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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(11) : 115101 DOI: 10.1088/1674-1137/41/11/115101

Two-flavor hybrid stars with the Dyson-Schwinger quark model

  • 1.

      School of Mathematics and Physics, China University of Geosciences, Lumo Road 388, Wuhan 430074, China

  • 2.

      INFN Sezione di Catania, Dipartimento di Fisica, Universitá

  • We study the properties of two-flavor quark matter in the Dyson-Schwinger model and investigate the possible consequences for hybrid neutron stars, with particular regard to the two-solar-mass limit. We find that with some extreme values of the model parameters, the mass fraction of two-flavor quark matter in heavy neutron stars can be as high as 30 percent and the possible energy release during the conversion from nucleonic neutron stars to hybrid stars can reach 1052 erg.
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  • References

    [1] N. K. Glendenning, Compact Stars, Nuclear Physics, Particle Physics, and General Relativity, Second edition, (New York:Springer-Verlag, 2000)
    [2] P. B. Demorest, T. Pennucci, S. M. Ransom, M. S. E. Roberts, and J. W. T. Hessels, Nature, 467:1081(2010)
    [3] J. A. Antoniadis et al, Science, 340:6131(2013)
    [4] E. Fonseca et al, Astrophys. J., 832:167(2016)
    [5] M. Buballa et al, J. Phys. G:Nucl. Part. Phys., 41:123001(2014)
    [6] F. Weber, G. A. Contrera, M. G. Orsaria, W. Spinella, and O. Zubairi, Mod. Phys. Lett. A, 29:1430022(2014)
    [7] M. Orsaria, H. Rodrigues, F. Weber, and G. A. Contrera, Phys. Rev. C, 89:015806(2014)
    [8] A. Drago, A. Lavagno, and G. Pagliara, Phys. Rev. D, 89:043014(2014)
    [9] D. Alvarez-Castillo, A. Ayriyan, S. Benic, D. Blaschke, H. Grigorian, and S. Typel, Eur. Phys. J. A, 52:69(2016)
    [10] M. G. Alford and S. Han, Eur. Phys. J. A, 52:62(2016)
    [11] Z. Dai, Q. Peng, and T. Lu, Astrophys. J., 440:815(1995)
    [12] A. Drago, A. Lavagno, and I. Parenti, Astrophys. J., 659:1519(2007)
    [13] T. Klhn et al, Phys. Lett. B, 654:170(2007)
    [14] S. Furusawa, T. Sanada, and S. Yamada, Phys. Rev. D, 93:043018(2016)
    [15] H. Chen, M. Baldo, G. F. Burgio, and H.-J. Schulze, Phys. Rev. D, 84:105023(2011)
    [16] H. Chen, J. B. Wei, M. Baldo, G. F. Burgio, and H.-J. Schulze, Phys. Rev. D, 91:105002(2015)
    [17] H. Chen, J. B. Wei, and H.-J. Schulze, Eur. Phys. J. A, 52:291(2016)
    [18] M. Baldo, I. Bombaci, and G. F. Burgio, Astron. Astrophys., 328:274(1997)
    [19] X. R. Zhou, G. F. Burgio, U. Lombardo, H.-J. Schulze, and W. Zuo, Phys. Rev. C, 69:018801(2004)
    [20] H.-J. Schulze, A. Polls, A. Ramos, and I. Vidana, Phys. Rev. C, 73:058801(2006)
    [21] Z. H. Li and H.-J. Schulze, Phys. Rev. C, 78:028801(2008)
    [22] V. Baluni, Phys. Rev. D, 17:2092(1978)
    [23] E. S. Fraga, R. D. Pisarski, and J. Schaffner-Bielich, Phys. Rev. D, 63:121702(R) (2001)
    [24] A. Kurkela, P. Romatschke, and A. Vuorinen, Phys. Rev. D, 81:105021(2010)
    [25] J. F. Xu, G. X. Peng, F. Liu, D. F. Hou, and L. W. Chen, Phys. Rev. D, 92:025025(2015)
    [26] G. N. Fowler, S. Raha, and R. M. Weiner, Z. Phys. C, 9:271(1981)
    [27] S. Chakrabarty, Phys. Rev. D, 43:627(1991)
    [28] O. G. Benvenuto and G. Lugones, Phys. Rev. D, 51:1989(1995)
    [29] A. Li, R. X. Xu, and J. F. Lu, MNRAS, 402:2715(2010)
    [30] J. R. Torres and D. P. Menezes, Eur. Phys. Lett., 101:42003(2013)
    [31] M. Buballa, Phys. Rep., 407:205(2005)
    [32] K. Schertler, S. Leupold, and J. Schaffner-Bielich, Phys. Rev. C, 60:025801(1999)
    [33] T. Klhn, R. Lastowiecki, and D. Blaschke, Phys. Rev. D, 88:085001(2013)
    [34] P. C. Chu et al, Phys. Rev. D, 93:094032(2016); P. C. Chu et al, Phys. Rev. D, 94:123014(2016)
    [35] A. Zacchi, R. Stiele, and J. Schaffner-Bielich, Phys. Rev. D, 92:045022(2015)
    [36] A. Peshier, B. Kmpfer, and G. Soff, Phys. Rev. C, 61:045203(2000)
    [37] Y. L. Tian, Y. Yan, H. Li, X. L. Luo, and H. S. Zong, Phys. Rev. D, 85:045009(2012)
    [38] T. Zhao, Y. Yan, X. L. Luo, and H. S. Zong, Phys. Rev. D, 91:034018(2015)
    [39] A. Li, W. Zuo, and G. X. Peng, Phys. Rev. C, 91:035803(2015)
    [40] C. D. Roberts and A. G. Williams, Prog. Part. Nucl. Phys., 33:477(1994)
    [41] R. Alkofer and L. von Smekal, Phys. Rep., 353:281(2001)
    [42] A. Maas, Phys. Rep., 524:203(2013)
    [43] C. D. Roberts, M. S. Bhagwat, A. Hll, and S. V. Wright, Eur. Phys. J. Special Topics, 140:53(2007)
