At You https://orcid.org/0000-0002-8231-063X [email protected], Xinwu Cao https://orcid.org/0000-0002-2355-3498 [email protected], Zhen Yan https://orcid.org/0000-0002-5385-9586 [email protected], Jean Marie Hameury https://orcid.org/0000-0002-6412-0103, Bozena Czerny https://orcid.org/0000-0001-5848-4333, Yue Wu https://orcid.org/0000-0002-5225-637X, Tianyu Xia https://orcid.org/0000-0002-8438-8529, Marek Tit https://orcid.org/0000-0003-1667-7334, Shuang-Nan Zhang https://orcid.org/0000-0001-5586-1017, Pu Ofand Piotr T. Zycki https://orcid.org/0000-0002-7596-4221Authors Info & Affiliations
Science
31 Aug 2023
Vol 381, Issue 6661
pp. 961–964
Editor’s summary
As material falls toward a black hole, it forms an accretion disk that emits x-rays and optical light and sometimes also a jet that is visible at radio wavelengths. Theory predicts that if the disk contains a sufficiently strong magnetic field, then it can resist the gravitational pull of the black hole and temporarily halt the accretion process. You et al. compared observations of a transient black hole accretion event at x-ray, optical, and radio wavelengths. They found time delays between brightening at the different wavelengths and used models to show that this behavior is produced by a magnetically arrested disk. —Keith T. Smith
Abstract
Accretion of material onto a black hole drags any magnetic fields present inwards, increasing their strength. Theory predicts that sufficiently strong magnetic fields can halt the accretion flow, producing a magnetically arrested disk (MAD). We analyzed archival multiwavelength observations of an outburst from the black hole x-ray binary MAXI J1820+070 in 2018. The radio and optical fluxes were delayed compared with the x-ray flux by about 8 and 17 days, respectively. We interpret this as evidence for the formation of a MAD. In this scenario, the magnetic field is amplified by an expanding corona, forming a MAD around the time of the radio peak. We propose that the optical delay is due to thermal viscous instability in the outer disk.
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Volume 381 | Issue 6661
1 September 2023
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Copyright © 2023 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works.
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Received: 5 February 2022
Accepted: 30 June 2023
Published in print: 1 September 2023
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Acknowledgments
We thank W.-F. Yu, J.-F. Wu, F.-G. Xie, W.-M. Gu, and M.-Y. Sun for useful discussions. B.Y. thanks Y.-K. Zhang (Jinan University) for help in producing movie S1. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide, which we used in this research.
Funding: B.Y. is supported by the National Program on Key Research and Development Project 2021YFA0718500, the National Science Foundation of China (NSFC) grants 12273026 and U1931203, the Natural Science Foundation of Hubei Province of China 2022CFB167, the Fundamental Research Funds for the Central Universities 2042022rc0002, and the Xiaomi Foundation/Xiaomi Young Talents Program. X.C. is supported by the NSFC grants 11833007, 12073023, 12233007, and 12147103; the China Manned Space Project science research grant CMS-CSST- 2021-A06; and the fundamental research fund for Chinese central universities. Z.Y. is supported by NSFC grants U1838203 and U1938114, the Youth Innovation Promotion Association of CAS ID 2020265, and the funds for key programs of Shanghai astronomical observatory. S.-N.Z. is supported by the National Program on Key Research and Development Project grant 2016YFA0400802 and by the International Partnership Program of Chinese Academy of Sciences (grant 113111KYSB20190020). P.D. is supported by NSFC grants 12022301 and 11991051.
Author contributions: B.Y. initiated the project, performed the data analysis and model interpretation, and led the writing of the manuscript. X.C. led the interpretation of the MAD and the writing of the related text. Z.Y. contributed to the data analysis, model discussion, and the writing of the text. J.-M.H. provided the DIM code and contributed to the model discussion and to the writing of the text. B.C. contributed to the discussion of the DIM. Y.W. and T.X. contributed to the simulation of the DIM and the data analysis. M.S., S.-N.Z., P.D., and P.Z. contributed to the model discussion and the writing of the text.
Competing interests: The authors declare no competing interests.
Data and materials availability: The Insight-HXMT data used in this work are available from http://archive.hxmt.cn/ under Obs ID P0114661. The radio luminosities were taken from previous work[SourceDatafile([SourceDatafile(26)], then corrected to our adopted distance (18). The optical data were obtained from https://www.aavso.org/data-download; we used object “MAXI J1820+070,” start date “03/01/2018,” and end date “03/01/2019.” The reduced data (including LE, ME, and HE light curves and x-ray, radio, and V-band luminosities), our scripts for the ICCF analysis and figure plotting, and the numerical codes we used to compute the magnetic field strength and DIM are all available at https://github.com/Bei-You-BH/MAD and archived at Zenodo (40).
Authors
Affiliations
Department of Astronomy, School of Physics and Technology, Wuhan University, Wuhan 430072, China.
Roles: Conceptualization, Data curation, Formal analysis, Funding acquisition, Investigation, Methodology, Project administration, Resources, Software, Supervision, Validation, Visualization, Writing – original draft, and Writing – review & editing.
Institute for Astronomy, School of Physics, Zhejiang University, Hangzhou 310058, China.
Roles: Conceptualization, Data curation, Formal analysis, Funding acquisition, Investigation, Methodology, Project administration, Resources, Software, Supervision, Validation, Visualization, Writing – original draft, and Writing – review & editing.
Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China.
Roles: Conceptualization, Formal analysis, Funding acquisition, Investigation, Validation, Visualization, Writing – original draft, and Writing – review & editing.
Strasbourg Astronomical Observatory, University of Strasbourg and National Center for Scientific Research, Unite Mixte de Recherche 7550, 67000 Strasbourg, France.
Roles: Conceptualization, Formal analysis, Methodology, Software, and Writing – review & editing.
Center for Theoretical Physics, Polish Academy of Sciences, 02-668 Warsaw, Poland.
Roles: Conceptualization, Methodology, and Writing – review & editing.
Department of Astronomy, School of Physics and Technology, Wuhan University, Wuhan 430072, China.
School of Astronomy and Space Science, Nanjing University, Nanjing 210023, China.
Key laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry o f Education, Nanjing 210023, China.
Roles: Data curation, Investigation, Methodology, Software, Validation, Visualization, Writing – original draft, and Writing – review & editing.
Department of Astronomy, School of Physics and Technology, Wuhan University, Wuhan 430072, China.
Key laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei 230026, China.
School of Astronomy and Space Sciences, University of Science and Technology of China, Hefei 230026, China.
Roles: Software, Validation, and Visualization.
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716 Warsaw, Poland.
Roles: Conceptualization, Investigation, Methodology, and Writing – original draft.
Key Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China.
Roles: Investigation, Project administration, Supervision, Validation, and Writing – review & editing.
Pu Of
Key Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
Roles: Software, Writing – original draft, and Writing – review & editing.
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716 Warsaw, Poland.
Roles: Conceptualization and Writing – original draft.
Funding Information
National Program on Key Research and Development Project: 2021YFA0718500
Xiaomi Foundation / Xiaomi Young Talents Program
Youth Innovation Promotion Association of CAS: 2020265
Key programs of Shanghai astronomical observatory
Fundamental Research Funds for the Central Universities (Zhejiang University)
China Manned Space Project: CMS-CSST-2021-A06
International Partnership Program of Chinese Academy of Sciences: 113111KYSB20190020
National Program on Key Research and Development Project: 2016YFA0400802
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Observations of a black hole x-ray binary indicate formation of a magnetically arrested disk.Science381,961-964(2023).DOI:10.1126/science.abo4504
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