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《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2017, Vol. 41> Issue(7) : 075101 DOI: 10.1088/1674-1137/41/7/075101

Neutrino emissivity of the nucleon direct URCA process for rotational traditional and hyperonic neutron stars

  • 1.

      Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment,Institute of Space Sciences, Shandong University, Weihai 264209, China

  • 2.

      School of Nuclear Science and Technology, Lanzhou University, Lanzhou 730000, China

  • Based on covariant density functional theory, we study the effects of rotation on the nucleon direct URCA (N-DURCA) process for traditional and hyperonic neutron stars. The calculated results indicate that, for a fixed mass sequence of rotational traditional neutron stars, the neutrino emissivity of the star is nearly invariant with increasing frequency, while it always increases for rotational hyperonic neutron stars. Thus, rotation has different effects on the N-DURCA process for these two kinds of neutron stars.
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  • References

    [1] S. L. Shapiro, S. A. Teukolsky, Black Holes, White Dwarfs, and Neutron Stars: The Physics of Compact Objects (New York: A Wiley-Interscience Publication, 1983)
    [2] J. M. Lattimer, C. J. Pethick, M. Prakash, and P. Haensel, Phys. Rev. Lett., 66: 21 (1991)
    [3] D. G. Yakovlev, O. Y. Gnedin, A. D. Kaminker, and A. Y. Potekhin, AIP Conf. Proc., 983: 379 (2008)
    [4] D. Page, U. Geppert, and F. Weber, Nucl. Phys. A, 777: 497 (2006)
    [5] D. G. Yakovlev, A. D. Kaminkera, O. Y. Gnedinc, and P. Haenseld, Physics Reports, 354: 1 (2001)
    [6] N. K. Glendenning, Astrophys. J., 293: 470 (1985)
    [7] W. B. Ding, Z. Yu, and Y. H. Liu, Chin. Phys. Lett., 28: 072601 (2011)
    [8] Y. Xu, G. Z. Liu, Y. R. Wu, M. F. Zhu, Z. Yu, H. Y. Wang, and E. G. Zhao, Chin. Phys. Lett., 28: 079701 (2011)
    [9] Y. Xu, G. Z. Liu, C. Z. Liu, C. B. Fan, H. Y. Wang, M. F. Zhu, and E. G. Zhao, Chin. Phys. Lett., 30: 129501 (2013)
    [10] Y. Xu, G. Z. Liu, C. Z. Liu, C. B. Fan, X. W. Han, X. J. Zhang, H. Y. Wang, M. F. Zhu, and Y. Meng, Chin. Sci. Bull., 59: 273 (2014)
    [11] Y. Xu, X. L. Huang, X. J. Zhang, T. Bao, L. Xiao, C. B. Fan, and C. Z, Liu, arXiv:1509.05150v4 (2016)
    [12] M. Prakash, M. Prakash, J. M. Lattimer, and C. J. Pethick, Astrophys. J.,390: L77 (1992)
    [13] C. Schaab, S. Balberg, and J. Schaffner-Bielich, Astrophys. J.,504: L99 (1998)
    [14] D. Page, M. Prakash, J. M. Lattimer, and A. Steiner, Phys. Rev. Lett.,85: 2048 (2000)
    [15] I. Vidana and L. Tolos, Phys. Rev. C,70: 028802 (2004)
    [16] P. G. Krastev, B. A. Li, and A. Worley, Astrophys. J., 676: 1170 (2008)
    [17] R. Negreiros, S. Schramm, and F. Weber, Astron. Nachr., 335: 703 (2014)
    [18] J. Meng, H. Toki, S. G. Zhou, S. Q. Zhang, W. H. Long, and L. S. Geng, Prog. Part. Nucl. Phys., 57: 470 (2006)
    [19] P. Ring, Prog. Part. Nucl. Phys., 37: 193 (1996)
    [20] S. F. Ban, J. Li, S. Q. Zhang, H. Y. Jia, J. P. Sang, and J. Meng, Phys. Rev. C, 69: 045805 (2004)
    [21] N. B. Zhang, B. Qi, S. Y. Wang, S. L. Ge, and B. Y. Sun, Int. Jou. Mod. Phys. E, 22: 1350085 (2013)
    [22] C. Y. Ryua, M. K. Cheouna, T. Kajinob, T. Maruyamad, and G. J. Mathewse, Astroparticle Physics, 38: 25 (2012)
    [23] T. Miyatsu, S. Yamamuro, and K. Nakazato, Astrophys. J., 774: 4 (2013)
    [24] J. N. Hu, A. Li, H. Toki, and W. Zuo, Phys. Rev. C, 89: 025802 (2014)
    [25] H. Fujii, T. Maruyama, T. Muto, and T. Tatsumi, Nucl. Phys. A, 597: 645 (1996)
    [26] N. K. Glendenning, and J. Schaffner-Bielich, Phys. Rev. Lett., 81: 4564 (1998)
    [27] W. Z. Jiang, B. A. Li, and L. W. Chen, Astrophys. J., 756: 56 (2012)
    [28] D. B. Kaplan, and A. E. Nelson, Phys. Lett. B, 175: 57 (1986)
    [29] B. Y. Sun, W. H. Long, J. Meng, and U. Lombardo, Phys. Rev. C, 78: 065805 (2008)
    [30] S. Wang, H. F. Zhang, and J. M. Dong, Phys. Rev. C, 90: 055801 (2014)
    [31] B. Qi, N. B. Zhang, S. Y. Wang, and B. Y. Sun, Chin. Phys. Lett., 32: 112101 (2015)
    [32] B. Qi, N. B. Zhang, B. Y. Sun, S. Y. Wang, and J. H. Gao, RAA, 16: 60 (2016)
    [33] T. Miyatsu, M. K. Cheoun, and K. Saito, Phys. Rev. C, 88: 015802 (2013)
    [34] P. A. M. Guichon, Phys. Lett. B, 200: 235 (1988)
    [35] K. Saito, and A. W. Thomas, Phys. Lett. B, 327: 9 (1994)
    [36] P. A. M. Guichon, A. W. Thomas, and K. Tsushima, Nucl. Phys. A, 814: 66 (2008)
    [37] T. Miyatsu, and K. Saito, PThPh, 122: 1035 (2010)
    [38] S. Nagai, T. Miyatsu, K. Saito, and K. Tsushima, Phys. Lett. B, 666: 239 (2008)
    [39] N. K. Glendenning, Compact Stars, Nuclear Physics, ParticlePhysics and General Relativity, 2nd ed. (Springer-Verlag, New York, 2000)
    [40] W. H. Long, J. Meng, N. Van Giai, and S. G. Zhou, Phys. Rev. C, 69: 034319 (2004)
    [41] Y. Sugahara, and H. Toki, Prog. Theor. Phys., 92: 803 (1994)
    [42] S. A. Moszkowski, Phys. Rev. D, 9: 1613 (1974)
    [43] J. W. Negele, and D. Vautherin, Nucl. Phys. A, 207: 298 (1973)
    [44] G. Baym, C. Pethick, and D. Sutherland, Astrophys. J., 170: 299 (1971)
    [45] J. Rikovska-Stone, G P. A. M. uichon, H. H. Matevosyan, and A. W. Thomas, Nucl. Phys. A, 792: 341 (2007)
    [46] D. L. Whittenbury, J. D. Carroll, A. W. Thomas, K. Tsushima, and J. R. Stone, arXiv:1204.2614 (2012)
    [47] N. Stergioulas, Living Rev. Relativ., 6: 3 (2003)
    [48] H. Komatsu, Y. Eriguchi, and I. Hachisu, MNRAS, 237: 355 (1989)
    [49] G. B. Cook, S. L. Shapiro, and S. A. Teukolsky, Astrophys. J., 424: 823 (1994)
    [50] N. Stergioulas, and J. L. Friedman, Astrophys. J., 444: 306 (1995)
    [51] T. Nozawa, N. Stergioulas, E. Gourgoulhon, and Y. Eriguchi, A A, 132: 431 (1998)
    [52] L. B. Leinson, and A. Prez, Phys. Lett. B, 518: 15 (2001a)
    [53] L. B. Leinson, and A. Prez, Phys. Lett. B, 522: 358 (2001b)

