Two-component TeV Emissions for Blazars
Two-component TeV Emissions for Blazars
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Blazar 的双组分 TeV 发射
DOI:
10.1088/1538-3873/ac76de
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发表时间:
2022-06
影响因子:
3.5
通讯作者:
Junhui Fan
中科院分区:
文献类型:
--
作者:
Zhuang Zhang;Xiangtao Zeng;Z. Y. Pei;Xiao Hu-Bing;Xuhong Ye;Junhui Fan
Abstract For blazars, its radio emissions are composed of two components. In the high energy bands, Tera-electronvolts (TeV; 10 12 electronvolts) emissions were detected from some blazars. Does the TeV emission also consist of two components? To investigate the TeV emission component, we compiled a sample of 51 TeV blazars with available radio core dominance parameters and applied a two-component (the beamed and the unbeamed) model to study the composition of blazar TeV emission. We obtained the core-dominance parameter at the TeV band through applying a relativistic beaming model, and found that the average TeV core-dominance parameter is log R TeV BL = 〈 3.12 ± 2.83 〉 for 46 BL Lacs, and that is log R TeV FSRQ = 〈 4.80 ± 1.76 〉 for 5 FSRQs, which shows an indication that the core dominance parameter in BL Lacs is smaller than that in FSRQs. For the three subclasses of BL Lacs—high synchrotron peaked BL Lacs(HBLs), intermediate synchrotron peaked BL Lacs(IBLs) and low synchrotron peaked(LBLs), log R TeV HBL is smaller than log R TeV IBL and log R TeV LBL . Our results suggest that the blazar TeV emission from the core is thousands times stronger than from the extended region and the TeV emission is more core-dominated for the lower synchrotron peaked sources. In addition, a significant correlation between the TeV core-dominance parameter ( log R TeV ) and the radio one ( log R radio ) log R TeV = ( 2.56 ± 0.08 ) log R radio + 0.99 , is obtained suggesting that the TeV emission is beamed and the TeV core-dominance parameter is an indicator of beaming effect at the TeV bands, and that the TeV emission has stronger beaming effect than the radio emission.
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DOI:
10.1007/s11433-019-1454-6
发表时间:
2019-05
期刊:
Science China Physics, Mechanics & Astronomy
影响因子:
--
作者:
ZhiYuan Pei;JunHui Fan;Denis Bastieri;JiangHe Yang;HuBing Xiao
通讯作者:
HuBing Xiao
影响因子:
4.8
作者:
A. Kembhavi
通讯作者:
A. Kembhavi
DOI:
10.1088/0004-6256/147/6/143
发表时间:
2014-03
期刊:
The Astronomical Journal
影响因子:
--
作者:
T. Hovatta;M. Aller;H. Aller;E. Clausen-Brown;D. Homan;Y. Kovalev;M. Lister;A. Pushkarev;
通讯作者:
T. Hovatta;M. Aller;H. Aller;E. Clausen-Brown;D. Homan;Y. Kovalev;M. Lister;A. Pushkarev;
影响因子:
64.8
作者:
The H.E.S.S. Collaboration
通讯作者:
The H.E.S.S. Collaboration
DOI:
10.3847/1538-4357/ac3a09
发表时间:
2012-10
期刊:
PASJ
影响因子:
--
作者:
Hua, Tong Xu;Liu, Yi;Qin, Yi-Ping;Huang, Yong
通讯作者:
Huang, Yong