1
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Zhang B. A surprising stochastic behavior of fast radio bursts. Sci Bull (Beijing) 2024; 69:1593-1594. [PMID: 38704354 DOI: 10.1016/j.scib.2024.04.026] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 05/06/2024]
Affiliation(s)
- Bing Zhang
- The Nevada Center for Astrophysics, University of Nevada, Las Vegas 89154, USA; Department of Physics and Astronomy, University of Nevada, Las Vegas 89154, USA.
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2
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Zhang YK, Li D, Feng Y, Wang P, Niu CH, Dai S, Yao JM, Tsai CW. The arrival time and energy of FRBs traverse the time-energy bivariate space like a Brownian motion. Sci Bull (Beijing) 2024; 69:1020-1026. [PMID: 38453537 DOI: 10.1016/j.scib.2024.02.010] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/24/2023] [Revised: 11/22/2023] [Accepted: 02/02/2024] [Indexed: 03/09/2024]
Abstract
The origin of fast radio bursts (FRBs), the brightest cosmic explosion in radio bands, remains unknown. We introduce here a novel method for a comprehensive analysis of active FRBs' behaviors in the time-energy domain. Using "Pincus Index" and "Maximum Lyapunov Exponent", we were able to quantify the randomness and chaoticity, respectively, of the bursting events and put FRBs in the context of common transient physical phenomena, such as pulsar, earthquakes, and solar flares. In the bivariate time-energy domain, repeated FRB bursts' behaviors deviate significantly (more random, less chaotic) from pulsars, earthquakes, and solar flares. The waiting times between FRB bursts and the corresponding energy changes exhibit no correlation and remain unpredictable, suggesting that the emission of FRBs does not exhibit the time and energy clustering observed in seismic events. The pronounced stochasticity may arise from a singular source with high entropy or the combination of diverse emission mechanisms/sites. Consequently, our methodology serves as a pragmatic tool for illustrating the congruities and distinctions among diverse physical processes.
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Affiliation(s)
- Yong-Kun Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; Key Laboratory of Radio Astronomy and Technolgoy, Chinese Academy of Sciences, Beijing 100101, China; University of Chinese Academy of Sciences, Beijing 100049, China
| | - Di Li
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; Key Laboratory of Radio Astronomy and Technolgoy, Chinese Academy of Sciences, Beijing 100101, China; University of Chinese Academy of Sciences, Beijing 100049, China; Research Center for Astronomical Computing, Zhejiang Laboratory, Hangzhou 311100, China; New Cornerstone Science Laboratory, Shenzhen 518054, China.
| | - Yi Feng
- Research Center for Astronomical Computing, Zhejiang Laboratory, Hangzhou 311100, China
| | - Pei Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; Key Laboratory of Radio Astronomy and Technolgoy, Chinese Academy of Sciences, Beijing 100101, China; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China
| | - Chen-Hui Niu
- Institute of Astrophysics, Central China Normal University, Wuhan 430079, China
| | - Shi Dai
- School of Science, Western Sydney University, Penrith NSW 2751, Australia
| | - Ju-Mei Yao
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Urumqi 830011, China; Xinjiang Key Laboratory of Radio Astrophysics, Urumqi 830011, China
| | - Chao-Wei Tsai
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; Key Laboratory of Radio Astronomy and Technolgoy, Chinese Academy of Sciences, Beijing 100101, China; University of Chinese Academy of Sciences, Beijing 100049, China; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China
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3
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Hu CP, Narita T, Enoto T, Younes G, Wadiasingh Z, Baring MG, Ho WCG, Guillot S, Ray PS, Güver T, Rajwade K, Arzoumanian Z, Kouveliotou C, Harding AK, Gendreau KC. Rapid spin changes around a magnetar fast radio burst. Nature 2024; 626:500-504. [PMID: 38356071 DOI: 10.1038/s41586-023-07012-5] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/19/2023] [Accepted: 12/21/2023] [Indexed: 02/16/2024]
Abstract
Magnetars are neutron stars with extremely high magnetic fields (≳1014 gauss) that exhibit various X-ray phenomena such as sporadic subsecond bursts, long-term persistent flux enhancements and variable rotation-period derivative1,2. In 2020, a fast radio burst (FRB), akin to cosmological millisecond-duration radio bursts, was detected from the Galactic magnetar SGR 1935+2154 (refs. 3-5), confirming the long-suspected association between some FRBs and magnetars. However, the mechanism for FRB generation in magnetars remains unclear. Here we report the X-ray observation of two glitches in SGR 1935+2154 within a time interval of approximately nine hours, bracketing an FRB that occurred on 14 October 20226,7. Each glitch involved a significant increase in the magnetar's spin frequency, being among the largest abrupt changes in neutron-star rotation8-10 observed so far. Between the glitches, the magnetar exhibited a rapid spin-down phase, accompanied by an increase and subsequent decline in its persistent X-ray emission and burst rate. We postulate that a strong, ephemeral, magnetospheric wind11 provides the torque that rapidly slows the star's rotation. The trigger for the first glitch couples the star's crust to its magnetosphere, enhances the various X-ray signals and spawns the wind that alters magnetospheric conditions that might produce the FRB.
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Affiliation(s)
- Chin-Ping Hu
- Department of Physics, National Changhua University of Education, Changhua City, Taiwan.
- Extreme Natural Phenomena RIKEN Hakubi Research Team, Cluster of Pioneering Research, RIKEN, Wako, Japan.
| | - Takuto Narita
- Department of Physics, Graduate School of Science, Kyoto University, Kyoto, Japan
| | - Teruaki Enoto
- Extreme Natural Phenomena RIKEN Hakubi Research Team, Cluster of Pioneering Research, RIKEN, Wako, Japan.
- Department of Physics, Graduate School of Science, Kyoto University, Kyoto, Japan.
| | - George Younes
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA.
| | - Zorawar Wadiasingh
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA.
- Department of Astronomy, University of Maryland College Park, College Park, MD, USA.
- Center for Research and Exploration in Space Science and Technology, NASA/GSFC, Greenbelt, MD, USA.
| | - Matthew G Baring
- Department of Physics and Astronomy, Rice University, Houston, TX, USA
| | - Wynn C G Ho
- Department of Physics and Astronomy, Haverford College, Haverford, PA, USA
| | - Sebastien Guillot
- Institut de Recherche en Astrophysique et Planétologie, UPS-OMP, CNRS, CNES, Toulouse, France
| | - Paul S Ray
- Space Science Division, US Naval Research Laboratory, Washington DC, USA
| | - Tolga Güver
- Science Faculty, Department of Astronomy and Space Sciences, Istanbul University, Istanbul, Turkey
- Observatory Research and Application Center, Istanbul University, Istanbul, Turkey
| | - Kaustubh Rajwade
- ASTRON, The Netherlands Institute for Radio Astronomy, Dwingeloo, The Netherlands
| | - Zaven Arzoumanian
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | | | - Alice K Harding
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, USA
| | - Keith C Gendreau
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
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4
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Iwamoto M, Matsumoto Y, Amano T, Matsukiyo S, Hoshino M. Linearly Polarized Coherent Emission from Relativistic Magnetized Ion-Electron Shocks. PHYSICAL REVIEW LETTERS 2024; 132:035201. [PMID: 38307077 DOI: 10.1103/physrevlett.132.035201] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/30/2023] [Revised: 08/30/2023] [Accepted: 11/27/2023] [Indexed: 02/04/2024]
Abstract
Fast radio bursts (FRBs) are millisecond transient astrophysical phenomena and bright at radio frequencies. The emission mechanism, however, remains unsolved yet. One scenario is a coherent emission associated with the magnetar flares and resulting relativistic shock waves. Here, we report unprecedentedly large-scale simulations of relativistic magnetized ion-electron shocks, showing that strongly linear-polarized electromagnetic waves are excited. The kinetic energy conversion to the emission is so efficient that the wave amplitude is responsible for the brightness. We also find a polarization angle swing reflecting shock front modulation, implicating the polarization property of some repeating FRBs. The results support the shock scenario as an origin of the FRBs.
