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《中国物理C》(英文)编辑部
2024年10月30日

Scale-invariance in soft gamma repeaters

  • The statistical properties of the soft gamma repeater SGR J1550-5418 are investigated carefully. We find that the cumulative distributions of fluence, peak flux and duration can be well fitted by a bent power law, while the cumulative distribution of waiting time follows a simple power law. In particular, the probability density functions of fluctuations of fluence, peak flux, and duration have a sharp peak and fat tails, which can be well fitted by a q-Gaussian function. The q values keep approximately steady for different scale intervals, indicating a scale-invariant structure of soft gamma repeaters. Those results support that the origin of soft gamma repeaters is crustquakes of neutron stars with extremely strong magnetic fields.
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  • [1] E. P. Mazets, S. V. Golenetskii, V. N. Il'inskii et al, Nature,282: 587 (1979)
    [2] E. P. Mazets, S. V. Golenetskij, and Y. A. Guryan, Soviet AstronomyLetters, 5: 343 (1979)
    [3] K. Hurley, Advances in Space Research, 47: 1326 (2011).
    [4] P. M. Woods, Advances in Space Research, 33: 630 (2004)
    [5] E. Ggş, C. Kouveliotou, P. M. Woods et al, The AstrophysicalJournal, 558: 228 (2001)
    [6] R. L. Aptekar, D. D. Frederiks, S. V. Golenetskii et al, TheAstrophysical Journal Supplement Series, 137: 227 (2001)
    [7] S. Mereghetti, The Astronomy and Astrophysics Review, 15:225 (2008)
    [8] R. C. Duncan and C. Thompson, The Astrophysical Journal,392: L9 (1992)
    [9] C. Kouveliotou, S. Dieters, T. Strohmayer et al, Nature, 393:235 (1998)
    [10] C. Kouveliotou, T. Strohmayer, K. Hurley et al, The AstrophysicalJournal, 510: L115 (1999)
    [11] C. Thompson, M. Lyutikov, and S. Kulkarni, The AstrophysicalJournal, 574: 332 (2002)
    [12] C. Thompson and R. C. Duncan, The Astrophysical Journal,473: 322 (1996)
    [13] F. P. Gavriil, V. M. Kaspi, and P. M. Woods, Nature, 419: 142(2002)
    [14] R. C. Lamb and T. H. Markert, The Astrophysical Journal,244: 94 (1981)
    [15] M. Sugizaki, K. Mitsuda, H. Kaneda et al, The AstrophysicalJournal Supplement Series, 134: 77 (2001)
    [16] J. D. Gelfand and B. M. Gaensler, The Astrophysical Journal,667: 1111 (2007)
    [17] F. Camilo, S. M. Ransom, J. P. Halpern et al, The AstrophysicalJournal Letters, 666: L93 (2007)
    [18] G. L. Israel, P. Esposito, N. Rea et al, Monthly Notices of the Royal Astronomical Society, 408: 1387 (2010)
    [19] P. Scholz and V. M. Kaspi, The Astrophysical Journal, 739: 94 (2011)
    [20] A. von Kienlin, D. Gruber, C. Kouveliotou et al, The Astrophysical Journal, 755: 150 (2012)
    [21] A. J. van der Horst, C. Kouveliotou, N. M. Gorgone et al, The Astrophysical Journal, 749: 122 (2012)
    [22] G. Younes, C. Kouveliotou, A. J. van der Horst et al, The Astrophysical Journal, 785: 52 (2014)
    [23] D. Palmer, GRB Coordinates Network, Circular Service, 8901(2009)
    [24] C. Kouveliotou, A. von Kienlin, G. Fishman et al, GRB Coordinates Network, Circular Service, 8915 (2009)
    [25] A. C. Collazzi, C. Kouveliotou, A. J. van der Horst et al, The Astrophysical Journal Supplement Series, 218: 11 (2015)
    [26] B. Cheng, R. I. Epstein, R. A. Guyer et al, Nature, 382: 518(1996)
    [27] Z. Prieskorn and P. Kaaret, The Astrophysical Journal, 755:1 (2012)
    [28] E. Ggş, P. M. Woods, C. Kouveliotou et al, The Astrophysical Journal Letters, 526: L93 (1999)
    [29] E. Ggş, P. M. Woods, C. Kouveliotou et al, The Astrophysical Journal Letters: 532: L121 (2000)
    [30] F. Y. Wang and H. Yu (2016), arXiv:1604.08676
    [31] P. Wang, Z. Chang, H. Wang et al, The European Physical Journal B, 88: 1 (2015)
    [32] F. Caruso, A. Pluchino, V. Latora et al, Phys. Rev. E, 75: 055101 (2007)
    [33] D. Freedman and P. Diaconis, Probability theory and related fields, 57: 453 (1981)
    [34] G. A. F. Seber and C. J. Wild, Nonlinear regression (Hoboken, NJ : Wiley-Interscience, 2003)
    [35] P. R. Bevington and D. K. Robinson, Data reduction and error analysis for the Physical Sciences (McGraw-Hill, 2003)
    [36] C. Guidorzi, S. Dichiara, and L. Amati, AA, 589: A98 (2016)
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Get Citation
null. Scale-invariance in soft gamma repeaters[J]. Chinese Physics C, 2017, 41(6): 065104. doi: 10.1088/1674-1137/41/6/065104
null. Scale-invariance in soft gamma repeaters[J]. Chinese Physics C, 2017, 41(6): 065104.  doi: 10.1088/1674-1137/41/6/065104 shu
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Received: 2016-11-28
Revised: 2017-01-20
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    Supported by National Natural Science Foundation of China (11375203, 11675182, 11690022, 11603005), and Fundamental Research Funds for Central Universities (106112016CDJCR301206)}

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Scale-invariance in soft gamma repeaters

Fund Project:  Supported by National Natural Science Foundation of China (11375203, 11675182, 11690022, 11603005), and Fundamental Research Funds for Central Universities (106112016CDJCR301206)}

Abstract: The statistical properties of the soft gamma repeater SGR J1550-5418 are investigated carefully. We find that the cumulative distributions of fluence, peak flux and duration can be well fitted by a bent power law, while the cumulative distribution of waiting time follows a simple power law. In particular, the probability density functions of fluctuations of fluence, peak flux, and duration have a sharp peak and fat tails, which can be well fitted by a q-Gaussian function. The q values keep approximately steady for different scale intervals, indicating a scale-invariant structure of soft gamma repeaters. Those results support that the origin of soft gamma repeaters is crustquakes of neutron stars with extremely strong magnetic fields.

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