1
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Dong DZ, Hallinan G, Nakar E, Ho AYQ, Hughes AK, Hotokezaka K, Myers ST, De K, Mooley KP, Ravi V, Horesh A, Kasliwal MM, Kulkarni SR. A transient radio source consistent with a merger-triggered core collapse supernova. Science 2021; 373:1125-1129. [PMID: 34516837 DOI: 10.1126/science.abg6037] [Citation(s) in RCA: 13] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
[Figure: see text].
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Affiliation(s)
- D Z Dong
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - G Hallinan
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - E Nakar
- School of Physics and Astronomy, Tel Aviv University, Tel Aviv, 69978, Israel
| | - A Y Q Ho
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA.,Department of Astronomy, University of California, Berkeley, CA 94720, USA.,Miller Institute for Basic Research in Science, Berkeley, CA 94720, USA
| | - A K Hughes
- Department of Physics, University of Alberta, Edmonton, Alberta T6G 2E1, Canada
| | - K Hotokezaka
- Research Center for the Early Universe, Graduate School of Science, University of Tokyo, Bunkyo-ku Tokyo 113-033, Japan
| | - S T Myers
- National Radio Astronomy Observatory, Socorro, NM 87801, USA
| | - K De
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - K P Mooley
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA.,National Radio Astronomy Observatory, Socorro, NM 87801, USA
| | - V Ravi
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - A Horesh
- Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem, 91904, Israel
| | - M M Kasliwal
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - S R Kulkarni
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
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2
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Evans PA, Cenko SB, Kennea JA, Emery SWK, Kuin NPM, Korobkin O, Wollaeger RT, Fryer CL, Madsen KK, Harrison FA, Xu Y, Nakar E, Hotokezaka K, Lien A, Campana S, Oates SR, Troja E, Breeveld AA, Marshall FE, Barthelmy SD, Beardmore AP, Burrows DN, Cusumano G, D'Aì A, D'Avanzo P, D'Elia V, de Pasquale M, Even WP, Fontes CJ, Forster K, Garcia J, Giommi P, Grefenstette B, Gronwall C, Hartmann DH, Heida M, Hungerford AL, Kasliwal MM, Krimm HA, Levan AJ, Malesani D, Melandri A, Miyasaka H, Nousek JA, O'Brien PT, Osborne JP, Pagani C, Page KL, Palmer DM, Perri M, Pike S, Racusin JL, Rosswog S, Siegel MH, Sakamoto T, Sbarufatti B, Tagliaferri G, Tanvir NR, Tohuvavohu A. Swift and NuSTAR observations of GW170817: Detection of a blue kilonova. Science 2017; 358:1565-1570. [PMID: 29038371 DOI: 10.1126/science.aap9580] [Citation(s) in RCA: 46] [Impact Index Per Article: 6.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/14/2017] [Accepted: 10/04/2017] [Indexed: 11/02/2022]
Abstract
With the first direct detection of merging black holes in 2015, the era of gravitational wave (GW) astrophysics began. A complete picture of compact object mergers, however, requires the detection of an electromagnetic (EM) counterpart. We report ultraviolet (UV) and x-ray observations by Swift and the Nuclear Spectroscopic Telescope Array of the EM counterpart of the binary neutron star merger GW170817. The bright, rapidly fading UV emission indicates a high mass (≈0.03 solar masses) wind-driven outflow with moderate electron fraction (Ye ≈ 0.27). Combined with the x-ray limits, we favor an observer viewing angle of ≈30° away from the orbital rotation axis, which avoids both obscuration from the heaviest elements in the orbital plane and a direct view of any ultrarelativistic, highly collimated ejecta (a γ-ray burst afterglow).
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Affiliation(s)
- P A Evans
- University of Leicester, X-ray and Observational Astronomy Research Group, Leicester Institute for Space and Earth Observation, Department of Physics and Astronomy, University Road, Leicester LE1 7RH, UK.
