摘要
Fast radio bursts(FRBs) are extremely strong radio flares lasting several milliseconds,most of which come from unidentified objects at a cosmological distance.They can be apparently repeating or not.In this paper,we analyzed 18 repeaters and 12 non-repeating FRBs observed in the frequency bands of 400–800 MHz from Canadian Hydrogen Intensity Mapping Experiment(CHIME).We investigated the distributions of FRB isotropic-equivalent radio luminosity,considering the K correction.Statistically,the luminosity distribution can be better fitted by Gaussian form than by power-law.Based on the above results,together with the observed FRB event rate,pulse duration,and radio luminosity,FRB origin models are evaluated and constrained such that the gamma-ray bursts(GRBs) may be excluded for the non-repeaters while magnetars or neutron stars(NSs) emitting the supergiant pulses are preferred for the repeaters.We also found the necessity of a small FRB emission beaming solid angle(about 0.1 sr) from magnetars that should be considered,and/or the FRB association with soft gamma-ray repeaters(SGRs) may lie at a low probability of about 10%.Finally,we discussed the uncertainty of FRB luminosity caused by the estimation of the distance that is inferred by the simple relation between the redshift and dispersion measure(DM).
作者
Xiang-Han Cui
Cheng-Min Zhang
Shuang-Qiang Wang
Jian-Wei Zhang
Di Li
Bo Peng
Wei-Wei Zhu
Richard Strom
Na Wang
Qingdong Wu
Chang-Qing Ye
De-Hua Wang
Yi-Yan Yang
Zhen-Qi Diao
崔翔翰;张承民;王双强;张见微;李菂;彭勃;朱炜玮;李查德;王娜;吴庆东;叶长青;王德华;杨佚沿;刁振琪(CAS Key Laboratory of FAST,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China;School of Astronomy and Space Science,University of Chinese Academy of Sciences,Beijing 100049,China;School of Physical Sciences,University of Chinese Academy of Sciences,Beijing 100049,China;Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China;Department of Astronomy,Beijing Normal University,Beijing 100875,China;NAOC-UKZN Computational Astrophysics Centre,University of KwaZulu-Natal,Durban 4000,South Africa;Key Laboratory of Radio Astronomy,Chinese Academy of Sciences,Beijing 100101,China;Netherlands Institute for Radio Astronomy(ASTRON),Postbus 2,7990 AA Dwingeloo,the Netherlands;Astronomical Institute ‘Anton Pannekoek’ Faculty of Science,University of Amsterdam,1090 GE Amsterdam,the Netherlands;TianQin Research Center for Gravitational Physics,Sun Yat-sen University,Zhuhai 519082,China;School of Physics and Electronic Sciences,Guizhou Education University,Guiyang 550018,China)
基金
supported by the National Natural Science Foundation of China (Grant Nos.11988101,U1938117,U1731238,11703003 and 11725313)
the International Partnership Program of Chinese Academy of Sciences (Grant No.114A11KYSB20160008)
the National Key R&D Program of China (No.2016YFA0400702)
the Guizhou Provincial Science and Technology Foundation (Grant No.[2020]1Y019)。