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Affiliation(s)
- Masanori Iwamoto
- Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa-Oiwakecho, Sakyo-Ku, Kyoto 606-8502, Japan
- Faculty of Engineering Sciences, Kyushu University, 6-1, Kasuga-koen, Kasuga, Fukuoka 816-8580, Japan
| | - Yosuke Matsumoto
- Institute for Advanced Academic Research, Chiba University, 1-33 Yayoi, Inage-ku, Chiba, Chiba 263-8522, Japan
| | - Takanobu Amano
- Department of Earth and Planetary Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
| | - Shuichi Matsukiyo
- Faculty of Engineering Sciences, Kyushu University, 6-1, Kasuga-koen, Kasuga, Fukuoka 816-8580, Japan
| | - Masahiro Hoshino
- Department of Earth and Planetary Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
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5
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Ryder SD, Bannister KW, Bhandari S, Deller AT, Ekers RD, Glowacki M, Gordon AC, Gourdji K, James CW, Kilpatrick CD, Lu W, Marnoch L, Moss VA, Prochaska JX, Qiu H, Sadler EM, Simha S, Sammons MW, Scott DR, Tejos N, Shannon RM. A luminous fast radio burst that probes the Universe at redshift 1. Science 2023; 382:294-299. [PMID: 37856596 DOI: 10.1126/science.adf2678] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/12/2022] [Accepted: 09/04/2023] [Indexed: 10/21/2023]
Abstract
Fast radio bursts (FRBs) are millisecond-duration pulses of radio emission originating from extragalactic distances. Radio dispersion is imparted on each burst by intervening plasma, mostly located in the intergalactic medium. In this work, we observe the burst FRB 20220610A and localize it to a morphologically complex host galaxy system at redshift 1.016 ± 0.002. The burst redshift and dispersion measure are consistent with passage through a substantial column of plasma in the intergalactic medium and extend the relationship between those quantities measured at lower redshift. The burst shows evidence for passage through additional turbulent magnetized plasma, potentially associated with the host galaxy. We use the burst energy of 2 × 1042 erg to revise the empirical maximum energy of an FRB.
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Affiliation(s)
- S D Ryder
- School of Mathematical and Physical Sciences, Macquarie University, Sydney, NSW 2109, Australia
- Astrophysics and Space Technologies Research Centre, Macquarie University, Sydney, NSW 2109, Australia
| | - K W Bannister
- Australia Telescope National Facility, Commonwealth Science and Industrial Research Organisation, Space and Astronomy, Epping, NSW 1710, Australia
| | - S Bhandari
- Netherlands Institute for Radio Astronomy (ASTRON), 7991 PD Dwingeloo, Netherlands
- Joint institute for Very Long Baseline Interferometry in Europe, 7991 PD Dwingeloo, Netherlands
| | - A T Deller
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia
| | - R D Ekers
- Australia Telescope National Facility, Commonwealth Science and Industrial Research Organisation, Space and Astronomy, Epping, NSW 1710, Australia
- International Centre for Radio Astronomy Research, Curtin Institute of Radio Astronomy, Curtin University, Perth, WA 6102, Australia
| | - M Glowacki
- International Centre for Radio Astronomy Research, Curtin Institute of Radio Astronomy, Curtin University, Perth, WA 6102, Australia
| | - A C Gordon
- Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, Evanston, IL 60208, USA
| | - K Gourdji
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia
| | - C W James
- International Centre for Radio Astronomy Research, Curtin Institute of Radio Astronomy, Curtin University, Perth, WA 6102, Australia
| | - C D Kilpatrick
- Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, Evanston, IL 60208, USA
- Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA
| | - W Lu
- Department of Astronomy University of California, Berkeley, CA 94720, USA
- Theoretical Astrophysics Center, University of California, Berkeley, CA 94720, USA
| | - L Marnoch
- School of Mathematical and Physical Sciences, Macquarie University, Sydney, NSW 2109, Australia
- Astrophysics and Space Technologies Research Centre, Macquarie University, Sydney, NSW 2109, Australia
- Australia Telescope National Facility, Commonwealth Science and Industrial Research Organisation, Space and Astronomy, Epping, NSW 1710, Australia
- Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Macquarie University, Sydney, NSW 2109, Australia
| | - V A Moss
- Australia Telescope National Facility, Commonwealth Science and Industrial Research Organisation, Space and Astronomy, Epping, NSW 1710, Australia
| | - J X Prochaska
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
- Kavli Institute for the Physics and Mathematics of the Universe, Kashiwa, 277-8583, Japan
| | - H Qiu
- Square Kilometre Array Observatory, Jodrell Bank, Lower Withington, Macclesfield SK11 9FT, UK
| | - E M Sadler
- Australia Telescope National Facility, Commonwealth Science and Industrial Research Organisation, Space and Astronomy, Epping, NSW 1710, Australia
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | - S Simha
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - M W Sammons
- International Centre for Radio Astronomy Research, Curtin Institute of Radio Astronomy, Curtin University, Perth, WA 6102, Australia
| | - D R Scott
- International Centre for Radio Astronomy Research, Curtin Institute of Radio Astronomy, Curtin University, Perth, WA 6102, Australia
| | - N Tejos
- Instituto de Física, Pontificia Universidad Católica de Valparaíso, Casilla 4059, Valparaíso, Chile
| | - R M Shannon
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia
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6
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Xie Y, Geng JJ, Zhu XW, Zhao ZH, Lei Z, Yuan WQ, Zhao G, Wu XF, Qiao B. Origin of FRB-associated X-ray burst: QED magnetic reconnection. Sci Bull (Beijing) 2023; 68:1857-1861. [PMID: 37355391 DOI: 10.1016/j.scib.2023.06.005] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/30/2023] [Revised: 04/19/2023] [Accepted: 06/05/2023] [Indexed: 06/26/2023]
Affiliation(s)
- Yu Xie
- State Key Laboratory of Nuclear Physics and Technology, Center for Applied Physics and Technology, and HEDPS, School of Physics, Peking University, Beijing 100094, China; Research Center of Laser Fusion, China Academy of Engineering Physics, Mianyang 621900, China
| | - Jin-Jun Geng
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Xi-Wei Zhu
- State Key Laboratory of Nuclear Physics and Technology, Center for Applied Physics and Technology, and HEDPS, School of Physics, Peking University, Beijing 100094, China
| | - Zhong-Hai Zhao
- State Key Laboratory of Nuclear Physics and Technology, Center for Applied Physics and Technology, and HEDPS, School of Physics, Peking University, Beijing 100094, China
| | - Zhu Lei
- State Key Laboratory of Nuclear Physics and Technology, Center for Applied Physics and Technology, and HEDPS, School of Physics, Peking University, Beijing 100094, China
| | - Wen-Qiang Yuan
- State Key Laboratory of Nuclear Physics and Technology, Center for Applied Physics and Technology, and HEDPS, School of Physics, Peking University, Beijing 100094, China
| | - Gang Zhao
- Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100094, China
| | - Xue-Feng Wu
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China; School of Astronomy and Space Sciences, University of Science and Technology of China, Hefei 230026, China.
| | - Bin Qiao
- State Key Laboratory of Nuclear Physics and Technology, Center for Applied Physics and Technology, and HEDPS, School of Physics, Peking University, Beijing 100094, China; Frontiers Science Center for Nano-optoelectronic, Peking University, Beijing 100094, China.