| | - S B Cenko
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.,Joint Space-Science Institute, University of Maryland, College Park, MD 20742, USA
| | - J A Kennea
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
| | - S W K Emery
- University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking RH5 6NT, UK
| | - N P M Kuin
- University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking RH5 6NT, UK
| | - O Korobkin
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545 USA
| | - R T Wollaeger
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545 USA
| | - C L Fryer
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545 USA
| | - K K Madsen
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - F A Harrison
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - Y Xu
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - E Nakar
- The Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel
| | - K Hotokezaka
- Center for Computational Astrophysics, Simons Foundation, 162 5th Avenue, New York, NY 10010, USA
| | - A Lien
- Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.,Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA
| | - S Campana
- Istituto Nazionale di Astrofisica (INAF)-Osservatorio Astronomico di Brera, Via Bianchi 46, I-23807 Merate, Italy
| | - S R Oates
- Department of Physics, University of Warwick, Coventry CV4 7AL, UK
| | - E Troja
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.,Department of Physics and Astronomy, University of Maryland, College Park, MD 20742-4111, USA
| | - A A Breeveld
- University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking RH5 6NT, UK
| | - F E Marshall
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - S D Barthelmy
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - A P Beardmore
- University of Leicester, X-ray and Observational Astronomy Research Group, Leicester Institute for Space and Earth Observation, Department of Physics and Astronomy, University Road, Leicester LE1 7RH, UK
| | - D N Burrows
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
| | - G Cusumano
- INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Palermo, via Ugo La Malfa 153, I-90146, Palermo, Italy
| | - A D'Aì
- INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Palermo, via Ugo La Malfa 153, I-90146, Palermo, Italy
| | - P D'Avanzo
- Istituto Nazionale di Astrofisica (INAF)-Osservatorio Astronomico di Brera, Via Bianchi 46, I-23807 Merate, Italy
| | - V D'Elia
- INAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monteporzio Catone, Italy.,Space Science Data Center-Agenzia Spaziale Italiana (ASI), I-00133 Roma, Italy
| | - M de Pasquale
- Department of Astronomy and Space Sciences, University of Istanbul, Beyzt 34119, Istanbul, Turkey
| | - W P Even
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545 USA.,Department of Physical Sciences, Southern Utah University, Cedar City, UT 84720, USA
| | - C J Fontes
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545 USA
| | - K Forster
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - J Garcia
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - P Giommi
- Space Science Data Center-Agenzia Spaziale Italiana (ASI), I-00133 Roma, Italy
| | - B Grefenstette
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - C Gronwall
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA.,Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA
| | - D H Hartmann
- Kinard Lab of Physics, Department of Physics and Astronomy, Clemson University, Clemson, SC 29634-0978, USA
| | - M Heida
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - A L Hungerford
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545 USA
| | - M M Kasliwal
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - H A Krimm
- Universities Space Research Association, 7178 Columbia Gateway Drive, Columbia, MD 21046, USA.,National Science Foundation, 2415 Eisenhower Avenue, Alexandria, VA 22314, USA
| | - A J Levan
- Department of Physics, University of Warwick, Coventry CV4 7AL, UK
| | - D Malesani
- Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark
| | - A Melandri
- Istituto Nazionale di Astrofisica (INAF)-Osservatorio Astronomico di Brera, Via Bianchi 46, I-23807 Merate, Italy
| | - H Miyasaka
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - J A Nousek
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
| | - P T O'Brien
- University of Leicester, X-ray and Observational Astronomy Research Group, Leicester Institute for Space and Earth Observation, Department of Physics and Astronomy, University Road, Leicester LE1 7RH, UK
