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O'Connor B, Troja E, Ryan G, Beniamini P, van Eerten H, Granot J, Dichiara S, Ricci R, Lipunov V, Gillanders JH, Gill R, Moss M, Anand S, Andreoni I, Becerra RL, Buckley DAH, Butler NR, Cenko SB, Chasovnikov A, Durbak J, Francile C, Hammerstein E, van der Horst AJ, Kasliwal MM, Kouveliotou C, Kutyrev AS, Lee WH, Srinivasaragavan GP, Topolev V, Watson AM, Yang Y, Zhirkov K. A structured jet explains the extreme GRB 221009A. SCIENCE ADVANCES 2023; 9:eadi1405. [PMID: 37285439 DOI: 10.1126/sciadv.adi1405] [Citation(s) in RCA: 2] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/05/2023] [Accepted: 05/02/2023] [Indexed: 06/09/2023]
Abstract
Long-duration gamma-ray bursts (GRBs) are powerful cosmic explosions, signaling the death of massive stars. Among them, GRB 221009A is by far the brightest burst ever observed. Because of its enormous energy (Eiso ≈ 1055 erg) and proximity (z ≈ 0.15), GRB 221009A is an exceptionally rare event that pushes the limits of our theories. We present multiwavelength observations covering the first 3 months of its afterglow evolution. The x-ray brightness decays as a power law with slope ≈t-1.66, which is not consistent with standard predictions for jetted emission. We attribute this behavior to a shallow energy profile of the relativistic jet. A similar trend is observed in other energetic GRBs, suggesting that the most extreme explosions may be powered by structured jets launched by a common central engine.
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Affiliation(s)
- Brendan O'Connor
- Department of Physics, The George Washington University, 725 21st Street NW, Washington, DC 20052, USA
- Astronomy, Physics and Statistics Institute of Sciences (APSIS), Washington, DC 20052, USA
- Department of Astronomy, University of Maryland, College Park, MD 20742-4111, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA
| | - Eleonora Troja
- Department of Physics, University of Rome "Tor Vergata", via della Ricerca Scientifica 1, I-00133 Rome, Italy
- INAF - Istituto di Astrofisica e Planetologia Spaziali, via Fosso del Cavaliere 100, 00133 Rome, Italy
| | - Geoffrey Ryan
- Perimeter Institute for Theoretical Physics, 31 Caroline St. N., Waterloo, ON N2L 2Y5, Canada
| | - Paz Beniamini
- Department of Natural Sciences, The Open University of Israel, P.O. Box 808, Ra'anana 4353701, Israel
- Astrophysics Research Center of the Open university (ARCO), P.O. Box 808, Ra'anana 4353701, Israel
| | - Hendrik van Eerten
- Physics Department, University of Bath, Claverton Down, Bath BA2 7AY, UK
| | - Jonathan Granot
- Department of Physics, The George Washington University, 725 21st Street NW, Washington, DC 20052, USA
- Department of Natural Sciences, The Open University of Israel, P.O. Box 808, Ra'anana 4353701, Israel
- Astrophysics Research Center of the Open university (ARCO), P.O. Box 808, Ra'anana 4353701, Israel
| | - Simone Dichiara
- The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA
| | - Roberto Ricci
- Istituto Nazionale di Ricerca Metrologica, I-10135 Torino, Italy
- INAF - Istituto di Radioastronomia, via Gobetti 101, I-40129 Bologna, Italy
| | - Vladimir Lipunov
- Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetsky pr. 13, 119234 Moscow, Russia
| | - James H Gillanders
- Department of Physics, University of Rome "Tor Vergata", via della Ricerca Scientifica 1, I-00133 Rome, Italy
| | - Ramandeep Gill
- Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Antigua Carretera. a Pátzcuaro #8701, Ex-Hda. San José de la Huerta, Morelia, Michoacán, C.P. 58089, México
| | - Michael Moss
- Department of Physics, The George Washington University, 725 21st Street NW, Washington, DC 20052, USA
| | - Shreya Anand
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - Igor Andreoni
- Department of Astronomy, University of Maryland, College Park, MD 20742-4111, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA
- Joint Space-Science Institute, University of Maryland, College Park, MD 20742, USA
| | - Rosa L Becerra
- Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, 04510 México, CDMX, Mexico
| | - David A H Buckley
- Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch 7701, South Africa
- South African Astronomical Observatory, PO Box 9, 7935 Observatory, Cape Town, South Africa
| | - Nathaniel R Butler
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA
| | - Stephen B Cenko
- Astrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA
- Joint Space-Science Institute, University of Maryland, College Park, MD 20742, USA
| | - Aristarkh Chasovnikov
- Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetsky pr. 13, 119234 Moscow, Russia
| | - Joseph Durbak
- Department of Astronomy, University of Maryland, College Park, MD 20742-4111, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA
| | - Carlos Francile
- Observatorio Astronomico Felix Aguilar (OAFA), San Juan 5400, Argentina
- Facultad de Ciencias Exactas Fisicas y Naturales, San Juan National University, San Juan 5400, Argentina
