around 6%. The AMMs only have a small influence on the EOS of neutron star matter, and increase the maximum mass of a neutron star by 0.02Msun. Neutral particles are spin polarized due to the presence of the AMMs.

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