| | - J P Osborne
- University of Leicester, X-ray and Observational Astronomy Research Group, Leicester Institute for Space and Earth Observation, Department of Physics and Astronomy, University Road, Leicester LE1 7RH, UK
| | - C Pagani
- University of Leicester, X-ray and Observational Astronomy Research Group, Leicester Institute for Space and Earth Observation, Department of Physics and Astronomy, University Road, Leicester LE1 7RH, UK
| | - K L Page
- University of Leicester, X-ray and Observational Astronomy Research Group, Leicester Institute for Space and Earth Observation, Department of Physics and Astronomy, University Road, Leicester LE1 7RH, UK
| | - D M Palmer
- Los Alamos National Laboratory, B244, Los Alamos, NM 87545, USA
| | - M Perri
- INAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monteporzio Catone, Italy.,Space Science Data Center-Agenzia Spaziale Italiana (ASI), I-00133 Roma, Italy
| | - S Pike
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - J L Racusin
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - S Rosswog
- The Oskar Klein Centre, Department of Astronomy, AlbaNova, Stockholm University, SE-106 91 Stockholm, Sweden
| | - M H Siegel
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
| | - T Sakamoto
- Department of Physics and Mathematics, Aoyama Gakuin University, Sagamihara, Kanagawa, 252-5258, Japan
| | - B Sbarufatti
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
| | - G Tagliaferri
- Istituto Nazionale di Astrofisica (INAF)-Osservatorio Astronomico di Brera, Via Bianchi 46, I-23807 Merate, Italy
| | - N R Tanvir
- University of Leicester, X-ray and Observational Astronomy Research Group, Leicester Institute for Space and Earth Observation, Department of Physics and Astronomy, University Road, Leicester LE1 7RH, UK
| | - A Tohuvavohu
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
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3
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Hallinan G, Corsi A, Mooley KP, Hotokezaka K, Nakar E, Kasliwal MM, Kaplan DL, Frail DA, Myers ST, Murphy T, De K, Dobie D, Allison JR, Bannister KW, Bhalerao V, Chandra P, Clarke TE, Giacintucci S, Ho AYQ, Horesh A, Kassim NE, Kulkarni SR, Lenc E, Lockman FJ, Lynch C, Nichols D, Nissanke S, Palliyaguru N, Peters WM, Piran T, Rana J, Sadler EM, Singer LP. A radio counterpart to a neutron star merger. Science 2017; 358:1579-1583. [PMID: 29038372 DOI: 10.1126/science.aap9855] [Citation(s) in RCA: 325] [Impact Index Per Article: 46.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/17/2017] [Accepted: 10/09/2017] [Indexed: 11/02/2022]
Abstract
Gravitational waves have been detected from a binary neutron star merger event, GW170817. The detection of electromagnetic radiation from the same source has shown that the merger occurred in the outskirts of the galaxy NGC 4993, at a distance of 40 megaparsecs from Earth. We report the detection of a counterpart radio source that appears 16 days after the event, allowing us to diagnose the energetics and environment of the merger. The observed radio emission can be explained by either a collimated ultrarelativistic jet, viewed off-axis, or a cocoon of mildly relativistic ejecta. Within 100 days of the merger, the radio light curves will enable observers to distinguish between these models, and the angular velocity and geometry of the debris will be directly measurable by very long baseline interferometry.
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Affiliation(s)
- G Hallinan
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA.
| | - A Corsi
- Department of Physics and Astronomy, Texas Tech University, Lubbock, TX 79409, USA
| | - K P Mooley
- Astrophysics, Department of Physics, University of Oxford, Oxford OX1 3RH, UK
| | - K Hotokezaka
- Center for Computational Astrophysics, Flatiron Institute, 162 5th Avenue, New York, NY 10010, USA.,Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
| | - E Nakar
- Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel
| | - M M Kasliwal
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - D L Kaplan
- Department of Physics, University of Wisconsin, Milwaukee, WI 53201, USA
| | - D A Frail
- National Radio Astronomy Observatory, Socorro, NM 87801, USA
| | - S T Myers
- National Radio Astronomy Observatory, Socorro, NM 87801, USA
| | - T Murphy
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)
| | - K De
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - D Dobie
