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
×
近期发现有不法分子冒充我刊与作者联系，借此进行欺诈等不法行为，请广大作者加以鉴别，如遇诈骗行为，请第一时间与我刊编辑部联系确认（《中国物理C》（英文）编辑部电话：010-88235947,010-88236950），并作报警处理。
本刊再次郑重声明：
（1）本刊官方网址为cpc.ihep.ac.cn和https://iopscience.iop.org/journal/1674-1137
（2）本刊采编系统作者中心是投稿的唯一路径，该系统为ScholarOne远程稿件采编系统，仅在本刊投稿网网址（https://mc03.manuscriptcentral.com/cpc）设有登录入口。本刊不接受其他方式的投稿，如打印稿投稿、E-mail信箱投稿等，若以此种方式接收投稿均为假冒。
（3）所有投稿均需经过严格的同行评议、编辑加工后方可发表，本刊不存在所谓的“编辑部内部征稿”。如果有人以“编辑部内部人员”名义帮助作者发稿，并收取发表费用，均为假冒。
                  
《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2017, Vol. 41> Issue(12) : 125101 DOI: 10.1088/1674-1137/41/12/125101

Very high-frequency gravitational waves from magnetars and gamma-ray bursts

  • 1.

     Department of Physics, Chongqing University, Chongqing 401331, China

  • Extremely powerful astrophysical electromagnetic (EM) systems could be possible sources of high-frequency gravitational waves (HFGWs). Here, based on properties of magnetars and gamma-ray bursts (GRBs), we address "Gamma-HFGWs" (with very high-frequency around 1020 Hz) caused by ultra-strong EM radiation (in the radiation-dominated phase of GRB fireballs) interacting with super-high magnetar surface magnetic fields (~1011 T). By certain parameters of distance and power, the Gamma-HFGWs would have far field energy density Ωgw around 10-6 and they would cause perturbed signal EM waves of ~10-20 W/m2 in a proposed HFGW detection system based on the EM response to GWs. Specially, Gamma-HFGWs would possess distinctive envelopes with characteristic shapes depending on the particular structures of surface magnetic fields of magnetars, which could be exclusive features helpful to distinguish them from background noise. Results obtained suggest that magnetars could be involved in possible astrophysical EM sources of GWs in the very high-frequency band, and Gamma-HFGWs could be potential targets for observations in the future.
      PCAS:
  • 加载中