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7
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Zhu W, Xu H, Zhou D, Lin L, Wang B, Wang P, Zhang C, Niu J, Chen Y, Li C, Meng L, Lee K, Zhang B, Feng Y, Ge M, Göğüş E, Guan X, Han J, Jiang J, Jiang P, Kouveliotou C, Li D, Miao C, Miao X, Men Y, Niu C, Wang W, Wang Z, Xu J, Xu R, Xue M, Yang Y, Yu W, Yuan M, Yue Y, Zhang S, Zhang Y. A radio pulsar phase from SGR J1935+2154 provides clues to the magnetar FRB mechanism. SCIENCE ADVANCES 2023; 9:eadf6198. [PMID: 37506211 DOI: 10.1126/sciadv.adf6198] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/02/2022] [Accepted: 06/27/2023] [Indexed: 07/30/2023]
Abstract
The megajansky radio burst, FRB 20200428, and other bright radio bursts detected from the Galactic source SGR J1935+2154 suggest that magnetars can make fast radio bursts (FRBs), but the emission site and mechanism of FRB-like bursts are still unidentified. Here, we report the emergence of a radio pulsar phase of the magnetar 5 months after FRB 20200428. Pulses were detected in 16.5 hours over 13 days using the Five-hundred-meter Aperture Spherical radio Telescope, with luminosities of about eight decades fainter than FRB 20200428. The pulses were emitted in a narrow phase window anti-aligned with the x-ray pulsation profile observed using the x-ray telescopes. The bursts, conversely, appear in random phases. This dichotomy suggests that radio pulses originate from a fixed region within the magnetosphere, but bursts occur in random locations and are possibly associated with explosive events in a dynamically evolving magnetosphere. This picture reconciles the lack of periodicity in cosmological repeating FRBs within the magnetar engine model.
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Affiliation(s)
- Weiwei Zhu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China
| | - Heng Xu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Department of Astronomy, Peking University, Beijing 100871, China
- Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China
| | - Dejiang Zhou
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
| | - Lin Lin
- Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China
- Department of Astronomy, Beijing Normal University, Beijing 100875, China
| | - Bojun Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Department of Astronomy, Peking University, Beijing 100871, China
| | - Pei Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China
| | - Chunfeng Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Department of Astronomy, Peking University, Beijing 100871, China
| | - Jiarui Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
| | - Yutong Chen
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
| | - Chengkui Li
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Lingqi Meng
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
| | - Kejia Lee
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Department of Astronomy, Peking University, Beijing 100871, China
- Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China
| | - Bing Zhang
- Nevada Center for Astrophysics, University of Nevada, Las Vegas, NV 89154, USA
- Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA
| | - Yi Feng
- Zhejiang Lab, Hangzhou, Zhejiang 311121, China
| | - Mingyu Ge
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Ersin Göğüş
- Faculty of Engineering and Natural Sciences, Sabancı University, 34956 İstanbul, Turkey
| | - Xing Guan
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Jinlin Han
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Jinchen Jiang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Department of Astronomy, Peking University, Beijing 100871, China
| | - Peng Jiang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Department of Physics, The George Washington University, 725 21st St. NW, Washington, DC 20052, USA
| | - Chryssa Kouveliotou
- Max-Planck Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany
| | - Di Li
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Faculty of Engineering and Natural Sciences, Sabancı University, 34956 İstanbul, Turkey
| | - Chenchen Miao
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
| | - Xueli Miao
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Yunpeng Men
- GuangXi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, GuangXi University, Naning 530004, China
| | - Chenghui Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Weiyang Wang
- Department of Astronomy, Peking University, Beijing 100871, China
- University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
| | - Zhengli Wang
- GuangXi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, GuangXi University, Naning 530004, China
| | - Jiangwei Xu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Department of Astronomy, Peking University, Beijing 100871, China
| | - Renxin Xu
- Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China
| | - Mengyao Xue
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Yuanpei Yang
- South-Western Institute for Astronomy Research, Yunnan University, Kunming 650500, Yunnan, China
| | - Wenfei Yu
- Shanghai Astronomical Observatory, Chinese Academy of Science, Shanghai 200030, China
| | - Mao Yuan
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
| | - Youling Yue
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Shuangnan Zhang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Yongkun Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
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8
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Kaspi VM. Slow-beating radio waves from a long-lived source. Nature 2023; 619:472-473. [PMID: 37468593 DOI: 10.1038/d41586-023-02295-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 07/21/2023]
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9
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Anna-Thomas R, Connor L, Dai S, Feng Y, Burke-Spolaor S, Beniamini P, Yang YP, Zhang YK, Aggarwal K, Law CJ, Li D, Niu C, Chatterjee S, Cruces M, Duan R, Filipovic MD, Hobbs G, Lynch RS, Miao C, Niu J, Ocker SK, Tsai CW, Wang P, Xue M, Yao JM, Yu W, Zhang B, Zhang L, Zhu S, Zhu W. Magnetic field reversal in the turbulent environment around a repeating fast radio burst. Science 2023; 380:599-603. [PMID: 37167388 DOI: 10.1126/science.abo6526] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 05/13/2023]
Abstract
Fast radio bursts (FRBs) are brief, intense flashes of radio waves from unidentified extragalactic sources. Polarized FRBs originate in highly magnetized environments. We report observations of the repeating FRB 20190520B spanning 17 months, which show that the FRB's Faraday rotation is highly variable and twice changes sign. The FRB also depolarizes below radio frequencies of about 1 to 3 gigahertz. We interpret these properties as being due to changes in the parallel component of the magnetic field integrated along the line of sight, including reversing direction of the field. This could result from propagation through a turbulent magnetized screen of plasma, located 10-5 to [Formula: see text] parsecs from the FRB source. This is consistent with the bursts passing through the stellar wind of a binary companion of the FRB source.