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO).,Australia Telescope National Facility, Commonwealth Scientific and Industrial Research Organisation, Astronomy and Space Science, Epping, NSW 1710, Australia
| | - J R Allison
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics in 3 Dimensions (ASTRO 3D)
| | - K W Bannister
- Australia Telescope National Facility, Commonwealth Scientific and Industrial Research Organisation, Astronomy and Space Science, Epping, NSW 1710, Australia
| | - V Bhalerao
- Department of Physics, Indian Institute of Technology Bombay, Mumbai 400076, India
| | - P Chandra
- National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune University Campus, Ganeshkhind Pune 411007, India
| | - T E Clarke
- Remote Sensing Division, Naval Research Laboratory, Washington, DC 20375, USA
| | - S Giacintucci
- Remote Sensing Division, Naval Research Laboratory, Washington, DC 20375, USA
| | - A Y Q Ho
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - A Horesh
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - N E Kassim
- Remote Sensing Division, Naval Research Laboratory, Washington, DC 20375, USA
| | - S R Kulkarni
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - E Lenc
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)
| | - F J Lockman
- Green Bank Observatory, Green Bank, WV 24944, USA
| | - C Lynch
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)
| | - D Nichols
- Institute of Mathematics, Astrophysics and Particle Physics, Radboud University, 6525 AJ Nijmegen, Netherlands
| | - S Nissanke
- Institute of Mathematics, Astrophysics and Particle Physics, Radboud University, 6525 AJ Nijmegen, Netherlands
| | - N Palliyaguru
- Department of Physics and Astronomy, Texas Tech University, Lubbock, TX 79409, USA
| | - W M Peters
- Remote Sensing Division, Naval Research Laboratory, Washington, DC 20375, USA
| | - T Piran
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - J Rana
- Inter University Centre for Astronomy and Astrophysics, Pune University Campus, Pune, Maharashtra 411007, India
| | - E M Sadler
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)
| | - L P Singer
- Astroparticle Physics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
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4
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Kasliwal MM, Nakar E, Singer LP, Kaplan DL, Cook DO, Van Sistine A, Lau RM, Fremling C, Gottlieb O, Jencson JE, Adams SM, Feindt U, Hotokezaka K, Ghosh S, Perley DA, Yu PC, Piran T, Allison JR, Anupama GC, Balasubramanian A, Bannister KW, Bally J, Barnes J, Barway S, Bellm E, Bhalerao V, Bhattacharya D, Blagorodnova N, Bloom JS, Brady PR, Cannella C, Chatterjee D, Cenko SB, Cobb BE, Copperwheat C, Corsi A, De K, Dobie D, Emery SWK, Evans PA, Fox OD, Frail DA, Frohmaier C, Goobar A, Hallinan G, Harrison F, Helou G, Hinderer T, Ho AYQ, Horesh A, Ip WH, Itoh R, Kasen D, Kim H, Kuin NPM, Kupfer T, Lynch C, Madsen K, Mazzali PA, Miller AA, Mooley K, Murphy T, Ngeow CC, Nichols D, Nissanke S, Nugent P, Ofek EO, Qi H, Quimby RM, Rosswog S, Rusu F, Sadler EM, Schmidt P, Sollerman J, Steele I, Williamson AR, Xu Y, Yan L, Yatsu Y, Zhang C, Zhao W. Illuminating gravitational waves: A concordant picture of photons from a neutron star merger. Science 2017; 358:1559-1565. [PMID: 29038373 DOI: 10.1126/science.aap9455] [Citation(s) in RCA: 441] [Impact Index Per Article: 63.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/14/2017] [Accepted: 10/05/2017] [Indexed: 11/02/2022]
Abstract
Merging neutron stars offer an excellent laboratory for simultaneously studying strong-field gravity and matter in extreme environments. We establish the physical association of an electromagnetic counterpart (EM170817) with gravitational waves (GW170817) detected from merging neutron stars. By synthesizing a panchromatic data set, we demonstrate that merging neutron stars are a long-sought production site forging heavy elements by r-process nucleosynthesis. The weak gamma rays seen in EM170817 are dissimilar to classical short gamma-ray bursts with ultrarelativistic jets. Instead, we suggest that breakout of a wide-angle, mildly relativistic cocoon engulfing the jet explains the low-luminosity gamma rays, the high-luminosity ultraviolet-optical-infrared, and the delayed radio and x-ray emission. We posit that all neutron star mergers may lead to a wide-angle cocoon breakout, sometimes accompanied by a successful jet and sometimes by a choked jet.
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Affiliation(s)
- M M Kasliwal
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA.
