1
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Zhang SB, Wang JS, Yang X, Li Y, Geng JJ, Tang ZF, Chang CM, Luo JT, Wang XC, Wu XF, Dai ZG, Zhang B. A bright burst from FRB 20200120E in a globular cluster of the nearby galaxy M81. Nat Commun 2024; 15:7454. [PMID: 39198464 PMCID: PMC11358292 DOI: 10.1038/s41467-024-51711-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/23/2024] [Accepted: 08/14/2024] [Indexed: 09/01/2024] Open
Abstract
Fast radio bursts (FRBs) are immensely energetic millisecond-duration radio pulses. Observations indicate that nearby FRBs can be produced by old stellar populations, as suggested by the localization of the repeating source FRB 20200120E in a globular cluster of M81. Nevertheless, the burst energies of FRB 20200120E are significantly smaller than those of other cosmological FRBs. Here, we report the detection of a bright burst from FRB 20200120E in 1.1 - 1.7 GHz, with a fluence of approximately 30 Jy ms, which is more than 42 times larger than the previously detected bursts near 1.4 GHz frequency. It reaches one-third of the energy of the weakest burst from FRB 20121102A and is detectable at a distance exceeding 200 Mpc. Our finding bridges the gap between nearby and cosmological FRBs and indicates that FRBs hosted in globular clusters can be bright enough to be observable at cosmological distances.
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Affiliation(s)
- S B Zhang
- Purple Mountain Observatory, Chinese Academy of Sciences, 210023, Nanjing, China
| | - J S Wang
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117, Heidelberg, Germany
| | - X Yang
- Purple Mountain Observatory, Chinese Academy of Sciences, 210023, Nanjing, China
- School of Astronomy and Space Sciences, University of Science and Technology of China, 230026, Hefei, China
| | - Y Li
- Purple Mountain Observatory, Chinese Academy of Sciences, 210023, Nanjing, China
| | - J J Geng
- Purple Mountain Observatory, Chinese Academy of Sciences, 210023, Nanjing, China
| | - Z F Tang
- Purple Mountain Observatory, Chinese Academy of Sciences, 210023, Nanjing, China
- School of Astronomy and Space Sciences, University of Science and Technology of China, 230026, Hefei, China
| | - C M Chang
- Purple Mountain Observatory, Chinese Academy of Sciences, 210023, Nanjing, China
- School of Astronomy and Space Sciences, University of Science and Technology of China, 230026, Hefei, China
| | - J T Luo
- National Time Service Center, Chinese Academy of Sciences, 710600, Xi'an, China
- University of Chinese Academy of Sciences, No.19A Yuquan Road, Shijingshan District, 100049, Beijing, China
| | - X C Wang
- National Time Service Center, Chinese Academy of Sciences, 710600, Xi'an, China
| | - X F Wu
- Purple Mountain Observatory, Chinese Academy of Sciences, 210023, Nanjing, China.
- School of Astronomy and Space Sciences, University of Science and Technology of China, 230026, Hefei, China.
| | - Z G Dai
- Department of Astronomy, University of Science and Technology of China, 230026, Hefei, China.
| | - B 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.
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2
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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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3
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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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4
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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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5
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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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6
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Feng Y, Zhang YK, Li D, Yang YP, Wang P, Niu CH, Dai S, Yao JM. Circular polarization in two active repeating fast radio bursts. Sci Bull (Beijing) 2022; 67:2398-2401. [PMID: 36566060 DOI: 10.1016/j.scib.2022.11.014] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/18/2022] [Revised: 10/26/2022] [Accepted: 11/15/2022] [Indexed: 11/17/2022]
Affiliation(s)
- Yi Feng
- Research Center for Intelligent Computing Platforms, Zhejiang Laboratory, Hangzhou 311100, China
| | - Yong-Kun Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; Research Center for Intelligent Computing Platforms, Zhejiang Laboratory, Hangzhou 311100, China; University of Chinese Academy of Sciences, Beijing 100049, China
| | - Di Li
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China; Research Center for Intelligent Computing Platforms, Zhejiang Laboratory, Hangzhou 311100, China; University of Chinese Academy of Sciences, Beijing 100049, China; NAOC-UKZN Computational Astrophysics Centre, University of KwaZulu-Natal, Durban 4000, South Africa.