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Affiliation(s)
- Reshma Anna-Thomas
- Department of Physics and Astronomy, West Virginia University, Morgantown, WV 26506, USA
- Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV 26506, USA
| | - Liam Connor
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA
- Owens Valley Radio Observatory, California Institute of Technology, Big Pine, CA 93513, USA
| | - Shi Dai
- School of Science, Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Australia Telescope National Facility, Commonwealth Scientific and Industrial Research Organisation-Space and Astronomy, Epping, NSW 1710, Australia
| | - Yi Feng
- Zhejiang Lab, Hangzhou, Zhejiang 311121, China
| | - Sarah Burke-Spolaor
- Department of Physics and Astronomy, West Virginia University, Morgantown, WV 26506, USA
- Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV 26506, USA
| | - Paz Beniamini
- Department of Natural Sciences, Open University of Israel, Ra'anana 43107, Israel
- Astrophysics Research Center of the Open University, The Open University of Israel, Ra'anana 43537, Israel
| | - Yuan-Pei Yang
- South-Western Institute for Astronomy Research, Yunnan University, Kunming 650500, Yunnan, China
| | - Yong-Kun Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Kshitij Aggarwal
- Department of Physics and Astronomy, West Virginia University, Morgantown, WV 26506, USA
- Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV 26506, USA
| | - Casey J Law
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA
- Owens Valley Radio Observatory, California Institute of Technology, Big Pine, CA 93513, USA
| | - Di Li
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Zhejiang Lab, Hangzhou, Zhejiang 311121, China
- University of Chinese Academy of Sciences, Beijing 100049, China
- National Astronomical Observatories, Chinese Academy of Sciences-University of KwaZulu-Natal Computational Astrophysics Centre, University of KwaZulu-Natal, Durban 4000, South Africa
| | - Chenhui Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Shami Chatterjee
- Department of Astronomy, Cornell University, Ithaca, NY 14853, USA
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY 14853, USA
| | - Marilyn Cruces
- Max-Planck Institute for Radio Astronomy, D-53121 Bonn, Germany
| | - Ran Duan
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Miroslav D Filipovic
- School of Science, Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia
| | - George Hobbs
- Australia Telescope National Facility, Commonwealth Scientific and Industrial Research Organisation-Space and Astronomy, Epping, NSW 1710, Australia
| | - Ryan S Lynch
- Green Bank Observatory, Green Bank, WV 24401, USA
| | - Chenchen Miao
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Jiarui Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Stella K Ocker
- Department of Astronomy, Cornell University, Ithaca, NY 14853, USA
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY 14853, USA
| | - Chao-Wei Tsai
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- University of Chinese Academy of Sciences, Beijing 100049, China
- Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China
| | - Pei Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Mengyao Xue
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Ju-Mei Yao
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, Xinjiang 830011, China
| | - Wenfei Yu
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
| | - Bing Zhang
- Nevada Center for Astrophysics, Las Vegas, NV 89154, USA
- Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA
| | - Lei Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | | | - Weiwei Zhu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
- Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing 102206, China
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10
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Bailes M. The discovery and scientific potential of fast radio bursts. Science 2022; 378:eabj3043. [DOI: 10.1126/science.abj3043] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
Abstract
Fast radio bursts (FRBs) are millisecond-time-scale bursts of coherent radio emission that are luminous enough to be detectable at cosmological distances. In this Review, I describe the discovery of FRBs, subsequent advances in understanding them, and future prospects. Thousands of potentially observable FRBs reach Earth every day, which likely originate from highly magnetic and/or rapidly rotating neutron stars in the distant Universe. Some FRBs repeat, with this subclass often occurring in highly magnetic environments. Two repeating FRBs exhibit cyclic activity windows, consistent with an orbital period. One nearby FRB was emitted by a Galactic magnetar during an x-ray outburst. The host galaxies of some FRBs have been located, providing information about the host environments and the total baryonic content of the Universe.
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Affiliation(s)
- Matthew Bailes
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia
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11
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Wang FY, Zhang GQ, Dai ZG, Cheng KS. Repeating fast radio burst 20201124A originates from a magnetar/Be star binary. Nat Commun 2022; 13:4382. [PMID: 36130932 PMCID: PMC9492772 DOI: 10.1038/s41467-022-31923-y] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/15/2022] [Accepted: 07/05/2022] [Indexed: 11/21/2022] Open
Abstract
Fast radio bursts (FRBs) are cosmic sources emitting millisecond-duration radio bursts. Although several hundreds FRBs have been discovered, their physical nature and central engine remain unclear. The variations of Faraday rotation measure and dispersion measure, due to local environment, are crucial clues to understanding their physical nature. The recent observations on the rotation measure of FRB 20201124A show a significant variation on a day time scale. Intriguingly, the oscillation of rotation measure supports that the local contribution can change sign, which indicates the magnetic field reversal along the line of sight. Here we present a physical model that explains observed characteristics of FRB 20201124A and proposes that repeating signal comes from a binary system containing a magnetar and a Be star with a decretion disk. When the magnetar approaches the periastron, the propagation of radio waves through the disk of the Be star naturally leads to the observed varying rotation measure, depolarization, large scattering timescale, and Faraday conversion. This study will prompt to search for FRB signals from Be/X-ray binaries. Fast radio bursts (FRBs) are bright millisecond or shorter duration transient events. Here, the authors propose that FRB 20201124A comes from a binary system of a magnetar and a Be star with a decretion disk.
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Affiliation(s)
- F Y Wang
- School of Astronomy and Space Science, Nanjing University, Nanjing, 210093, China. .,Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, China.
| | - G Q Zhang
- School of Astronomy and Space Science, Nanjing University, Nanjing, 210093, China
| | - Z G Dai
- School of Astronomy and Space Science, Nanjing University, Nanjing, 210093, China.,Department of Astronomy, University of Science and Technology of China, Hefei, 230026, China
| | - K S Cheng
- Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong, China
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12
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A fast radio burst source at a complex magnetized site in a barred galaxy. Nature 2022; 609:685-688. [PMID: 36131036 DOI: 10.1038/s41586-022-05071-8] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/07/2021] [Accepted: 07/05/2022] [Indexed: 11/08/2022]
Abstract
Fast radio bursts (FRBs) are highly dispersed, millisecond-duration radio bursts1-3. Recent observations of a Galactic FRB4-8 suggest that at least some FRBs originate from magnetars, but the origin of cosmological FRBs is still not settled. Here we report the detection of 1,863 bursts in 82 h over 54 days from the repeating source FRB 20201124A (ref. 9). These observations show irregular short-time variation of the Faraday rotation measure (RM), which scrutinizes the density-weighted line-of-sight magnetic field strength, of individual bursts during the first 36 days, followed by a constant RM. We detected circular polarization in more than half of the burst sample, including one burst reaching a high fractional circular polarization of 75%. Oscillations in fractional linear and circular polarizations, as well as polarization angle as a function of wavelength, were detected. All of these features provide evidence for a complicated, dynamically evolving, magnetized immediate environment within about an astronomical unit (AU; Earth-Sun distance) of the source. Our optical observations of its Milky-Way-sized, metal-rich host galaxy10-12 show a barred spiral, with the FRB source residing in a low-stellar-density interarm region at an intermediate galactocentric distance. This environment is inconsistent with a young magnetar engine formed during an extreme explosion of a massive star that resulted in a long gamma-ray burst or superluminous supernova.
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13
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Leung C, Kader Z, Masui KW, Dobbs M, Michilli D, Mena-Parra J, Mckinven R, Ng C, Bandura K, Bhardwaj M, Brar C, Cassanelli T, Chawla P, Dong FA, Good D, Kaspi V, Lanman AE, Lin HH, Meyers BW, Pearlman AB, Pen UL, Petroff E, Pleunis Z, Rafiei-Ravandi M, Rahman M, Sanghavi P, Scholz P, Shin K, Siegel S, Smith KM, Stairs I, Tendulkar SP, Vanderlinde K. Constraining primordial black holes using fast radio burst gravitational-lens interferometry with CHIME/FRB. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043017] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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14
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Abstract
Fast radio bursts (FRBs) are millisecond-duration flashes of radio waves that are visible at distances of billions of light years1. The nature of their progenitors and their emission mechanism remain open astrophysical questions2. Here we report the detection of the multicomponent FRB 20191221A and the identification of a periodic separation of 216.8(1) ms between its components, with a significance of 6.5σ. The long (roughly 3 s) duration and nine or more components forming the pulse profile make this source an outlier in the FRB population. Such short periodicity provides strong evidence for a neutron-star origin of the event. Moreover, our detection favours emission arising from the neutron-star magnetosphere3,4, as opposed to emission regions located further away from the star, as predicted by some models5.