    [44] C. S. Fischer and R. Williams, Phys. Rev. Lett., 103:122001(2009)
    [45] L. Chang and C. D. Roberts, Phys. Rev. Lett., 103:081601(2009)
    [46] L. Chang, I. C. Clot, C. D. Roberts, S. M. Schmidt, and P. C. Tandy, Phys. Rev. Lett., 111:141802(2013)
    [47] G. Eichmann, R. Alkofer, A. Krassnigg, and D. Nicmorus, Phys. Rev. Lett., 104:201601(2010)
    [48] G. Eichmann, H. Sanchis-Alepuz, R. Williams, R. Alkofer, and C. S. Fischer, Prog. Part. Nucl. Phys., 91:1(2016)
    [49] C. D. Roberts and S. M. Schmidt, Prog. Part. Nucl. Phys., 45:S1(2000)
    [50] H. Chen, W. Yuan, L. Chang, Y. X. Liu, T. Klhn, and C. D. Roberts, Phys. Rev. D, 78:116015(2008)
    [51] C. S. Fischer, Phys. Rev. Lett., 103:052003(2009)
    [52] S. X. Qin, L. Chang, H. Chen, Y. X. Liu, and C. D. Roberts, Phys. Rev. Lett., 106:172301(2011)
    [53] F. Gao, S. X. Qin, Y. X. Liu, C. D. Roberts, and S. M. Schmidt, Phys. Rev. D, 89:076009(2014)
    [54] C. S. Fischer, L. Fister, J. Luecker, and J. M. Pawlowski, Phys. Lett. B, 732:273(2014)
    [55] C. S. Fischer, J. Luecker, and C. A. Welzbacher, Phys. Rev. D, 90:034022(2014)
    [56] T. Klhn and T. Fischer, Astrophys. J., 810:134(2015)
    [57] G. Eichmann, C. S. Fischer, and C. A. Welzbacher, Phys. Rev. D, 93:034013(2016)
    [58] F. Gao, J. Chen, Y. X. Liu, S. X. Qin, C. D. Roberts, and S. M. Schmidt, Phys. Rev. D, 93:094019(2016)
    [59] D. Mller, M. Buballa, and J. Wambach, Eur. Phys. J. A, 49:96(2013)
    [60] D. Mller, M. Buballa, and J. Wambach, arXiv:1603.02865[hep-ph].
    [61] T. Zhao, S. S. Xu, Y. Yan, X. L. Luo, X. J. Liu, and H. S. Zong, Phys. Rev. D, 92:054012(2015)
    [62] M. Baldo, Nuclear Methods and the Nuclear Equation of State:International Review of Nuclear Physics, Vol. 8(Singapore:World Scientific, 1999)
    [63] R. B. Wiringa, V. G. J. Stoks, and R. Schiavilla, Phys. Rev. C, 51:38(1995)
    [64] R. Machleidt, K. Holinde, and Ch. Elster, Phys. Rep., 149:1(1987);
    [65] R. Machleidt, Adv. Nucl. Phys., 19:189(1989)
    [66] M. M. Nagels, T. A. Rijken, and J. J. de Swart, Phys. Rev. D, 17:768(1978);
    [67] V. G. J. Stoks, R. A. M. Klomp, C. P. F. Terheggen, and J. J. de Swart, Phys. Rev. C, 49:2950(1994)
    [68] A. Lejeune, P. Grang, M. Martzolff, and J. Cugnon, Nucl. Phys. A, 453:189(1986);
    [69] W. Zuo, A. Lejeune, U. Lombardo, and J. F. Mathiot, Nucl. Phys. A, 706:418(2002);
    [70] Z. H. Li, U. Lombardo, H.-J. Schulze, and W. Zuo, Phys. Rev. C, 77:034316(2008)
    [71] J. Carlson, V. R. Pandharipande, and R. B. Wiringa, Nucl. Phys. A, 401:59(1983)
    [72] R. Schiavilla, V. R. Pandharipande, and R. B. Wiringa, Nucl. Phys. A, 449:219(1986)
    [73] B. S. Pudliner, V. R. Pandharipande, J. Carlson, S. C. Pieper, and R. B. Wiringa, Phys. Rev. C, 56:1720(1997)
    [74] G. Taranto, M. Baldo, and G. F. Burgio Phys. Rev. C, 87:045803(2013)
    [75] D. Miskowiec et al, Phys. Rev. Lett., 72:3650(1994)
    [76] C. Fuchs, Prog. Part. Nucl. Physics, 56:1(2006)
    [77] P. Danielewicz, R. Lacey, and W. G. Lynch, Science, 298:1592(2002)
    [78] H.-J. Schulze, M. Baldo, U. Lombardo, J. Cugnon, and A. Lejeune, Phys. Rev. C, 57:704(1998)
    [79] M. Baldo, G. F. Burgio, and H.-J. Schulze, Phys. Rev. C, 58:3688(1998)
    [80] M. Baldo, G. F. Burgio, and H.-J. Schulze, Phys. Rev. C, 61:055801(2000)
    [81] I. Vidaa, A. Polls, A. Ramos, M. Hjorth-Jensen, and V. G. J. Stoks, Phys. Rev. C, 61:025802(2000)
    [82] H.-J. Schulze and T. Rijken, Phys. Rev. C, 84:035801(2011)
    [83] Y. Jiang, H. Chen, W. M. Sun, and H. S. Zong, JHEP, 04:014(2013)
    [84] R. Alkofer, P. Watson, and H. Weigel, Phys. Rev. D, 65:094026(2002)
    [85] T. Klhn, C. D. Roberts, L. Chang, H. Chen, and Y. X. Liu, Phys. Rev. C, 82:035801(2010)
    [86] H. Chen, M. Baldo, G. F. Burgio, and H.-J. Schulze, Phys. Rev. D, 86:045006(2012)
    [87] N. K. Glendenning, Phys. Rev. D, 46:1274(1992)
    [88] T. Maruyama, S. Chiba, H.-J. Schulze, and T. Tatsumi, Phys. Rev. D, 76:123015(2007)
    [89] H. Chen, G. F. Burgio, H.-J. Schulze, and N. Yasutake, Astron. Astrophys., 551:A13(2013)
    [90] S. L. Shapiro and S. A. Teukolsky, Black Holes, White Dwarfs, and Neutron Stars, First edition, (New York:John Wiley Sons, 1983)
    [91] J. W. Negele and D. Vautherin, Nucl. Phys. A, 207:298(1973)
    [92] R. P. Feynman, N. Metropolis, and E. Teller, Phys. Rev., 75:1561(1949)
    [93] G. Baym, C. Pethick, and D. Sutherland, Astrophys. J., 170:299(1971)