  • References

    [1] B. P. Abbott et al (LIGO Scientific Collaboration and Virgo Collaboration), Phys. Rev. Lett., 116(6):061102(2016)
    [2] B. P. Abbott et al (LIGO Scientific Collaboration and Virgo Collaboration), Phys. Rev. Lett., 116(24):241103(2016)
    [3] B. P. Abbott et al (LIGO Scientific Collaboration and Virgo Collaboration), Phys. Rev. Lett., 118:221101(2017)
    [4] B. P. Abbott et al (LIGO Scientific Collaboration and Virgo Collaboration), Phys. Rev. Lett., 119:141101(2017)
    [5] Y. Zhang, W. Zhao, Y. Yuan, and T. Xia, Chin. Phys. Lett., 22(7):1817(2005)
    [6] W. Zhao, M. Li, Phys. Lett. B, 737:329(2014)
    [7] W. Zhao, Y. Zhang, Phys. Rev. D, 74:083006(2006)
    [8] P. A. R. Ade, Y. Akiba, A. E. Anthony et al, Phys. Rev. Lett., 113(2):021301(2014)
    [9] D. Baskaran, L. P. Grishchuk, and A. G. Polnarev, Phys. Rev. D, 74:083008(2006)
    [10] A. G. Polnarev, N. J. Miller, and B. G. Keating, Mon. Not. R. Astron. Soc., 386:1053(2008)
    [11] U. Seljak, M. Zaldarriaga, Phys. Rev. Lett., 78:2054(1997)
    [12] J. R. Pritchard, M. Kamionkowski, Ann. Phys.(N.Y.), 318:3(2005)
    [13] M. Servin, G. Brodin, Phys. Rev. D, 68(4):044017(2003)
    [14] M. E. Gertsenshtein, Sov. Phys. JETP, 14:84(1962)
    [15] D. Boccaletti, V. De Sabbata, P. Fortint, and C. Gualdi, Nuovo Cim. B, 70:129(1970)
    [16] F. Y. Li, H. Wen, and Z. Y. Fang, Chin. Phys. B, 22:120402(2013)
    [17] F. Y. Li, H. Wen, Z. Y. Fang et al, Nucl. Phys. B, 911:500(2016)
    [18] F. Y. Li, M. X. Tang, and D. P. Shi, Phys. Rev. D, 67(10):104008(2003)
    [19] F. Y. Li, R. M. L. Baker, Z. Y. Fang, G. V. Stephenson, and Z. Y. Chen, Eur. Phys. J. C, 56:407(2008)
    [20] F. Y. Li, N. Yang, Z. Y. Fang, R. M. L. Baker, G. V. Stephenson, and H. Wen, Phys. Rev. D, 80(6):064013(2009)
    [21] H. Wen, F. Y. Li, Z. Y. Fang, Phys. Rev. D, 89(10):104025(2014)
    [22] H. Wen, F. Y. Li, Z. Y. Fang, and A. Beckwith, Eur. Phys. J. C, 74:2998(2014)
    [23] D. P. Shi, F. Y. Li, and Y. Zhang, Acta. Phys. Sin., 55:5041(2006)
    [24] J. Li, F. Y. Li, and Y. H. Zhong, Chin. Phys. B, 18:922(2009)
    [25] X. Li, S. Wang, H. Wen, Chin. Phys. C, 40(8):085101(2016)
    [26] T. Piran, Rev. Mod. Phys., 76(4):1143(2005)
    [27] B. D. Metzger, T. A. Thompson, and E. Quataert, Astro-phys. J., 659:561(2007)
    [28] T. Piran, Phys. Rep., 314:575(1999)
    [29] W. K. De Logi, A. R. Mickelson, Phys. Rev. D, 16(10):2915(1977)
    [30] K. H. Rdler, H. Fuchs, U. Geppert et al, Phys. Rev. D, 64(8):083008(2001)
    [31] C. Thompson, Astrophys. J., 688:1258(2008)
    [32] S. R. Kulkarni, S. G. Djorgovski, A. N. Ramaprakash et al, Nature, 393:35(1998)
    [33] S. R. Kulkarni, S. G. Djorgovski, S. C. Odewahn et al, Nature, 398:389(1999)
    [34] D. Eichler, M. Livio, T. Piran, and D. N. Schramm, Nature, 340:126(1999)
    [35] R. Narayan, B. Paczynski, and T. Piran, Astrophys. J. Lett., 395:L83(1992)
    [36] B. Paczynski, Acta Astron., 41:257(1991)
    [37] R. D. Blandford, R. L. Znajek, Mon. Not. R. Astron. Soc., 179:433(1977)
    [38] V. V. Usov, Nature, 357:472(1992)
    [39] V. V. Usov, Mon. Not. R. Astron. Soc., 267:1035(1994)
    [40] M. V. Smolsky, V. V. Usov, Astrophys. J., 461:858(1996)
    [41] M. V. Smolsky, V. V. Usov, Astrophys. J., 531:764(2000)
    [42] G. Drenkhahn, H. C. Spruit, Astron. Astrophys., 391:1141(2002)
    [43] H. C. Spruit, F. Daigne, and G. Drenkhahn, Astron. Astrophys., 369:694(2001)
    [44] D. Eichler, Mon. Not. R. Astron. Soc., 335:883(2002)
    [45] B. Zhang, P. Meszaros, Astrophys. J. Lett., 552:L35(2001)
    [46] T. A. Thompson, arXiv:astro-ph/0611368
    [47] A. Corsi, P. Mszros, Astrophys. J., 702:1171(2009)
    [48] Z. G. Dai, Astrophys. J., 606:1000(2004)
    [49] A. M. Pires, F. Haberl, V. E. Zavlin et al, Astron. Astrophys., 563:A50(2014)
    [50] C. Thompson, R. Gill, Astrophys. J., 791:46(2014)
    [51] D. Fargion, M. Grossi, Chin. J. Astron. Astrophys., 6:342(2006)
    [52] S. Dall'Osso, G. Stratta, D. Guetta et al, Astron. Astrophys., 526:A121(2011)
    [53] C. Thompson, R. C. Duncan, Astrophys. J., 561:980(2001)
    [54] C. Thompson, R. C. Duncan, Mon. Not. R. Astron. Soc., 275:255(1995)
    [55] Y. Kaneko, E. Gogus, C. Kouveliotou et al, Astrophys. J., 710:1335(2010)
    [56] B. D. Metzger, T. A. Thompson, and E. Quataert, AIP Conf. Proc., 1000:413(2008)
    [57] A. I. Ibrahim, T. E. Strohmayer, P. M. Woods et al, Astrophys. J., 558:237(2001)
    [58] J. J. Jia, Y. F. Huang, and K. S. Cheng, Astrophys. J., 677:488(2008)
    [59] G. L. Israel, P. Romano, V. Mangano et al, Astrophys. J., 685:1114(2008)
    [60] J. Goodman, Astrophys. J., 308:L47(1986)
    [61] B. Paczynski, Astrophys. J., 308:L43(1986)
    [62] T. Piran, A. Shemi, and R. Narayan, Mon. Not. R. Astron. Soc., 263:861(1993)
    [63] L. D. Landau, Е. М. Lifshitz, textit The Classical Theory of Fields} Fourth revised English edition (Oxford, MA:Butterworth-Heinemann, 1975), p.87
    [64] B. C. Thomas, C. H. Jackman, A. L. Melott et al, Astrophys. J. Lett., 622:L153(2005)
    [65] C. Thompson, M. Lyutikov, and S. R. Kulkarni, Astrophys. J., 574:332(2002)
    [66] L. Pavan, R. Turolla, S. Zane, and L. Nobili, Mon. Not. R. Astron. Soc., 395:753(2009)
    [67] S. Zane, R. Turolla, Mon. Not. R. Astron. Soc., 366:727(2006)
    [68] M. Ruderman, Astrophys. J., 382:576(1991)

