Impact factor of Chinese Physics C is 3.6 in 2023 Impact factor of Chinese Physics C is 3.6 in 2022 2021 Impact Factor 2.944
Advanced Search
×
近期发现有不法分子冒充我刊与作者联系，借此进行欺诈等不法行为，请广大作者加以鉴别，如遇诈骗行为，请第一时间与我刊编辑部联系确认（《中国物理C》（英文）编辑部电话：010-88235947,010-88236950），并作报警处理。
本刊再次郑重声明：
（1）本刊官方网址为cpc.ihep.ac.cn和https://iopscience.iop.org/journal/1674-1137
（2）本刊采编系统作者中心是投稿的唯一路径，该系统为ScholarOne远程稿件采编系统，仅在本刊投稿网网址（https://mc03.manuscriptcentral.com/cpc）设有登录入口。本刊不接受其他方式的投稿，如打印稿投稿、E-mail信箱投稿等，若以此种方式接收投稿均为假冒。
（3）所有投稿均需经过严格的同行评议、编辑加工后方可发表，本刊不存在所谓的“编辑部内部征稿”。如果有人以“编辑部内部人员”名义帮助作者发稿，并收取发表费用，均为假冒。
                  
《中国物理C》（英文）编辑部
2024年10月30日
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.
      PCAS:
  • 加载中

  • References

    [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)

  • Access

    加载中

Get Citation
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
Milestone
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)

Article Metric

Article Views(1498)
PDF Downloads(33)
Cited by(0)
Policy on re-use
To reuse of subscription content published by CPC, the users need to request permission from CPC, unless the content was published under an Open Access license which automatically permits that type of reuse.
通讯作者: 陈斌, bchen63@163.com
  • 1. 

    沈阳化工大学材料科学与工程学院 沈阳 110142

  1. 本站搜索
  2. 百度学术搜索
  3. 万方数据库搜索
  4. CNKI搜索

Email This Article

Title:
Email:

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.

    HTML

Reference (41)

目录

Link
IOPScience
SCOAP3
arXiv
Chinese Physical Society
Journal information
Introduction
Editorial Board
Others
Subscribe
Contact us
QQ: 1307685413
Tel: +86-010-88235947
Fax: +86-010-88233126
E-mail: cpc@ihep.ac.cn

  • CPC Website

  • IOP Website

  • CPC WeChat

Copyright © Institute of High Energy Physics, Chinese Academy of Sciences, 19B Yuquan Road, Beijing 100049, China 京ICP备05002789号-1

Supported by: Beijing Renhe Information Technology Co. Ltd  E-mail: info@rhhz.net

/

DownLoad:  Full-Size Img  PowerPoint
Return
Return