| | - E Nakar
- The Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel
| | - L P Singer
- Astroparticle Physics Laboratory, NASA Goddard Space Flight Center, Mail Code 661, Greenbelt, MD 20771, USA.,Joint Space-Science Institute, University of Maryland, College Park, MD 20742, USA
| | - D L Kaplan
- Department of Physics, University of Wisconsin, Milwaukee, WI 53201, USA
| | - D O Cook
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - A Van Sistine
- Department of Physics, University of Wisconsin, Milwaukee, WI 53201, USA
| | - R M Lau
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - C Fremling
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - O Gottlieb
- The Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel
| | - J E Jencson
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - S M Adams
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - U Feindt
- The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden
| | - K Hotokezaka
- Center for Computational Astrophysics, Simons Foundation, Flatiron Institute, 162 5th Avenue, New York, NY 10010, USA.,Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA
| | - S Ghosh
- Department of Physics, University of Wisconsin, Milwaukee, WI 53201, USA
| | - D A Perley
- Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Browlow Hill, Liverpool L3 5RF, UK
| | - P-C Yu
- Graduate Institute of Astronomy, National Central University, No. 300, Zhongda Road, Zhongli District, Taoyuan City 32001, Taiwan
| | - T Piran
- Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - J R Allison
- Sydney Institute for Astronomy, School of Physics A28, The University of Sydney, New South Wales 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics in 3 Dimensions, Australia
| | - G C Anupama
- Indian Institute of Astrophysics, II Block Koramangala, Bangalore 560034, India
| | - A Balasubramanian
- Indian Institute of Science Education and Research, Dr. Homi Bhabha Road, Pashan, Pune 411008, India
| | - K W Bannister
- Australia Telescope National Facility, Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation, Post Office Box 76, Epping, New South Wales 1710, Australia
| | - J Bally
- Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80305, USA
| | - J Barnes
- Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA
| | - S Barway
- South African Astronomical Observatory, Post Office Box 9, Observatory, Cape Town 7935, South Africa
| | - E Bellm
- Department of Astronomy, University of Washington, Seattle, WA 98195, USA
| | - V Bhalerao
- Department of Physics, Indian Institute of Technology Bombay, Mumbai 400076, India
| | - D Bhattacharya
- Inter-University Centre for Astronomy and Astrophysics, Post Office Bag 4, Ganeshkhind, Pune 411007, India
| | - N Blagorodnova
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - J S Bloom
- Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA.,Lawrence Berkeley National Laboratory, 1 Cyclotron Road, MS 50B-4206, Berkeley, CA 94720, USA
| | - P R Brady
- Department of Physics, University of Wisconsin, Milwaukee, WI 53201, USA
| | - C Cannella
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - D Chatterjee
- Department of Physics, University of Wisconsin, Milwaukee, WI 53201, USA
| | - S B Cenko
- Astroparticle Physics Laboratory, NASA Goddard Space Flight Center, Mail Code 661, Greenbelt, MD 20771, USA.,Joint Space-Science Institute, University of Maryland, College Park, MD 20742, USA
| | - B E Cobb
- Department of Physics, George Washington University, Washington, DC 20052, USA
| | - C Copperwheat
- Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Browlow Hill, Liverpool L3 5RF, UK
| | - A Corsi
- Department of Physics and Astronomy, Texas Tech University, Box 41051, Lubbock, TX 79409-1051, USA
| | - K De
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - D Dobie
- Sydney Institute for Astronomy, School of Physics A28, The University of Sydney, New South Wales 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics, Australia.,Australia Telescope National Facility, Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation, Post Office Box 76, Epping, New South Wales 1710, Australia
| | - S W K Emery
- University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking RH5 6NT, UK
| | - P A Evans
- X-ray and Observational Astronomy Research Group, Leicester Institute for Space and Earth Observation, Department of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK
| | - O D Fox
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - D A Frail
- National Radio Astronomy Observatory, Socorro, NM 87825, USA
| | - C Frohmaier
- Department of Physics and Astronomy, University of Southampton, Southampton, Hampshire SO17 1BJ, UK.,Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Burnaby Road, Portsmouth PO1 3FX, UK
| | - A Goobar
- The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden
| | - G Hallinan
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - F Harrison
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - G Helou
- Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA
| | - T Hinderer
- Institute of Mathematics, Astrophysics and Particle Physics, Radboud University, Heyendaalseweg 135, 6525 AJ Nijmegen, Netherlands
| | - A Y Q Ho
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - A Horesh
- Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - W-H Ip
- Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA
| | - R Itoh
- Department of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
| | - D Kasen
- Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA.,Department of Physics, University of California, Berkeley, CA 94720, USA
| | - H Kim
- Gemini Observatory, Casilla 603, La Serena, Chile
| | - N P M Kuin
- University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking RH5 6NT, UK
| | - T Kupfer
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - C Lynch
- Sydney Institute for Astronomy, School of Physics A28, The University of Sydney, New South Wales 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics, Australia
| | - K Madsen
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - P A Mazzali
- Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Browlow Hill, Liverpool L3 5RF, UK.,Max-Planck Institute for Astrophysics, Garching, Germany
| | - A A Miller
- Center for Interdisciplinary Exploration and Research in Astrophysics and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA.,The Adler Planetarium, Chicago, IL 60605, USA
| | - K Mooley
- Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
| | - T Murphy
- Sydney Institute for Astronomy, School of Physics A28, The University of Sydney, New South Wales 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics, Australia
| | - C-C Ngeow
- Graduate Institute of Astronomy, National Central University, No. 300, Zhongda Road, Zhongli District, Taoyuan City 32001, Taiwan
| | - D Nichols
- Institute of Mathematics, Astrophysics and Particle Physics, Radboud University, Heyendaalseweg 135, 6525 AJ Nijmegen, Netherlands
| | - S Nissanke
- Institute of Mathematics, Astrophysics and Particle Physics, Radboud University, Heyendaalseweg 135, 6525 AJ Nijmegen, Netherlands
| | - P Nugent
- Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA.,Lawrence Berkeley National Laboratory, 1 Cyclotron Road, MS 50B-4206, Berkeley, CA 94720, USA
| | - E O Ofek
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel
| | - H Qi
- Department of Physics, University of Wisconsin, Milwaukee, WI 53201, USA
| | - R M Quimby
- Department of Astronomy, San Diego State University, San Diego, CA 92182, USA.,Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - S Rosswog
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden
| | - F Rusu
- School of Engineering (EECS), University of California, Merced, CA 95343, USA
| | - E M Sadler
- Sydney Institute for Astronomy, School of Physics A28, The University of Sydney, New South Wales 2006, Australia.,Australian Research Council Centre of Excellence for All-sky Astrophysics, Australia
| | - P Schmidt
- Institute of Mathematics, Astrophysics and Particle Physics, Radboud University, Heyendaalseweg 135, 6525 AJ Nijmegen, Netherlands
| | - J Sollerman
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden
| | - I Steele
- Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Browlow Hill, Liverpool L3 5RF, UK
| | - A R Williamson
- Institute of Mathematics, Astrophysics and Particle Physics, Radboud University, Heyendaalseweg 135, 6525 AJ Nijmegen, Netherlands
| | - Y Xu
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA
| | - L Yan
- Division of Physics, Math and Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA.,Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA
| | - Y Yatsu
- Department of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan
| | - C Zhang
- Department of Physics, University of Wisconsin, Milwaukee, WI 53201, USA
| | - W Zhao
- School of Engineering (EECS), University of California, Merced, CA 95343, USA
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5
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Ofek EO, Sullivan M, Cenko SB, Kasliwal MM, Gal-Yam A, Kulkarni SR, Arcavi I, Bildsten L, Bloom JS, Horesh A, Howell DA, Filippenko AV, Laher R, Murray D, Nakar E, Nugent PE, Silverman JM, Shaviv NJ, Surace J, Yaron O. An outburst from a massive star 40 days before a supernova explosion. Nature 2013; 494:65-7. [PMID: 23389540 DOI: 10.1038/nature11877] [Citation(s) in RCA: 160] [Impact Index Per Article: 14.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/14/2012] [Accepted: 12/18/2012] [Indexed: 11/09/2022]
Abstract
Some observations suggest that very massive stars experience extreme mass-loss episodes shortly before they explode as supernovae, as do several models. Establishing a causal connection between these mass-loss episodes and the final explosion would provide a novel way to study pre-supernova massive-star evolution. Here we report observations of a mass-loss event detected 40 days before the explosion of the type IIn supernova SN 2010mc (also known as PTF 10tel). Our photometric and spectroscopic data suggest that this event is a result of an energetic outburst, radiating at least 6 × 10(47) erg of energy and releasing about 10(-2) solar masses of material at typical velocities of 2,000 km s(-1). The temporal proximity of the mass-loss outburst and the supernova explosion implies a causal connection between them. Moreover, we find that the outburst luminosity and velocity are consistent with the predictions of the wave-driven pulsation model, and disfavour alternative suggestions.
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Affiliation(s)
- E O Ofek
- Benoziyo Center for Astrophysics, Weizmann Institute of Science, 76100 Rehovot, Israel.
