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Optical and ultraviolet monitoring of the black hole X-ray binary MAXI J1820+070/ASASSN-18ey for 18 months
Sai, Hanna1; Wang, Xiaofeng1,2; Wu, Jianfeng3; Lin, Jie1; Feng, Hua4,5; Zhang, Tianmeng6,7; Li, Wenxiong1; Zhang JJ(张居甲)8,9,10; Mo, Jun1; Sun, Tianrui11,12,13; Ehgamberdiev, Shuhrat A.14; Mirzaqulov, Davron14; Rui, Liming1; Lin, Weili1; Zhao, Xulin15; Lin, Han1; Zhang, Jicheng1; Zhang, Xinghan1; Zhao, Yong6,16; Li, Xue1; Xiang, Danfeng1; Wang, Lingzhi17,18; Wu, Chengyuan1
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2021-07
Volume504Issue:3Pages:4226-4241
DOI10.1093/mnras/stab1162
Contribution Rank第8完成单位
Indexed BySCI
Keywordaccretion, accretion discs stars: black holes X-rays: binaries
Abstract

MAXI J1820+070 is a low-mass black hole X-ray binary system with high luminosity in both optical and X-ray bands during its outburst periods. We present extensive photometry in the X-ray, ultraviolet, and optical bands, as well as densely cadenced optical spectra, covering the phase from the beginning of the optical outburst to similar to 550 days. During the rebrightening process, the optical emission precedes the X-ray by 20.80 +/- 2.85 days. The spectra are characterized by blue continua and emission features of Balmer series, He I, and He II lines and a broad Bowen blend. The pseudo equivalent widths (pEWs) of emission lines are found to show anticorrelations with the X-ray flux measured at comparable phases, due to increased suppression by the optical continuum. At around the X-ray peak, the full widths at half-maximum (FWHMs) of H beta and He II lambda 4686 tend to stabilize at 19.4 and 21.8 angstrom, corresponding to the line-forming regions at radii of 1.7 and 1.3 R-circle dot within the disc. We further analysed the absolute fluxes of the lines and found that the fluxes of H beta and He II lambda 4686 show positive correlations with the X-ray flux, favouring the suggestion that the irradiation model is responsible for the optical emission. However, the fact that X-ray emission experiences a dramatic flux drop at t similar to 200 days after the outburst, while the optical flux only shows a little variation, suggests that additional energy such as viscous energy may contribute to the optical radiation, in addition to X-ray irradiation.

Funding ProjectOpen Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[12033003] ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11761141001] ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11633002] ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[12003013] ; National Program on Key Research and Development Project[2016YFA0400803] ; Scholar Program of Beijing Academy of Science and Technology[BS2020002] ; President Fund of Xiamen University[20720190051] ; Chinese Academy of Sciences (CAS)Chinese Academy of Sciences ; Chinese Academy of SciencesChinese Academy of Sciences ; People's Government of Yunnan Province ; National Natural Science Foundation of ChinaNational Natural Science Foundation of China (NSFC)[U1938105]
Funding OrganizationOpen Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; National Natural Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[12033003, 11761141001, 11633002, 12003013] ; National Program on Key Research and Development Project[2016YFA0400803] ; Scholar Program of Beijing Academy of Science and Technology[BS2020002] ; President Fund of Xiamen University[20720190051] ; Chinese Academy of Sciences (CAS)Chinese Academy of Sciences ; Chinese Academy of SciencesChinese Academy of Sciences ; People's Government of Yunnan Province ; National Natural Science Foundation of ChinaNational Natural Science Foundation of China (NSFC)[U1938105]
Language英语
Subject Area天文学 ; 天体物理学 ; 高能天体物理学 ; 实测天体物理学 ; 恒星与银河系 ; 恒星物理学 ; 恒星天文学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherOXFORD UNIV PRESS
Publication PlaceGREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN0035-8711
URL查看原文
WOS IDWOS:000656139300074
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordDISC INSTABILITY MODEL ; DWARF-NOVAE ; MASS ; EMISSION ; OUTBURST ; SPECTROSCOPY ; TRANSIENTS ; SOFT
Citation statistics
Document Type期刊论文
Version出版稿
Identifierhttp://ir.ynao.ac.cn/handle/114a53/24433
Collection南方基地
中国科学院天体结构与演化重点实验室
Corresponding AuthorWang, Xiaofeng; Sun, Tianrui
Affiliation1.Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, China;
2.Beijing Planetarium, Beijing Academy of Science and Technology, Beijing 100044, China;
3.Department of Astronomy Xiamen University (Haiyun Campus), Siming District, Xiamen, Fujian 361005, China;
4.Department of Astronomy, Tsinghua University, Beijing 100084, China;
5.Department of Engineering Physics, Tsinghua University, Beijing 100084, China;
6.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China;
7.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 101408, China;
8.Yunnan Observatories (YNAO), Chinese Academy of Sciences, Kunming 650216, China;
9.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, China;
10.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China;
11.Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China;
12.Chinese Center for Antarctic Astronomy, Nanjing 210008, China;
13.School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China;
14.Ulugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Uzbekistan, Tashkent 100052, Uzbekistan;
15.School of Science, Tianjin University of Technology, Tianjin 300384, China;
16.University of Chinese Academy of Sciences, Beijing 100049, China;
17.National Astronomical Observatory of China, Chinese Academy of Sciences, Beijing, 100012, China;
18.Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS, Beijing 100101, China
Recommended Citation
GB/T 7714
Sai, Hanna,Wang, Xiaofeng,Wu, Jianfeng,et al. Optical and ultraviolet monitoring of the black hole X-ray binary MAXI J1820+070/ASASSN-18ey for 18 months[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2021,504(3):4226-4241.
APA Sai, Hanna.,Wang, Xiaofeng.,Wu, Jianfeng.,Lin, Jie.,Feng, Hua.,...&Wu, Chengyuan.(2021).Optical and ultraviolet monitoring of the black hole X-ray binary MAXI J1820+070/ASASSN-18ey for 18 months.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,504(3),4226-4241.
MLA Sai, Hanna,et al."Optical and ultraviolet monitoring of the black hole X-ray binary MAXI J1820+070/ASASSN-18ey for 18 months".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 504.3(2021):4226-4241.
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