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> 2018, Vol. 42> Issue(5) : 054103 DOI: 10.1088/1674-1137/42/5/054103

Crust-core properties of neutron stars in the Nambu-Jona-Lasinio model

  • 1.

     School of Physics, Southeast University, Nanjing 211189, China

  • We adopt the Nambu-Jona-Lasinio (NJL) model to study the crust-core transition properties in neutron stars (NSs). For a given momentum cutoff and symmetry energy of saturation density in the NJL model, decreasing the slope of the symmetry energy gives rise to an increase in the crust-core transition density and transition pressure. Given the slope of the symmetry energy at saturation density, the transition density and corresponding transition pressure increase with increasing symmetry energy. The increasing trend between the fraction of the crustal moment of inertia and the slope of symmetry energy at saturation density indicates that a relatively large momentum cutoff of the NJL model is preferred. For a momentum cutoff of 500 MeV, the fraction of the crustal moment of inertia clearly increases with the slope of symmetry energy at saturation density. Thus, at the required fraction (7%) of the crustal moment of inertia, the NJL model with momentum cutoff of 500 MeV and a large slope of the symmetry energy of saturation density can give the upper limit of the mass of the Vela pulsar to be above 1.40 M⊙.
      PCAS:
  • 加载中

  • References

    [1] J. M. Lattimer, M. Prakash, Astrophys. J., 550:426(2001)
    [2] M. Ruderman, Nature, 223:597(1969)
    [3] D. Pines, J. Shaham, M. Ruderman, Nat. Phys. Sci., 237:83(1972)
    [4] P. W. Anderson and N. Itoh, Nature (London), 256:25(1975)
    [5] D. Pines, M. Alpar, Nature, 316:27(1985)
    [6] B. Link, R. I. Epstein, and J. M. Lattimer, Phys. Rev. Lett., 83:3362(1999)
    [7] J. M. Lattimer, M. Prakash, Science, 304:536(2004)
    [8] J. M. Lattimer, M. Prakash, Phys. Rep., 442:109(2007)
    [9] N. Chamel, Phys. Rev. Lett., 110:011101(2013)
    [10] J. Piekarewicz, F. J. Fattoyev, C. J. Horowitz, Phys. Rev.C, 90:015803(2014)
    [11] N. Andersson, K. Glampedakis, W. C. G. Ho, and C. M. Espinoza, Phys. Rev. Lett., 109:241103(2012)
    [12] N. Chamel, Phys. Rev. C, 85:035801(2012)
    [13] M. Bigdeli and S. Elyasi, Eur. Phys. J. A, 51(3):38(2015)
    [14] J. Xu, L. W. Chen, B. A. Li, and H. R. Ma, Astrophys. J., 697:1549-1568(2009)
    [15] Ch. C. Moustakidis et al, Phys. Rev. C, 81:065803(2010)
    [16] C. Ducoin et al, Phys. Rev. C, 83:045810(2011)
    [17] Y. Nambu, G. J. Lasinio, Phys. Rev., 122:345(1961)
    [18] U. Vogl and W. Weise, Prog. Part. Nucl. Phys., 27:195-272(1991)
    [19] N. D. Merrnin, Rev. Mod. Phys., 64:3-49(1992); Rev. Mod. Phys., 64:1163-1163(1992); Rev. Mod. Phys., 64:635-635(1992); Rev. Mod. Phys., 66:249-249(1994)
    [20] M. Buballa, Phys. Rept., 407:205-376(2005)
    [21] V. Koch, T. S. Biro, J. Kunz, and U. Mosel, Phys. lett. B, 185:1(1987)
    [22] I. N. Mishustin, L. M. Satarov, and W. Greiner, Phys. Rep., 391:363(2004)
    [23] C. Da. Providencia, J. Da. Providencia, and S. A. Moszkowski, Int. J. Mod. Phys. B, 17:5208(2003)
    [24] S. N. Wei, W. Z. Jiang, R. Y. Yang, and D. R. Zhang, Phys. Lett. B, 763:145-150(2016)
    [25] T. J. Brvenich and D. G. Madland, Nucl. Phys. A, 729:769(2003)
    [26] H. Pais, D. P. Menezes, and C. Providencia, Phys. Rev. C, 93:065805(2016)
    [27] S. Kubis, Phys. Rev. C, 70:065804(2004)
    [28] S. Kubis, Phys. Rev. C, 76:025801(2007)
    [29] X. D. Ji, Phys. Rev. Lett., 74:1071(1995)
    [30] M. Procura, B. U. Musch, T. Wollenweber, T. R. Hemmert, and W. Weise, Phys. Rev. D, 73:114510(2006)
    [31] W. G. Lynch, M. B. Tsang, Y. Zhang, P. Danielewicz, M. Famiano, Z. Li, and A. W. Steiner, Prog. Part. Nucl. Phys., 62:427(2009)