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15
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Wang F. 重复快速射电暴的偏振频率演化规律. CHINESE SCIENCE BULLETIN-CHINESE 2022. [DOI: 10.1360/tb-2022-0352] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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16
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Xu J, Li D. 快速射电暴脉冲研究进入高统计性时代. CHINESE SCIENCE BULLETIN-CHINESE 2022. [DOI: 10.1360/tb-2022-0346] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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17
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Abstract
This review considers synchronous and follow-up MASTER Global Robotic Net optical observations of high energy astrophysical phenomena such as fast radio bursts (FRB), gamma-ray bursts (including prompt optical emission polarization discovery), gravitational-wave events, detected by LIGO/VIRGO (including GW170817 and independent Kilonova discovery), high energy neutrino sources (including the detection of IC-170922A progenitor) and others. We report on the first large optical monitoring campaign of the closest at that moment radio burster FRB 180916.J0158+65 simultaneously with a radio burst. We obtained synchronous limits on the optical flux of the FRB 180916.J0158+65 and FRB 200428 (soft gamma repeater SGR 1935+2154)(The CHIME/FRB Collaboration, Nature 2020, 587) at 155093 MASTER images with the total exposure time equal to 2,705,058 s, i.e., 31.3 days. It follows from these synchronous limitations that the ratio of the energies released in the optical and radio ranges does not exceed 4 × 105. Our optical monitoring covered a total of 6 weeks. On 28 April 2020, MASTER automatically following up on a Swift alert began to observe the galactic soft gamma repeater SGR 1935+2154 experienced another flare. On the same day, radio telescopes detected a short radio burst FRB 200428 and MASTER-Tavrida telescope determined the best prompt optical limit of FRB/SGR 1935+2154. Our optical limit shows that X-ray and radio emissions are not explained by a single power-law spectrum. In the course of our observations, using special methods, we found a faint extended afterglow in the FRB 180916.J0158+65 direction associated with the extended emission of the host galaxy.
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18
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Li D. A commentary of "Consistency radio bursts in the Milky Way": 10 remarkable discoveries from 2020 in Nature. FUNDAMENTAL RESEARCH 2022; 2:347-348. [PMID: 38933149 PMCID: PMC11197586 DOI: 10.1016/j.fmre.2022.01.008] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/25/2022] [Accepted: 01/25/2022] [Indexed: 10/19/2022] Open
Abstract
The first detection and deep follow-up of a Galactic fast radio burst (FRB) phenomenon were reported in three papers published in the journal Nature in November 2020. Interestingly, this FRB is accompanied by a X-ray burst. The observations from multiple space and ground-based telescopes were combined to accomplish this discovery and ascertain its association with a source in the Milky Way. As the name implies, a FRB is a transient bright pulse of radio waves with a burst duration measured in milliseconds. This phenomenon was first discovered in 2007. It is extremely difficult to detect and even more so to determine their position in the sky due to their brief existence. This is the first detection of a FRB with radiation other than radio waves, as well as the first of its kind in the Milky Way. For the first time, these observations have confirmed that the source(s) of FRBs can be a magnetar(s), which so far is the only verified celestial body capable of producing FRBs. It is worth noting that one of the papers was written by a Chinese research team, the co-first authors of which are Lin Lin from Beijing Normal University, Chunfeng Zhang from Peking University, and Pei Wang from the National Astronomical Observatories of China. The observations came from China's "Sky Eye"-the Five-hundred-meter Aperture Spherical radio Telescope (FAST).
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Affiliation(s)
- Di Li
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China
- NAOC-UKZN Computational Astrophysics Centre, University of KwaZulu-Natal, Durban, 4000, South Africa
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19
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20
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Abstract
Fast radio bursts (FRBs) represent one of the most exciting astrophysical discoveries of the recent past. The study of their low-frequency emission, which was only effectively picked up about ten years after their discovery, has helped shape the field thanks to some of the most important detections to date. Observations between 400 and 800 MHz, carried out by the CHIME/FRB telescope, in particular, have led to the detection of ∼500 FRBs in little more than 1 year and, among them, ∼20 repeating sources. Detections at low frequencies have uncovered a nearby population that we can study in detail via continuous monitoring and targeted campaigns. The latest, most important discoveries include: periodicity, both at the days level in repeaters and at the millisecond level in apparently non-repeating sources; the detection of an FRB-like burst from a galactic magnetar; and the localisation of an FRB inside a globular cluster in a nearby galaxy. The systematic study of the population at low frequencies is important for the characterisation of the environment surrounding the FRBs and, at a global level, to understand the environment of the local universe. This review is intended to give an overview of the efforts leading to the current rich variety of low-frequency studies and to put into a common context the results achieved in order to trace a possible roadmap for future progress in the field.
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21
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Abstract
Fast radio bursts (FRBs) have a story which has been told and retold many times over the past few years as they have sparked excitement and controversy since their pioneering discovery in 2007. The FRB class encompasses a number of microsecond- to millisecond-duration pulses occurring at Galactic to cosmological distances with energies spanning about 8 orders of magnitude. While most FRBs have been observed as singular events, a small fraction of them have been observed to repeat over various timescales leading to an apparent dichotomy in the population. ∼50 unique progenitor theories have been proposed, but no consensus has emerged for their origin(s). However, with the discovery of an FRB-like pulse from the Galactic magnetar SGR J1935+2154, magnetar engine models are the current leading theory. Overall, FRB pulses exhibit unique characteristics allowing us to probe line-of-sight magnetic field strengths, inhomogeneities in the intergalactic/interstellar media, and plasma turbulence through an assortment of extragalactic and cosmological propagation effects. Consequently, they are formidable tools to study the Universe. This review follows the progress of the field between 2007 and 2020 and presents the science highlights of the radio observations.
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22
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Qu K, Meuren S, Fisch NJ. Signature of Collective Plasma Effects in Beam-Driven QED Cascades. PHYSICAL REVIEW LETTERS 2021; 127:095001. [PMID: 34506208 DOI: 10.1103/physrevlett.127.095001] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/21/2020] [Revised: 07/21/2021] [Accepted: 08/02/2021] [Indexed: 06/13/2023]
Abstract
QED cascades play an important role in extreme astrophysical environments like magnetars. They can also be produced by passing a relativistic electron beam through an intense laser field. Signatures of collective pair plasma effects in these QED cascades are shown to appear, in exquisite detail, through plasma-induced frequency upshifts in the laser spectrum. Remarkably, these signatures can be detected even in small plasma volumes moving at relativistic speeds. Strong-field quantum and collective pair plasma effects can thus be explored with existing technology, provided that ultradense electron beams are colocated with multipetawatt lasers.