| | - Yuan-Pei Yang
- South-Western Institute for Astronomy Research, Yunnan University, Kunming 650500, China; Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, 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
| | - Chen-Hui Niu
- Institute of Astrophysics, Central China Normal University, Wuhan 430079, China; National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Shi Dai
- School of Science, Western Sydney University, Locked Bag 1797, Penrith NSW 2751, Australia
| | - Ju-Mei Yao
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China
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7
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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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8
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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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9
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The Statistical Similarity of Repeating and Non-Repeating Fast Radio Bursts. UNIVERSE 2022. [DOI: 10.3390/universe8070355] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
In this paper, we present a sample of 21 repeating fast radio bursts (FRBs) detected by different radio instruments before September 2021. Using the Anderson–Darling test, we compared the distributions of extra-Galactic dispersion measure (DME) of non-repeating FRBs, repeating FRBs and all FRBs. It was found that the DME values of three sub-samples are log-normally distributed. The DME of repeaters and non-repeaters were drawn from a different distribution on basis of the Mann–Whitney–Wilcoxon test. In addition, assuming that the non-repeating FRBs identified currently may be potentially repeators, i.e., the repeating FRBs to be universal and representative, one can utilize the averaged fluence of repeating FRBs as an indication from which to derive an apparent intensity distribution function (IDF) with a power-law index of a1=1.10±0.14 (a2=1.01±0.16, the observed fluence as a statistical variant), which is in good agreement with the previous IDF of 16 non-repeating FRBs found by Li et al. Based on the above statistics of repeating and non-repeating FRBs, we propose that both types of FRBs may have different cosmological origins, spatial distributions and circum-burst environments. Interestingly, the differential luminosity distributions of repeating and non-repeating FRBs can also be well described by a broken power-law function with the same power-law index of −1.4.
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10
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Niu CH, Aggarwal K, Li D, Zhang X, Chatterjee S, Tsai CW, Yu W, Law CJ, Burke-Spolaor S, Cordes JM, Zhang YK, Ocker SK, Yao JM, Wang P, Feng Y, Niino Y, Bochenek C, Cruces M, Connor L, Jiang JA, Dai S, Luo R, Li GD, Miao CC, Niu JR, Anna-Thomas R, Sydnor J, Stern D, Wang WY, Yuan M, Yue YL, Zhou DJ, Yan Z, Zhu WW, Zhang B. A repeating fast radio burst associated with a persistent radio source. Nature 2022; 606:873-877. [PMID: 35676486 PMCID: PMC9242862 DOI: 10.1038/s41586-022-04755-5] [Citation(s) in RCA: 10] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/23/2021] [Accepted: 04/11/2022] [Indexed: 12/15/2022]
Abstract
The dispersive sweep of fast radio bursts (FRBs) has been used to probe the ionized baryon content of the intergalactic medium1, which is assumed to dominate the total extragalactic dispersion. Although the host-galaxy contributions to the dispersion measure appear to be small for most FRBs2, in at least one case there is evidence for an extreme magneto-ionic local environment3,4 and a compact persistent radio source5. Here we report the detection and localization of the repeating FRB 20190520B, which is co-located with a compact, persistent radio source and associated with a dwarf host galaxy of high specific-star-formation rate at a redshift of 0.241 ± 0.001. The estimated host-galaxy dispersion measure of approximately [Formula: see text] parsecs per cubic centimetre, which is nearly an order of magnitude higher than the average of FRB host galaxies2,6, far exceeds the dispersion-measure contribution of the intergalactic medium. Caution is thus warranted in inferring redshifts for FRBs without accurate host-galaxy identifications.
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Affiliation(s)
- C-H Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - K Aggarwal
- Department of Physics and Astronomy, West Virginia University, Morgantown, WV, USA
- Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV, USA
| | - D Li
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China.
- University of Chinese Academy of Sciences, Beijing, China.
- Research Center for Intelligent Computing Platforms, Zhejiang Laboratory, Hangzhou, China.
| | - X Zhang
- University of Chinese Academy of Sciences, Beijing, China
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
| | - S Chatterjee
- Cornell Center for Astrophysics and Planetary Science, and Department of Astronomy, Cornell University, Ithaca, NY, USA
| | - C-W Tsai
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - W Yu
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China.
| | - C J Law
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA.
- Owens Valley Radio Observatory, California Institute of Technology, Big Pine, CA, USA.