  • Access

    加载中

Get Citation
Hao Wen, Fang-Yu Li, Jin Li, Zhen-Yun Fang and Andrew Beckwith. Very high-frequency gravitational waves from magnetars and gamma-ray bursts[J]. Chinese Physics C, 2017, 41(12): 125101. doi: 10.1088/1674-1137/41/12/125101
Hao Wen, Fang-Yu Li, Jin Li, Zhen-Yun Fang and Andrew Beckwith. Very high-frequency gravitational waves from magnetars and gamma-ray bursts[J]. Chinese Physics C, 2017, 41(12): 125101.  doi: 10.1088/1674-1137/41/12/125101 shu
Milestone
Received: 2017-05-15
Revised: 2017-09-18
Fund

    Supported by National Natural Science Foundation of China (11605015, 11375279, 11205254, 11647307) and the Fundamental Research Funds for the Central Universities (106112017CDJXY300003, 106112017CDJXFLX0014)

Article Metric

Article Views(1651)
PDF Downloads(14)
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:

Very high-frequency gravitational waves from magnetars and gamma-ray bursts

    Corresponding author: Hao Wen,
  • 1. Department of Physics, Chongqing University, Chongqing 401331, China
  • Received Date: 2017-05-15
  • Accepted Date: 2017-09-18
  • Available Online: 2017-12-05
Fund Project:  Supported by National Natural Science Foundation of China (11605015, 11375279, 11205254, 11647307) and the Fundamental Research Funds for the Central Universities (106112017CDJXY300003, 106112017CDJXFLX0014)

Abstract: Extremely powerful astrophysical electromagnetic (EM) systems could be possible sources of high-frequency gravitational waves (HFGWs). Here, based on properties of magnetars and gamma-ray bursts (GRBs), we address "Gamma-HFGWs" (with very high-frequency around 1020 Hz) caused by ultra-strong EM radiation (in the radiation-dominated phase of GRB fireballs) interacting with super-high magnetar surface magnetic fields (~1011 T). By certain parameters of distance and power, the Gamma-HFGWs would have far field energy density Ωgw around 10-6 and they would cause perturbed signal EM waves of ~10-20 W/m2 in a proposed HFGW detection system based on the EM response to GWs. Specially, Gamma-HFGWs would possess distinctive envelopes with characteristic shapes depending on the particular structures of surface magnetic fields of magnetars, which could be exclusive features helpful to distinguish them from background noise. Results obtained suggest that magnetars could be involved in possible astrophysical EM sources of GWs in the very high-frequency band, and Gamma-HFGWs could be potential targets for observations in the future.

    HTML

Reference (68)

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