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Affiliation(s)
- Kenan Qu
- Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544, USA
| | - Sebastian Meuren
- Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544, USA
- Stanford PULSE Institute, SLAC National Accelerator Laboratory, Menlo Park, California 94025, USA
| | - Nathaniel J Fisch
- Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544, USA
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23
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Abstract
A neutron star was first detected as a pulsar in 1967. It is one of the most mysterious compact objects in the universe, with a radius of the order of 10 km and masses that can reach two solar masses. In fact, neutron stars are star remnants, a kind of stellar zombie (they die, but do not disappear). In the last decades, astronomical observations yielded various contraints for neutron star masses, and finally, in 2017, a gravitational wave was detected (GW170817). Its source was identified as the merger of two neutron stars coming from NGC 4993, a galaxy 140 million light years away from us. The very same event was detected in γ-ray, X-ray, UV, IR, radio frequency and even in the optical region of the electromagnetic spectrum, starting the new era of multi-messenger astronomy. To understand and describe neutron stars, an appropriate equation of state that satisfies bulk nuclear matter properties is necessary. GW170817 detection contributed with extra constraints to determine it. On the other hand, magnetars are the same sort of compact object, but bearing much stronger magnetic fields that can reach up to 1015 G on the surface as compared with the usual 1012 G present in ordinary pulsars. While the description of ordinary pulsars is not completely established, describing magnetars poses extra challenges. In this paper, I give an overview on the history of neutron stars and on the development of nuclear models and show how the description of the tiny world of the nuclear physics can help the understanding of the cosmos, especially of the neutron stars.
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24
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Sironi L, Plotnikov I, Nättilä J, Beloborodov AM. Coherent Electromagnetic Emission from Relativistic Magnetized Shocks. PHYSICAL REVIEW LETTERS 2021; 127:035101. [PMID: 34328748 DOI: 10.1103/physrevlett.127.035101] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/28/2021] [Revised: 06/05/2021] [Accepted: 06/11/2021] [Indexed: 06/13/2023]
Abstract
Relativistic magnetized shocks are a natural source of coherent emission, offering a plausible radiative mechanism for fast radio bursts (FRBs). We present first-principles 3D simulations that provide essential information for the FRB models based on shocks: the emission efficiency, spectrum, and polarization. The simulated shock propagates in an e^{±} plasma with magnetization σ>1. The measured fraction of shock energy converted to coherent radiation is ≃10^{-3}σ^{-1}, and the energy-carrying wave number of the wave spectrum is ≃4ω_{c}/c, where ω_{c} is the upstream gyrofrequency. The ratio of the O-mode and X-mode energy fluxes emitted by the shock is ≃0.4σ^{-1}. The dominance of the X mode at σ≫1 is particularly strong, approaching 100% in the spectral band around 2ω_{c}. We also provide a detailed description of the emission mechanism for both X and O modes.
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Affiliation(s)
- Lorenzo Sironi
- Department of Astronomy and Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA
| | - Illya Plotnikov
- IRAP, Université de Toulouse III-Paul Sabatier, OMP, Toulouse 31400, France
| | - Joonas Nättilä
- Physics Department and Columbia Astrophysics Laboratory, Columbia University, 538 West 120th Street, New York, New York 10027, USA and Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, New York 10010, USA
| | - Andrei M Beloborodov
- Physics Department and Columbia Astrophysics Laboratory, Columbia University, 538 West 120th Street, New York, New York 10027, USA and Max Planck Institute for Astrophysics, Karl-Schwarzschild-Straße 1, D-85741 Garching, Germany
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25
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Wilson LB, Brosius AL, Gopalswamy N, Nieves‐Chinchilla T, Szabo A, Hurley K, Phan T, Kasper JC, Lugaz N, Richardson IG, Chen CHK, Verscharen D, Wicks RT, TenBarge JM. A Quarter Century of Wind Spacecraft Discoveries. REVIEWS OF GEOPHYSICS (WASHINGTON, D.C. : 1985) 2021; 59:e2020RG000714. [PMCID: PMC9285980 DOI: 10.1029/2020rg000714] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/14/2020] [Revised: 01/29/2021] [Accepted: 03/05/2021] [Indexed: 06/13/2023]
Abstract
The Wind spacecraft, launched on November 1, 1994, is a critical element in NASA’s Heliophysics System Observatory (HSO)—a fleet of spacecraft created to understand the dynamics of the Sun‐Earth system. The combination of its longevity (>25 years in service), its diverse complement of instrumentation, and high resolution and accurate measurements has led to it becoming the “standard candle” of solar wind measurements. Wind has over 55 selectable public data products with over ∼1,100 total data variables (including OMNI data products) on SPDF/CDAWeb alone. These data have led to paradigm shifting results in studies of statistical solar wind trends, magnetic reconnection, large‐scale solar wind structures, kinetic physics, electromagnetic turbulence, the Van Allen radiation belts, coronal mass ejection topology, interplanetary and interstellar dust, the lunar wake, solar radio bursts, solar energetic particles, and extreme astrophysical phenomena such as gamma‐ray bursts. This review introduces the mission and instrument suites then discusses examples of the contributions by Wind to these scientific topics that emphasize its importance to both the fields of heliophysics and astrophysics. Wind has made seminal advances to the fields of astrophysics, turbulence, kinetic physics, magnetic reconnection, and the radiation belts Wind pioneered the study of the source and evolution of solar radio emissions below 15 MHz Wind revolutionized our understanding of coronal mass ejections, their internal magnetic structure, and evolution
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Affiliation(s)
- Lynn B. Wilson
- NASA Goddard Space Flight CenterHeliophysics Science DivisionGreenbeltMDUSA
| | - Alexandra L. Brosius
- NASA Goddard Space Flight CenterHeliophysics Science DivisionGreenbeltMDUSA
- Department of Meteorology and Atmospheric ScienceThe Pennsylvania State UniversityUniversity ParkPAUSA
| | | | | | - Adam Szabo
- NASA Goddard Space Flight CenterHeliophysics Science DivisionGreenbeltMDUSA
| | - Kevin Hurley
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | - Tai Phan
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | - Justin C. Kasper
- School of Climate and Space Sciences and EngineeringUniversity of MichiganAnn ArborAnn ArborMIUSA
| | - Noé Lugaz
- Space Science CenterInstitute for the Study of EarthOceans, and SpaceUniversity of New HampshireDurhamNHUSA
- Department of PhysicsUniversity of New HampshireDurhamNHUSA
| | - Ian G. Richardson
- NASA Goddard Space Flight CenterHeliophysics Science DivisionGreenbeltMDUSA
- Department of AstronomyUniversity of MarylandCollege ParkMDUSA
| | | | - Daniel Verscharen
- Space Science CenterInstitute for the Study of EarthOceans, and SpaceUniversity of New HampshireDurhamNHUSA
- Mullard Space Science LaboratoryUniversity College LondonSurreyUK
| | - Robert T. Wicks
- Department of MathematicsPhysics and Electrical EngineeringNorthumbria University: Newcastle upon TyneTyne and WearUK
| | - Jason M. TenBarge
- University of MarylandCollege ParkMDUSA
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
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26
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Enoto T, Terasawa T, Kisaka S, Hu CP, Guillot S, Lewandowska N, Malacaria C, Ray PS, Ho WCG, Harding AK, Okajima T, Arzoumanian Z, Gendreau KC, Wadiasingh Z, Markwardt CB, Soong Y, Kenyon S, Bogdanov S, Majid WA, Güver T, Jaisawal GK, Foster R, Murata Y, Takeuchi H, Takefuji K, Sekido M, Yonekura Y, Misawa H, Tsuchiya F, Aoki T, Tokumaru M, Honma M, Kameya O, Oyama T, Asano K, Shibata S, Tanaka SJ. Enhanced x-ray emission coinciding with giant radio pulses from the Crab Pulsar. Science 2021; 372:187-190. [PMID: 33833123 DOI: 10.1126/science.abd4659] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/23/2020] [Accepted: 03/05/2021] [Indexed: 11/02/2022]
Abstract
Giant radio pulses (GRPs) are sporadic bursts emitted by some pulsars that last a few microseconds and are hundreds to thousands of times brighter than regular pulses from these sources. The only GRP-associated emission outside of radio wavelengths is from the Crab Pulsar, where optical emission is enhanced by a few percentage points during GRPs. We observed the Crab Pulsar simultaneously at x-ray and radio wavelengths, finding enhancement of the x-ray emission by 3.8 ± 0.7% (a 5.4σ detection) coinciding with GRPs. This implies that the total emitted energy from GRPs is tens to hundreds of times higher than previously known. We discuss the implications for the pulsar emission mechanism and extragalactic fast radio bursts.