| | - S Burke-Spolaor
- Department of Physics and Astronomy, West Virginia University, Morgantown, WV, USA
- Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV, USA
- Canadian Institute for Advanced Research, Toronto, Ontario, Canada
| | - J M Cordes
- Cornell Center for Astrophysics and Planetary Science, and Department of Astronomy, Cornell University, Ithaca, NY, USA
| | - Y-K Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- University of Chinese Academy of Sciences, Beijing, China
| | - S K Ocker
- Cornell Center for Astrophysics and Planetary Science, and Department of Astronomy, Cornell University, Ithaca, NY, USA
| | - J-M Yao
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - P Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Y Feng
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- University of Chinese Academy of Sciences, Beijing, China
- Research Center for Intelligent Computing Platforms, Zhejiang Laboratory, Hangzhou, China
| | - Y Niino
- Institute of Astronomy, Graduate School of Science, The University of Tokyo, Tokyo, Japan
- Research Center for the Early Universe, The University of Tokyo, Tokyo, Japan
| | - C Bochenek
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - M Cruces
- Max-Planck-Institut für Radioastronomie, Bonn, Germany
| | - L Connor
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - J-A Jiang
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Japan
| | - S Dai
- CSIRO Space and Astronomy, Epping, New South Wales, Australia
- School of Science, Western Sydney University, Penrith South DC, New South Wales, Australia
| | - R Luo
- CSIRO Space and Astronomy, Epping, New South Wales, Australia
| | - G-D Li
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- University of Chinese Academy of Sciences, Beijing, China
| | - C-C Miao
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- University of Chinese Academy of Sciences, Beijing, China
| | - J-R Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- University of Chinese Academy of Sciences, Beijing, China
| | - R Anna-Thomas
- Department of Physics and Astronomy, West Virginia University, Morgantown, WV, USA
- Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV, USA
| | - J Sydnor
- Department of Physics and Astronomy, West Virginia University, Morgantown, WV, USA
- Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV, USA
| | - D Stern
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - W-Y Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- Department of Astronomy, School of Physics, Peking University, Beijing, China
| | - M Yuan
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- University of Chinese Academy of Sciences, Beijing, China
| | - Y-L Yue
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - D-J Zhou
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- University of Chinese Academy of Sciences, Beijing, China
| | - Z Yan
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China
| | - W-W Zhu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - B Zhang
- Department of Physics and Astronomy, University of Nevada, Las Vegas, Las Vegas, NV, USA
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11
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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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12
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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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13
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Feng Y, Li D, Yang YP, Zhang Y, Zhu W, Zhang B, Lu W, Wang P, Dai S, Lynch RS, Yao J, Jiang J, Niu J, Zhou D, Xu H, Miao C, Niu C, Meng L, Qian L, Tsai CW, Wang B, Xue M, Yue Y, Yuan M, Zhang S, Zhang L. Frequency-dependent polarization of repeating fast radio bursts-implications for their origin. Science 2022; 375:1266-1270. [PMID: 35298266 DOI: 10.1126/science.abl7759] [Citation(s) in RCA: 11] [Impact Index Per Article: 5.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The polarization of fast radio bursts (FRBs), which are bright astronomical transient phenomena, contains information about their environments. Using wide-band observations with two telescopes, we report polarization measurements of five repeating FRBs and find a trend of lower polarization at lower frequencies. This behavior is modeled as multipath scattering, characterized by a single parameter, σRM, the rotation measure (RM) scatter. Sources with higher σRM have higher RM magnitude and scattering time scales. The two sources with the highest σRM, FRB 20121102A and FRB 20190520B, are associated with compact persistent radio sources. These properties indicate a complex environment near the repeating FRBs, such as a supernova remnant or a pulsar wind nebula, consistent with their having arisen from young stellar populations.
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Affiliation(s)
- Yi Feng
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,Zhejiang Lab, Hangzhou, Zhejiang 311121, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Di Li
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,Zhejiang Lab, Hangzhou, Zhejiang 311121, China.,National Astronomical Observatories, Chinese Academy of Sciences-University of KwaZulu-Natal Computational Astrophysics Centre, University of KwaZulu-Natal, Durban 4000, South Africa
| | - Yuan-Pei Yang
- South-Western Institute for Astronomy Research, Yunnan University, Kunming, Yunnan 650504, China
| | - Yongkun Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Weiwei Zhu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Bing Zhang
- Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA.,Nevada Center for Astrophysics, University of Nevada, Las Vegas, NV 89154, USA
| | - Wenbin Lu
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
| | - Pei Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Shi Dai
- School of Science, Western Sydney University, Penrith, NSW 2751, Australia
| | - Ryan S Lynch
- Green Bank Observatory, Green Bank, WV 24401, USA
| | - Jumei Yao
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, Xinjiang 830011, China
| | - Jinchen Jiang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,School of Physics, Peking University, Beijing 100871, China
| | - Jiarui Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Dejiang Zhou
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Heng Xu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,School of Physics, Peking University, Beijing 100871, China
| | - Chenchen Miao
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Chenhui Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Lingqi Meng
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Lei Qian
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Chao-Wei Tsai
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Bojun Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,School of Physics, Peking University, Beijing 100871, China
| | - Mengyao Xue
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Youling Yue
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
| | - Mao Yuan
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China.,School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Songbo Zhang
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Lei Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China
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14
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Xu R. The impact of FAST on the research of fast radio bursts. Natl Sci Rev 2022; 8:nwab204. [PMID: 34987846 PMCID: PMC8692928 DOI: 10.1093/nsr/nwab204] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Download PDF] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/31/2021] [Revised: 11/11/2021] [Accepted: 11/12/2021] [Indexed: 11/13/2022] Open
Affiliation(s)
- Renxin Xu
- School of Physics and Kavli Institute for Astronomy and Astrophysics, Peking University, China
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15
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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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16
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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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