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J. B. Wei, H. Chen and H. -J. Schulze. Two-flavor hybrid stars with the Dyson-Schwinger quark model[J]. Chinese Physics C, 2017, 41(11): 115101. doi: 10.1088/1674-1137/41/11/115101
J. B. Wei, H. Chen and H. -J. Schulze. Two-flavor hybrid stars with the Dyson-Schwinger quark model[J]. Chinese Physics C, 2017, 41(11): 115101.  doi: 10.1088/1674-1137/41/11/115101 shu
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Received: 2017-02-16
Revised: 2017-07-14
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    Supported by NSFC (11305144, 11475149, 11303023), Central Universities (CUGL 140609) in China, NewCompStar, COST Action MP1304

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Two-flavor hybrid stars with the Dyson-Schwinger quark model

    Corresponding author: H. -J. Schulze, huanchen@cug.edu.cn
  • 1.  School of Mathematics and Physics, China University of Geosciences, Lumo Road 388, Wuhan 430074, China
  • 2.  INFN Sezione di Catania, Dipartimento di Fisica, Universitá
  • Received Date: 2017-02-16
  • Accepted Date: 2017-07-14
  • Available Online: 2017-11-05
Fund Project:  Supported by NSFC (11305144, 11475149, 11303023), Central Universities (CUGL 140609) in China, NewCompStar, COST Action MP1304

Abstract: We study the properties of two-flavor quark matter in the Dyson-Schwinger model and investigate the possible consequences for hybrid neutron stars, with particular regard to the two-solar-mass limit. We find that with some extreme values of the model parameters, the mass fraction of two-flavor quark matter in heavy neutron stars can be as high as 30 percent and the possible energy release during the conversion from nucleonic neutron stars to hybrid stars can reach 1052 erg.

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