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Optical Flux and Spectral Variability of BL Lacertae during Its Historical High Outburst in 2020

文献类型：期刊论文

作者Kalita,Nibedita1,7; Yuan,Yuhai4,6; Gu,Minfeng1; Fan,Junhui4,6; Mizuno,Yosuke2,5; Jiang,Peng7; Gupta,Alok C.1,3; Zhou,Hongyan7; Pan,Xiang7; Strigachev,Anton A.9
刊名The Astrophysical Journal
出版日期2023-02-01
卷号943期号:2页码:135
关键词active galactic nucleus intraday variability particle-acceleration webt campaigns broad-band flare microvariability dynamics fermi jets
ISSN号0004-637X
DOI10.3847/1538-4357/aca801
产权排序9
英文摘要Abstract BL Lacertae underwent a series of historical high flux activity over a year from 2020 August in the optical to VHE γ-rays. In this paper, we report on optical flux and spectral variability of the first historical maxima outburst event during October–November in the g, r, and i bands with the 1.26 m telescope at the Xinglong Observatory, China. We detected significant intranight variations with amplitude rising up to ～30%, where the fastest variability timescale was found to be a few tens of minutes, giving an emitting region size of the order 10?3 pc, which corresponds to ～100 Schwarzschild radius of the central black hole, likely coming from some jet mini-structures. Unlike on the intranight timescale, a clear frequency-dependent pattern along symmetric timescales (～11 days) of flux variation is detected on a long timescale. The spectral evolution was predominated by flattening of the spectra with increasing brightness i.e., a bluer-when-brighter trend in 96% of the cases. On the night before the outburst peak, the color indices shown in a color–magnitude diagram, clustered into two distinct branches, within a period of ～6 hr, which is connected to a hard-soft-hard spectral evolution trend extracted from time-resolved spectra. To the best of our knowledge, such a trend has never been seen in BL Lac or any other blazars before. The results obtained in this study can be explained in the context of shock-induced particle acceleration or magnetic reconnection in the jet where turbulent processes most likely resulted in the asymmetric flux variation on a nightly timescale.
语种英语
WOS记录号WOS:000924564300001
出版者The American Astronomical Society
源URL[http://ir.xao.ac.cn/handle/45760611-7/6215]  
专题研究单元未命名
通讯作者Kalita,Nibedita
作者单位1.Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People’s Republic of China; nibeditaklt1@gmail.com
2.School of Physics and Astronomy, Shanghai Jiao Tong University, 800 Dongchuan Road, Shanghai, 200240, People’s Republic of China
3.Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital, 263001, India
4.Astronomy Science and Technology Research Laboratory, Department of Education of Guangdong Province, Guangzhou 510006, People’s Republic of China
5.Tsung-Dao Lee Institute, Shanghai Jiao Tong University, 520 Shengrong Road, Shanghai, 201210, People’s Republic of China
6.Center for Astrophysics, Guangzhou University, Guangzhou 510006, People’s Republic of China
7.Key Laboratory for Polar Science, MNR, Polar Research Institute of China, 451 Jinqiao Road, Shanghai 200135, People’s Republic of China
8.Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science 1-Street, 830011 Urumqi, People’s Republic of China
9.Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, 72 Tsarigradsko shosse Boulevard, 1784 Sofia, Bulgaria
推荐引用方式
GB/T 7714		 Kalita,Nibedita,Yuan,Yuhai,Gu,Minfeng,et al. Optical Flux and Spectral Variability of BL Lacertae during Its Historical High Outburst in 2020[J]. The Astrophysical Journal,2023,943(2):135.
APA Kalita,Nibedita.,Yuan,Yuhai.,Gu,Minfeng.,Fan,Junhui.,Mizuno,Yosuke.,...&Cui,Lang.(2023).Optical Flux and Spectral Variability of BL Lacertae during Its Historical High Outburst in 2020.The Astrophysical Journal,943(2),135.
MLA Kalita,Nibedita,et al."Optical Flux and Spectral Variability of BL Lacertae during Its Historical High Outburst in 2020".The Astrophysical Journal 943.2(2023):135.

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