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6
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Soderberg AM, Berger E, Page KL, Schady P, Parrent J, Pooley D, Wang XY, Ofek EO, Cucchiara A, Rau A, Waxman E, Simon JD, Bock DCJ, Milne PA, Page MJ, Barentine JC, Barthelmy SD, Beardmore AP, Bietenholz MF, Brown P, Burrows A, Burrows DN, Byrngelson G, Cenko SB, Chandra P, Cummings JR, Fox DB, Gal-Yam A, Gehrels N, Immler S, Kasliwal M, Kong AKH, Krimm HA, Kulkarni SR, Maccarone TJ, Mészáros P, Nakar E, O’Brien PT, Overzier RA, de Pasquale M, Racusin J, Rea N, York DG. An extremely luminous X-ray outburst at the birth of a supernova. Nature 2008; 453:469-74. [PMID: 18497815 DOI: 10.1038/nature06997] [Citation(s) in RCA: 352] [Impact Index Per Article: 22.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/11/2008] [Accepted: 04/04/2008] [Indexed: 11/09/2022]
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7
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Gehrels N, Norris JP, Barthelmy SD, Granot J, Kaneko Y, Kouveliotou C, Markwardt CB, Mészáros P, Nakar E, Nousek JA, O'Brien PT, Page M, Palmer DM, Parsons AM, Roming PWA, Sakamoto T, Sarazin CL, Schady P, Stamatikos M, Woosley SE. A new gamma-ray burst classification scheme from GRB 060614. Nature 2007; 444:1044-6. [PMID: 17183315 DOI: 10.1038/nature05376] [Citation(s) in RCA: 44] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/30/2006] [Accepted: 10/20/2006] [Indexed: 11/09/2022]
Abstract
Gamma-ray bursts (GRBs) are known to come in two duration classes, separated at approximately 2 s. Long-duration bursts originate from star-forming regions in galaxies, have accompanying supernovae when these are near enough to observe and are probably caused by massive-star collapsars. Recent observations show that short-duration bursts originate in regions within their host galaxies that have lower star-formation rates, consistent with binary neutron star or neutron star-black hole mergers. Moreover, although their hosts are predominantly nearby galaxies, no supernovae have been so far associated with short-duration GRBs. Here we report that the bright, nearby GRB 060614 does not fit into either class. Its approximately 102-s duration groups it with long-duration GRBs, while its temporal lag and peak luminosity fall entirely within the short-duration GRB subclass. Moreover, very deep optical observations exclude an accompanying supernova, similar to short-duration GRBs. This combination of a long-duration event without an accompanying supernova poses a challenge to both the collapsar and the merging-neutron-star interpretations and opens the door to a new GRB classification scheme that straddles both long- and short-duration bursts.
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Affiliation(s)
- N Gehrels
- NASA/Goddard Space Flight Center, Greenbelt, Maryland 20771, USA.
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8
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Soderberg AM, Kulkarni SR, Nakar E, Berger E, Cameron PB, Fox DB, Frail D, Gal-Yam A, Sari R, Cenko SB, Kasliwal M, Chevalier RA, Piran T, Price PA, Schmidt BP, Pooley G, Moon DS, Penprase BE, Ofek E, Rau A, Gehrels N, Nousek JA, Burrows DN, Persson SE, McCarthy PJ. Relativistic ejecta from X-ray flash XRF 060218 and the rate of cosmic explosions. Nature 2006; 442:1014-7. [PMID: 16943832 DOI: 10.1038/nature05087] [Citation(s) in RCA: 383] [Impact Index Per Article: 21.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/18/2006] [Accepted: 07/13/2006] [Indexed: 11/09/2022]
Abstract
Over the past decade, long-duration gamma-ray bursts (GRBs)--including the subclass of X-ray flashes (XRFs)--have been revealed to be a rare variety of type Ibc supernova. Although all these events result from the death of massive stars, the electromagnetic luminosities of GRBs and XRFs exceed those of ordinary type Ibc supernovae by many orders of magnitude. The essential physical process that causes a dying star to produce a GRB or XRF, and not just a supernova, is still unknown. Here we report radio and X-ray observations of XRF 060218 (associated with supernova SN 2006aj), the second-nearest GRB identified until now. We show that this event is a hundred times less energetic but ten times more common than cosmological GRBs. Moreover, it is distinguished from ordinary type Ibc supernovae by the presence of 10(48) erg coupled to mildly relativistic ejecta, along with a central engine (an accretion-fed, rapidly rotating compact source) that produces X-rays for weeks after the explosion. This suggests that the production of relativistic ejecta is the key physical distinction between GRBs or XRFs and ordinary supernovae, while the nature of the central engine (black hole or magnetar) may distinguish typical bursts from low-luminosity, spherical events like XRF 060218.
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Affiliation(s)
- A M Soderberg
- Caltech Optical Observatories 105-24, California Institute of Technology, Pasadena, California 91125, USA.