    [32] C. Fuchs, Prog. Part. Nucl. Phys., 56:1(2006)
    [33] I. Sagert, L. Tolos, D. Chatterjee, J. Schaffner-Bielich, and C. Sturm, Phys. Rev. C, 86:045802(2012)
    [34] C. Fuchs, A. Faessler, E. Zabrodin, and Y. M. Zheng, Phys. Rev. Lett., 86:1974(2001)
    [35] P. Danielewicz, R. Lacey, and W. G. Lynch, Science, 298:1592(2002)
    [36] G. A. Lalazissis, J. Konig, and P. Ring,Phys. Rev. C, 55:540(1997)
    [37] M. M. Sharma, M. A. Nagarajan, and P. Ring, Phys. Lett. B, 312:377(1993)
    [38] Y. Sugahara and H. Toki, Nucl. Phys. A, 579:557(1994)
    [39] B. A. Li and X. Han, Phys. Lett. B, 727:276(2013)
    [40] L. W. Chen, C. M. Ko, B. A. Li, and J. Xu, Phys. Rev. C, 82:024321(2010)
    [41] L. W. Chen, Nucl. Phys. Rev., 31:273(2014)
    [42] C. Xu, B. A. Li, L. W. Chen, Phys. Rev. C, 82:054607(2010)
    [43] M. B. Tsang, J. R. Stone, F. Camera, P. Danielewicz et al, Phys. Rev. C, 86:015803(2012)
    [44] M. B. Tsang, Y. X. Zhang, P. Danielewicz, M. Famiano, Z. X. Li, W. G. Lynch, and A. W. Steiner, Phys. Rev. Lett., 102:122701(2009); ibid., Int. J. Mod. Phys. E, 19:1631(2010)
    [45] N. Wang, M. Liu, L. Ou, and Y. Zhang, Phys. Lett. B, 751:553(2015)
    [46] J. M. Lattimer and Y. Lim, Astrophys. J., 771:51(2013)
    [47] A. W. Steiner, S. Gandolfi, Phys. Rev. Lett., 108:081102(2012)
    [48] X. Roca-Maza, M. Brenna, B. K. Agrawal, P. F. Bortignon, G. Col'o, Li-Gang Cao, N. Paar, and D. Vretenar, Phys. Rev. C, 87:034301(2013)
    [49] D. V. Shetty, S. J. Yennello, G. A. Souliotis, Phys. Rev. C, 76:024606(2007)
    [50] P. Danielewicz and J. Lee, Nucl. Phys. A, 818:36(2009)
    [51] M. Gearheart, W. G. Newton, J. Hooker, and B. A. Li, Mon. Not. R. Astron. Soc., 418:2343(2011)
    [52] H. Sotani, K. Nakazato, K. Iida, and K. Oyamatsu, Mon. Not. R. Astron. Soc., 428:L21(2013)
    [53] W. G. Newton, B. A. Li, Phys. Rev. C, 80:065809(2009)
    [54] J. M. Lattimer and A. W. Steiner, Eur. Phys. J. A, 50:40(2014)
    [55] S. Gandolfi, J. Carlson, and Sanjay Reddy, Phys. Rev. C, 85:032801(2012)
    [56] K. Hebeler, J. M. Lattimer, C. J. Pethick, and A. Schwenk, Astrophys. J, 773:11(2013)
    [57] J. Oppenheimet and G. Volkoff, Phys. Rev., 55:374(1939)
    [58] R. C. Tolman, Phys. Rev., 55:364(1939)
    [59] G. Baym, C. Pethick, and P. Sutherland, Astrophys. J., 170:299(1971)
    [60] K. Iida and K. Sato, Astrophys. J., 477:294(1997)
    [61] P. Demorest, T. Pennucci, S. Ransom, M. Roberts, and J. Hessels, Nature, 467:1081(2010)
    [62] J. Antoniadis, P. C. Freire, N. Wex, T. M. Tauris, R. S. Lynch et al, Science, 340:1233232(2013)
    [63] A. W. Steiner, J. M. Lattimer, and E. F. Brown, Astrophys. J, 722:33(2010)
    [64] A. W. Steiner, J. M. Lattimer, and E. F. Brown, Astrophys. J., 765:L5(2013)
    [65] S. Guillot, M. Servillat, N. A. Webb, and R. E. Rutledge, Astrophys. J, 772:7(2013)
    [66] F. zel, G. Baym, and T. Guver, Phys. Rev. D, 82:101301(2010)
    [67] V. Suleimanov, J. Poutanen, M. Revnivtsev, and K. Werner, Astrophys. J, 742:122(2011)
    [68] S. Bogdanov, Astrophys. J., 762:96(2013)
    [69] J. Poutanen et al, Mon. Not. R. Astron. Soc., 442:3777(2014)
    [70] C. O. Heinke, H. N. Cohn, P. M. Lugger, N. A. Webb et al, Mon. Not. R. Astron. Soc., 444:443(2014)
    [71] J. M. Lattimer, A. W. Steiner, Astrophys. J., 784:123(2014)
    [72] B. A. Li, A. W. Steiner, Phys. Lett. B, 642:436(2006)
    [73] W. Z. Jiang, B. A. Li, L. W. Chen, Phys. Lett. B, 653:184(2007)
    [74] G. Watanabe and C. J. Pethick, Phys. Rev. Lett., 119:062701(2017)
    [75] J. M. Lattimer and M. Prakash. Phys. Rep., 333:121(2000)
    [76] G. G. Pavlov, V. E. Zavlin, D. Sanwal, V. Burwitz, and G. P. Garmire, Astrophys. J., 552:L129(2001)