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Affiliation(s)
- Teruaki Enoto
- Cluster for Pioneering Research, RIKEN, Wako 351-0198, Japan.
| | - Toshio Terasawa
- Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan. .,Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Mitaka 181-8588, Japan.,Interdisciplinary Theoretical Science Research Group, RIKEN, Wako 351-0198, Japan
| | - Shota Kisaka
- Frontier Research Institute for Interdisciplinary Sciences, Tohoku University, Sendai 980-8578, Japan. .,Astronomical Institute, Tohoku University, Sendai 980-8578, Japan.,Department of Physical Science, Hiroshima University, Higashi-Hiroshima 739-8526, Japan
| | - Chin-Ping Hu
- Cluster for Pioneering Research, RIKEN, Wako 351-0198, Japan. .,Department of Physics, National Changhua University of Education, Changhua 50007, Taiwan.,Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan
| | | | - Natalia Lewandowska
- Department of Physics and Astronomy, Haverford College, Haverford, PA 19041, USA
| | - Christian Malacaria
- NASA Marshall Space Flight Center, National Space Science and Technology Center, Huntsville, AL 35805, USA.,Universities Space Research Association, Science and Technology Institute, Huntsville, AL 35805, USA
| | - Paul S Ray
- US Naval Research Laboratory, Washington, DC 20375, USA
| | - Wynn C G Ho
- Department of Physics and Astronomy, Haverford College, Haverford, PA 19041, USA.,Mathematical Sciences and STAG Research Centre, University of Southampton, Southampton SO17 1BJ, UK
| | - Alice K Harding
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.,Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
| | | | | | | | - Zorawar Wadiasingh
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.,Universities Space Research Association, Columbia, MD 21046, USA
| | | | - Yang Soong
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Steve Kenyon
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Slavko Bogdanov
- Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA
| | - Walid A Majid
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.,California Institute of Technology, Pasadena, CA 91125, USA
| | - Tolga Güver
- Istanbul University, Science Faculty, Department of Astronomy and Space Sciences, Beyazıt, 34119 Istanbul, Turkey
| | - Gaurava K Jaisawal
- National Space Institute, Technical University of Denmark, Elektrovej 327-328, Denmark
| | - Rick Foster
- Massachusetts Institute of Technology Kavli Institute for Astrophysics and Space Research, Cambridge, MA 02139, USA
| | - Yasuhiro Murata
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan.,Usuda Deep Space Center, Japan Aerospace Exploration Agency, Saku 384-0306, Japan.,Department of Space and Astronautical Science, SOKENDAI (The Graduate University for Advanced Studies), Sagamihara 252-5210, Japan
| | - Hiroshi Takeuchi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, Japan.,Department of Space and Astronautical Science, SOKENDAI (The Graduate University for Advanced Studies), Sagamihara 252-5210, Japan
| | - Kazuhiro Takefuji
- Usuda Deep Space Center, Japan Aerospace Exploration Agency, Saku 384-0306, Japan.,Kashima Space Technology Center, National Institute of Information and Communications Technology, Kashima 314-8501, Japan
| | - Mamoru Sekido
- Kashima Space Technology Center, National Institute of Information and Communications Technology, Kashima 314-8501, Japan
| | | | - Hiroaki Misawa
- Planetary Plasma and Atmospheric Research Center, Tohoku University, Sendai 980-8578, Japan
| | - Fuminori Tsuchiya
- Planetary Plasma and Atmospheric Research Center, Tohoku University, Sendai 980-8578, Japan
| | - Takahiko Aoki
- The Research Institute for Time Studies, Yamaguchi University, Yamaguchi 753-8511, Japan
| | - Munetoshi Tokumaru
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya 464-8601, Japan
| | - Mareki Honma
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu 023-0861, Japan.,Department of Astronomy, University of Tokyo, Tokyo 113-0033, Japan.,Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), Mitaka 181-8588, Japan
| | - Osamu Kameya
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu 023-0861, Japan.,Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), Mitaka 181-8588, Japan
| | - Tomoaki Oyama
- Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Oshu 023-0861, Japan
| | - Katsuaki Asano
- Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan
| | - Shinpei Shibata
- Department of Physics, Yamagata University, Yamagata 990-8560, Japan
| | - Shuta J Tanaka
- Department of Physics and Mathematics, Aoyama Gakuin University, Sagamihara 252-5258, Japan
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27
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Abstract
Fast Radio Bursts (FRBs) represent a novel tool for probing the properties of the universe at cosmological distances. The dispersion measures of FRBs, combined with the redshifts of their host galaxies, has very recently yielded a direct measurement of the baryon content of the universe, and has the potential to directly constrain the location of the “missing baryons”. The first results are consistent with the expectations of ΛCDM for the cosmic density of baryons, and have provided the first constraints on the properties of the very diffuse intergalactic medium (IGM) and circumgalactic medium (CGM) around galaxies. FRBs are the only known extragalactic sources that are compact enough to exhibit diffractive scintillation in addition to showing exponential tails which are typical of scattering in turbulent media. This will allow us to probe the turbulent properties of the circumburst medium, the host galaxy ISM/halo, and intervening halos along the path, as well as the IGM. Measurement of the Hubble constant and the dark energy parameter w can be made with FRBs, but require very large samples of localised FRBs (>103) to be effective on their own—they are best combined with other independent surveys to improve the constraints. Ionisation events, such as for He ii, leave a signature in the dispersion measure—redshift relation, and if FRBs exist prior to these times, they can be used to probe the reionisation era, although more than 103 localised FRBs are required.
