AT 2023lli: A Tidal Disruption Event with Prominent Optical Early Bump and Delayed Episodic X-Ray Emission

被引：5

作者：

Huang, Shifeng ^{[1
,2
]}

Jiang, Ning ^{[1
,2
]}

Zhu, Jiazheng ^{[1
,2
]}

Wang, Yibo ^{[1
,2
]}

Wang, Tinggui ^{[1
,2
,3
]}

Wang, Shan-Qin ^{[4
]}

Gan, Wen-Pei ^{[5
]}

Liang, En-Wei ^{[4
]}

Qin, Yu-Jing ^{[6
]}

Lin, Zheyu ^{[1
,2
]}

Xu, Lin-Na ^{[4
]}

Cai, Min-Xuan ^{[1
,2
]}

Jiang, Ji-an ^{[1
,2
,7
]}

Kong, Xu ^{[1
,2
,3
]}

Li, Jiaxun ^{[1
,2
]}

Li, Long ^{[1
,2
]}

Wang, Jian-Guo ^{[8
,9
]}

Xu, Ze-Lin ^{[1
,2
]}

Xue, Yongquan ^{[1
,2
]}

Yuan, Ye-Fei ^{[1
,2
]}

Cheng, Jingquan ^{[10
]}

Fan, Lulu ^{[1
,2
,3
]}

Gao, Jie ^{[11
]}

Hu, Lei ^{[10
,12
]}

Hu, Weida ^{[13
]}

Li, Bin ^{[10
]}

Li, Feng ^{[11
]}

Liang, Ming ^{[14
]}

Liu, Hao ^{[11
]}

Liu, Wei ^{[10
]}

Lou, Zheng ^{[10
]}

Luo, Wentao ^{[3
]}

Qian, Yuan ^{[10
]}

Tang, Jinlong ^{[15
]}

Wan, Zhen ^{[1
,2
]}

Wang, Hairen ^{[10
]}

Wang, Jian ^{[3
,11
]}

Yang, Ji ^{[10
]}

Yao, Dazhi ^{[10
]}

Zhang, Hongfei ^{[11
]}

Zhang, Xiaoling ^{[10
]}

Zhao, Wen ^{[1
,2
]}

Zheng, Xianzhong ^{[10
]}

Zhu, Qingfeng ^{[1
,2
,3
]}

Zuo, Yingxi ^{[10
]}

机构：

[1] Univ Sci & Technol China, Dept Astron, CAS Key Lab Res Galaxies & Cosmol, Hefei 230026, Peoples R China

[2] Univ Sci & Technol China, Sch Astron & Space Sci, Hefei 230026, Peoples R China

[3] Inst Deep Space Sci, Deep Space Explorat Lab, Hefei 230026, Peoples R China

[4] Guangxi Univ, Sch Phys Sci & Technol, Guangxi Key Lab Relativist Astrophys, Nanning 530004, Peoples R China

[5] Nanjing Hopes Technol Co Ltd, Nanjing 210000, Peoples R China

[6] CALTECH, Div Phys Math & Astron, 1200 E Calif Blvd, Pasadena, CA 91125 USA

[7] Natl Inst Nat Sci, Natl Astron Observ Japan, Tokyo 1818588, Japan

[8] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China

[9] Key Lab Struct & Evolut Celestial Objects, Yunnan Observ, Kunming 650216, Peoples R China

[10] Chinese Acad Sci, Purple Mt Observ, Nanjing 210023, Peoples R China

[11] Univ Sci & Technol China, State Key Lab Particle Detect & Elect, Hefei 230026, Peoples R China

[12] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA

[13] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[14] NSFs Natl Opt Infrared Astron Res Lab, Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85726 USA

[15] Inst Opt & Elect, Chinese Acad Sci, Chengdu 610209, Peoples R China

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2024年 / 964卷 / 02期

基金：

中国博士后科学基金; 中国国家自然科学基金;

关键词：

BLACK-HOLE MASS; NUCLEAR TRANSIENT; HYDRODYNAMICAL SIMULATIONS; EARLY EVOLUTION; INFRARED ECHO; STELLAR MASS; STARS; DISCOVERY; TELESCOPE; CANDIDATE;

D O I：

10.3847/2041-8213/ad319f

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

High-cadence, multiwavelength observations have continuously revealed the diversity of tidal disruption events (TDEs), thus greatly advancing our knowledge and understanding of TDEs. In this work, we conducted an intensive optical-UV and X-ray follow-up campaign of TDE AT 2023lli and found a remarkable month-long bump in its UV/optical light curve nearly 2 months prior to maximum brightness. The bump represents the longest separation time from the main peak among known TDEs to date. The main UV/optical outburst declines as t -4.10, making it one of the fastest-decaying optically selected TDEs. Furthermore, we detected sporadic X-ray emission 30 days after the UV/optical peak, accompanied by a reduction in the period of inactivity. It is proposed that the UV/optical bump could be caused by the self-intersection of the stream debris, whereas the primary peak is generated by the reprocessed emission of the accretion process. In addition, our results suggest that episodic X-ray radiation during the initial phase of decline may be due to the patched obscurer surrounding the accretion disk, a phenomenon associated with the inhomogeneous reprocessing process. The double TDE scenario, in which two stars are disrupted in sequence, is also a possible explanation for producing the observed early bump and main peak. We anticipate that the multicolor light curves of TDEs, especially in the very early stages, and the underlying physics can be better understood in the near future with the assistance of dedicated surveys such as the deep high-cadence survey of the 2.5 m Wide Field Survey Telescope.

引用

页数：11

共 23 条

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Merloni, A.
Anderson, G. E.
Miller-Jones, J. C. A.
Markowitz, A. G.
Ciroi, S.
Di Mille, F.
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[23] Discovery of a Time Lag between the Soft X-Ray and Radio Emission of the Tidal Disruption Flare ASASSN-14li: Evidence for Linear Disk-Jet Coupling
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