  • Access

    加载中

Get Citation
Si-Na Wei, Rong-Yao Yang and Wei-Zhou Jiang. Crust-core properties of neutron stars in the Nambu-Jona-Lasinio model[J]. Chinese Physics C, 2018, 42(5): 054103. doi: 10.1088/1674-1137/42/5/054103
Si-Na Wei, Rong-Yao Yang and Wei-Zhou Jiang. Crust-core properties of neutron stars in the Nambu-Jona-Lasinio model[J]. Chinese Physics C, 2018, 42(5): 054103.  doi: 10.1088/1674-1137/42/5/054103 shu
Milestone
Received: 2017-10-25
Revised: 2018-02-25
Fund

    Supported by National Natural Science Foundation of China (11775049, 11275048) and the China Jiangsu Provincial Natural Science Foundation (BK20131286)

Article Metric

Article Views(1627)
PDF Downloads(31)
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:

Crust-core properties of neutron stars in the Nambu-Jona-Lasinio model

    Corresponding author: Wei-Zhou Jiang,
  • 1. School of Physics, Southeast University, Nanjing 211189, China
  • Received Date: 2017-10-25
  • Accepted Date: 2018-02-25
  • Available Online: 2018-05-05
Fund Project:  Supported by National Natural Science Foundation of China (11775049, 11275048) and the China Jiangsu Provincial Natural Science Foundation (BK20131286)

Abstract: We adopt the Nambu-Jona-Lasinio (NJL) model to study the crust-core transition properties in neutron stars (NSs). For a given momentum cutoff and symmetry energy of saturation density in the NJL model, decreasing the slope of the symmetry energy gives rise to an increase in the crust-core transition density and transition pressure. Given the slope of the symmetry energy at saturation density, the transition density and corresponding transition pressure increase with increasing symmetry energy. The increasing trend between the fraction of the crustal moment of inertia and the slope of symmetry energy at saturation density indicates that a relatively large momentum cutoff of the NJL model is preferred. For a momentum cutoff of 500 MeV, the fraction of the crustal moment of inertia clearly increases with the slope of symmetry energy at saturation density. Thus, at the required fraction (7%) of the crustal moment of inertia, the NJL model with momentum cutoff of 500 MeV and a large slope of the symmetry energy of saturation density can give the upper limit of the mass of the Vela pulsar to be above 1.40 M⊙.

    HTML

Reference (76)

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