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28
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Abstract
The origin and phenomenology of the Fast Radio Burst (FRB) remains unknown despite more than a decade of efforts. Though several models have been proposed to explain the observed data, none is able to explain alone the variety of events so far recorded. The leading models consider magnetars as potential FRB sources. The recent detection of FRBs from the galactic magnetar SGR J1935+2154 seems to support them. Still, emission duration and energetic budget challenge all these models. Like for other classes of objects initially detected in a single band, it appeared clear that any solution to the FRB enigma could only come from a coordinated observational and theoretical effort in an as wide as possible energy band. In particular, the detection and localisation of optical/NIR or/and high-energy counterparts seemed an unavoidable starting point that could shed light on the FRB physics. Multiwavelength (MWL) search campaigns were conducted for several FRBs, in particular for repeaters. Here we summarize the observational and theoretical results and the perspectives in view of the several new sources accurately localised that will likely be identified by various radio facilities worldwide. We conclude that more dedicated MWL campaigns sensitive to the millisecond–minute timescale transients are needed to address the various aspects involved in the identification of FRB counterparts. Dedicated instrumentation could be one of the key points in this respect. In the optical/NIR band, fast photometry looks to be the only viable strategy. Additionally, small/medium size radiotelescopes co-pointing higher energies telescopes look a very interesting and cheap complementary observational strategy.
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29
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Abstract
Fast radio bursts (FRBs) are recently discovered mysterious single pulses of radio emission, mostly coming from cosmological distances (∼1 Gpc). Their short duration, ∼1 ms, and large luminosity demonstrate coherent emission. I review the basic physics of coherent emission mechanisms proposed for FRBs. In particular, I discuss the curvature emission of bunches, the synchrotron maser, and the emission of radio waves by variable currents during magnetic reconnection. Special attention is paid to magnetar flares as the most promising sources of FRBs. Non-linear effects are outlined that could place bounds on the power of the outgoing radiation.
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30
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Lin L, Zhang CF, Wang P, Gao H, Guan X, Han JL, Jiang JC, Jiang P, Lee KJ, Li D, Men YP, Miao CC, Niu CH, Niu JR, Sun C, Wang BJ, Wang ZL, Xu H, Xu JL, Xu JW, Yang YH, Yang YP, Yu W, Zhang B, Zhang BB, Zhou DJ, Zhu WW, Castro-Tirado AJ, Dai ZG, Ge MY, Hu YD, Li CK, Li Y, Li Z, Liang EW, Jia SM, Querel R, Shao L, Wang FY, Wang XG, Wu XF, Xiong SL, Xu RX, Yang YS, Zhang GQ, Zhang SN, Zheng TC, Zou JH. No pulsed radio emission during a bursting phase of a Galactic magnetar. Nature 2020; 587:63-65. [PMID: 33149293 DOI: 10.1038/s41586-020-2839-y] [Citation(s) in RCA: 66] [Impact Index Per Article: 16.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/08/2020] [Accepted: 08/31/2020] [Indexed: 11/10/2022]
Abstract
Fast radio bursts (FRBs) are millisecond-duration radio transients of unknown physical origin observed at extragalactic distances1-3. It has long been speculated that magnetars are the engine powering repeating bursts from FRB sources4-13, but no convincing evidence has been collected so far14. Recently, the Galactic magnetar SRG 1935+2154 entered an active phase by emitting intense soft γ-ray bursts15. One FRB-like event with two peaks (FRB 200428) and a luminosity slightly lower than the faintest extragalactic FRBs was detected from the source, in association with a soft γ-ray/hard-X-ray flare18-21. Here we report an eight-hour targeted radio observational campaign comprising four sessions and assisted by multi-wavelength (optical and hard-X-ray) data. During the third session, 29 soft-γ-ray repeater (SGR) bursts were detected in γ-ray energies. Throughout the observing period, we detected no single dispersed pulsed emission coincident with the arrivals of SGR bursts, but unfortunately we were not observing when the FRB was detected. The non-detection places a fluence upper limit that is eight orders of magnitude lower than the fluence of FRB 200428. Our results suggest that FRB-SGR burst associations are rare. FRBs may be highly relativistic and geometrically beamed, or FRB-like events associated with SGR bursts may have narrow spectra and characteristic frequencies outside the observed band. It is also possible that the physical conditions required to achieve coherent radiation in SGR bursts are difficult to satisfy, and that only under extreme conditions could an FRB be associated with an SGR burst.
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Affiliation(s)
- L Lin
- Department of Astronomy, Beijing Normal University, Beijing, People's Republic of China
| | - C F Zhang
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - P Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - H Gao
- Department of Astronomy, Beijing Normal University, Beijing, People's Republic of China
| | - X Guan
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - J L Han
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China.,University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - J C Jiang
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - P Jiang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - K J Lee
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China. .,Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, People's Republic of China.
| | - D Li
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China. .,University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, People's Republic of China.
| | - Y P Men
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - C C Miao
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - C H Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - J R Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - C Sun
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - B J Wang
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - Z L Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - H Xu
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - J L Xu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - J W Xu
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - Y H Yang
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China
| | - Y P Yang
- South-Western Institute for Astronomy Research, Yunnan University, Kunming, People's Republic of China
| | - W Yu
- Shanghai Astronomical Observatory, Chinese Academy of Science, Shanghai, People's Republic of China
| | - B Zhang
- Department of Physics and Astronomy, University of Nevada, Las Vegas, NV, USA.
| | - B-B Zhang
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China.,Department of Physics and Astronomy, University of Nevada, Las Vegas, NV, USA.,Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, People's Republic of China
| | - D J Zhou
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China.,University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - W W Zhu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - A J Castro-Tirado
- Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain.,Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingenierías, Universidad de Málaga, Málaga, Spain
| | - Z G Dai
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China.,Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, People's Republic of China
| | - M Y Ge
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - Y D Hu
- Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain.,Facultad de Ciencias, Universidad de Granada, Granada, Spain
| | - C K Li
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - Y Li
- University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, People's Republic of China.,Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, People's Republic of China
| | - Z Li
- Department of Astronomy, Beijing Normal University, Beijing, People's Republic of China
| | - E W Liang
- Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University, Nanning, People's Republic of China
| | - S M Jia
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - R Querel
- National Institute of Water and Atmospheric Research (NIWA), Lauder, New Zealand
| | - L Shao
- College of Physics, Hebei Normal University, Shijiazhuang, People's Republic of China
| | - F Y Wang
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China.,Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, People's Republic of China
| | - X G Wang
- Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University, Nanning, People's Republic of China
| | - X F Wu
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, People's Republic of China
| | - S L Xiong
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - R X Xu
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, People's Republic of China
| | - Y-S Yang
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China
| | - G Q Zhang
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China
| | - S N Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China.,University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, People's Republic of China.,Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - T C Zheng
- Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University, Nanning, People's Republic of China
| | - J-H Zou
- College of Physics, Hebei Normal University, Shijiazhuang, People's Republic of China
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31
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Abstract
Fast radio bursts are mysterious millisecond-duration transients prevalent in the radio sky. Rapid accumulation of data in recent years has facilitated an understanding of the underlying physical mechanisms of these events. Knowledge gained from the neighbouring fields of gamma-ray bursts and radio pulsars has also offered insights. Here I review developments in this fast-moving field. Two generic categories of radiation model invoking either magnetospheres of compact objects (neutron stars or black holes) or relativistic shocks launched from such objects have been much debated. The recent detection of a Galactic fast radio burst in association with a soft gamma-ray repeater suggests that magnetar engines can produce at least some, and probably all, fast radio bursts. Other engines that could produce fast radio bursts are not required, but are also not impossible.
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32
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A bright millisecond-duration radio burst from a Galactic magnetar. Nature 2020; 587:54-58. [DOI: 10.1038/s41586-020-2863-y] [Citation(s) in RCA: 230] [Impact Index Per Article: 57.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/19/2020] [Accepted: 09/01/2020] [Indexed: 11/08/2022]
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33
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