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Nai-Bo Zhang, Shou-Yu Wang, Bin Qi, Jian-Hua Gao and Bao-Yuan Sun. Neutrino emissivity of the nucleon direct URCA process for rotational traditional and hyperonic neutron stars[J]. Chinese Physics C, 2017, 41(7): 075101. doi: 10.1088/1674-1137/41/7/075101
Nai-Bo Zhang, Shou-Yu Wang, Bin Qi, Jian-Hua Gao and Bao-Yuan Sun. Neutrino emissivity of the nucleon direct URCA process for rotational traditional and hyperonic neutron stars[J]. Chinese Physics C, 2017, 41(7): 075101.  doi: 10.1088/1674-1137/41/7/075101 shu
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Received: 2017-01-18
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    Supported by National Natural Science Foundation of China (11545011, 11405096), the Shandong Natural Science Foundation (ZR2014AQ012), the Young Scholars Program of Shandong University, Weihai (2015WHWLJH01) and the Fundamental Research Funds for the Central Universities (lzujbky-2016-30)

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Neutrino emissivity of the nucleon direct URCA process for rotational traditional and hyperonic neutron stars

    Corresponding author: Shou-Yu Wang,
    Corresponding author: Bin Qi,
  • 1.  Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment,Institute of Space Sciences, Shandong University, Weihai 264209, China
  • 2.  School of Nuclear Science and Technology, Lanzhou University, Lanzhou 730000, China
  • Received Date: 2017-01-18
  • Available Online: 2017-07-05
Fund Project:  Supported by National Natural Science Foundation of China (11545011, 11405096), the Shandong Natural Science Foundation (ZR2014AQ012), the Young Scholars Program of Shandong University, Weihai (2015WHWLJH01) and the Fundamental Research Funds for the Central Universities (lzujbky-2016-30)

Abstract: Based on covariant density functional theory, we study the effects of rotation on the nucleon direct URCA (N-DURCA) process for traditional and hyperonic neutron stars. The calculated results indicate that, for a fixed mass sequence of rotational traditional neutron stars, the neutrino emissivity of the star is nearly invariant with increasing frequency, while it always increases for rotational hyperonic neutron stars. Thus, rotation has different effects on the N-DURCA process for these two kinds of neutron stars.

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