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9
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Fox DB, Frail DA, Price PA, Kulkarni SR, Berger E, Piran T, Soderberg AM, Cenko SB, Cameron PB, Gal-Yam A, Kasliwal MM, Moon DS, Harrison FA, Nakar E, Schmidt BP, Penprase B, Chevalier RA, Kumar P, Roth K, Watson D, Lee BL, Shectman S, Phillips MM, Roth M, McCarthy PJ, Rauch M, Cowie L, Peterson BA, Rich J, Kawai N, Aoki K, Kosugi G, Totani T, Park HS, MacFadyen A, Hurley KC. The afterglow of GRB 050709 and the nature of the short-hard gamma-ray bursts. Nature 2005; 437:845-50. [PMID: 16208362 DOI: 10.1038/nature04189] [Citation(s) in RCA: 391] [Impact Index Per Article: 20.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/11/2005] [Accepted: 08/30/2005] [Indexed: 11/09/2022]
Abstract
The final chapter in the long-standing mystery of the gamma-ray bursts (GRBs) centres on the origin of the short-hard class of bursts, which are suspected on theoretical grounds to result from the coalescence of neutron-star or black-hole binary systems. Numerous searches for the afterglows of short-hard bursts have been made, galvanized by the revolution in our understanding of long-duration GRBs that followed the discovery in 1997 of their broadband (X-ray, optical and radio) afterglow emission. Here we present the discovery of the X-ray afterglow of a short-hard burst, GRB 050709, whose accurate position allows us to associate it unambiguously with a star-forming galaxy at redshift z = 0.160, and whose optical lightcurve definitively excludes a supernova association. Together with results from three other recent short-hard bursts, this suggests that short-hard bursts release much less energy than the long-duration GRBs. Models requiring young stellar populations, such as magnetars and collapsars, are ruled out, while coalescing degenerate binaries remain the most promising progenitor candidates.
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Affiliation(s)
- D B Fox
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, California 91125, USA.
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10
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11
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Cameron PB, Chandra P, Ray A, Kulkarni SR, Frail DA, Wieringa MH, Nakar E, Phinney ES, Miyazaki A, Tsuboi M, Okumura S, Kawai N, Menten KM, Bertoldi F. Detection of a radio counterpart to the 27 December 2004 giant flare from SGR 1806–20. Nature 2005; 434:1112-5. [PMID: 15858569 DOI: 10.1038/nature03605] [Citation(s) in RCA: 113] [Impact Index Per Article: 5.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/09/2005] [Accepted: 04/05/2005] [Indexed: 11/08/2022]
Abstract
It was established over a decade ago that the remarkable high-energy transients known as soft gamma-ray repeaters (SGRs) are located in our Galaxy and originate from neutron stars with intense (< or = 10(15)G) magnetic fields-so-called 'magnetars'. On 27 December 2004, a giant flare with a fluence exceeding 0.3 erg cm(-2) was detected from SGR 1806-20. Here we report the detection of a fading radio counterpart to this event. We began a monitoring programme from 0.2 to 250 GHz and obtained a high-resolution 21-cm radio spectrum that traces the intervening interstellar neutral hydrogen clouds. Analysis of the spectrum yields the first direct distance measurement of SGR 1806-20: the source is located at a distance greater than 6.4 kpc and we argue that it is nearer than 9.8 kpc. If correct, our distance estimate lowers the total energy of the explosion and relaxes the demands on theoretical models. The energetics and the rapid decay of the radio source are not compatible with the afterglow model that is usually invoked for gamma-ray bursts. Instead, we suggest that the rapidly decaying radio emission arises from the debris ejected during the explosion.
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Affiliation(s)
- P B Cameron
- Division of Physics, Mathematics and Astronomy, 105-24, California Institute of Technology, Pasadena, California 91125, USA.
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12
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Nakar E, Friedland L. Passage through resonance and autoresonance in x(2n)-type potentials. Phys Rev E Stat Phys Plasmas Fluids Relat Interdiscip Topics 1999; 60:5479-85. [PMID: 11970422 DOI: 10.1103/physreve.60.5479] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/07/1999] [Indexed: 04/18/2023]
Abstract
Resonant dynamics of a particle in an x(2n)-type potential driven by an oscillation with adiabatically varying frequency is investigated. It is shown that, under certain conditions, when the driving frequency increases in time and passes the resonance with the unperturbed system, the oscillator phase locks to the drive and, later, this phase locking is sustained, i.e., the system remains in autoresonance. The initial phase locking by passage through resonance is the main ingredient of the transition to autoresonance and comprises the generalization of previous results for nearly parabolic potentials.
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Affiliation(s)
- E Nakar
- Racah Institute of Physics, Hebrew University of Jerusalem, 91904 Jerusalem, Israel
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