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
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.
      PCAS:
  • 加载中

  • 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)

  • Access

    加载中

Get Citation
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
Milestone
Received: 2017-02-16
Revised: 2017-07-14
Fund

    Supported by NSFC (11305144, 11475149, 11303023), Central Universities (CUGL 140609) in China, NewCompStar, COST Action MP1304

Article Metric

Article Views(1584)
PDF Downloads(25)
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:

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.

    HTML

Reference (93)

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