| | - Erica Hammerstein
- Department of Astronomy, University of Maryland, College Park, MD 20742-4111, USA
| | - Alexander J van der Horst
- Department of Physics, The George Washington University, 725 21st Street NW, Washington, DC 20052, USA
| | - Mansi M Kasliwal
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | | | - Alexander S Kutyrev
- Department of Astronomy, University of Maryland, College Park, MD 20742-4111, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA
| | - William H Lee
- Instituto de Astronomía, Universidad Nacional Autónoma de México, 04510 México, CDMX, Mexico
| | | | - Vladislav Topolev
- Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetsky pr. 13, 119234 Moscow, Russia
| | - Alan M Watson
- Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetsky pr. 13, 119234 Moscow, Russia
| | - Yuhan Yang
- Department of Physics, University of Rome "Tor Vergata", via della Ricerca Scientifica 1, I-00133 Rome, Italy
| | - Kirill Zhirkov
- Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetsky pr. 13, 119234 Moscow, Russia
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Gamma-Ray Bursts Afterglow Physics and the VHE Domain. GALAXIES 2022. [DOI: 10.3390/galaxies10030066] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/07/2022]
Abstract
Afterglow radiation in gamma-ray bursts (GRB), extending from the radio band to GeV energies, is produced as a result of the interaction between the relativistic jet and the ambient medium. Although in general the origin of the emission is robustly identified as synchrotron radiation from the shock-accelerated electrons, many aspects remain poorly constrained, such as the role of inverse Compton emission, the particle acceleration mechanism, the properties of the environment and of the GRB jet itself. The extension of the afterglow emission into the TeV band has been discussed and theorized for years, but has eluded for a long time the observations. Recently, the Cherenkov telescopes, MAGIC and H.E.S.S., have unequivocally proven that afterglow radiation is also produced above 100 GeV, up to at least a few TeV. The accessibility of the TeV spectral window will largely improve with the upcoming facility CTA (the Cherenkov Telescope Array). In this review article, we first revise the current model for afterglow emission in GRBs, its limitations and open issues. Then, we describe the recent detections of very high energy emission from GRBs and the origin of this radiation. Implications on the understanding of afterglow radiation and constraints on the physics of the involved processes will be deeply investigated, demonstrating how future observations, especially by the CTA Observatory, are expected to give a key contribution in improving our comprehension of such elusive sources.
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Abstract
The recent multi-messenger and multi-wavelength observations of gamma-ray bursts (GRBs) have encouraged renewed interest in these energetic events. In spite of the substantial amount of data accumulated during the past few decades, the nature of the prompt emission remains an unsolved puzzle. We present an overview of the leading models for their prompt emission phase, focusing on the perspective opened by future missions.
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Bret A. Quantum electrodynamic effects on counter-streaming instabilities in the whole k space. Phys Rev E 2022; 105:015205. [PMID: 35193210 DOI: 10.1103/physreve.105.015205] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/28/2021] [Accepted: 01/01/2022] [Indexed: 06/14/2023]
Abstract
In a recent work [Bret, EPL 135, 35001 (2021)10.1209/0295-5075/ac1e44], quantum electrodynamic (QED) effects were evaluated for the two-stream instability. It pertains to the growth of perturbations with a wave vector oriented along the flow in a collisionless counter-streaming system. Here, the analysis is extended to every possible orientation of the wave vector. The previous result for the two-stream instability is recovered, and it is proved that, even within the framework of a three-dimensional (3D) analysis, this instability remains fundamentally 1D even when accounting for QED effects. The filamentation instability, found for wave vectors normal to the flow, is weakly affected by QED corrections. As in the classical case, its growth rate saturates at large k_{⊥}. The saturation value is found independent of QED corrections. Also, the smallest unstable k_{⊥} is independent of QED corrections. Surprisingly, unstable modes found for oblique wave vectors do not follow the same pattern. For some, QED corrections do reduce the growth rate. But, for others, the same corrections increase the growth rate instead. The possibility for QED effects to play a role in unmagnetized systems is evaluated. Pair production resulting from γ emission by particles oscillating in the exponentially growing fields is not accounted for.
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Affiliation(s)
- Antoine Bret
- ETSI Industriales, Universidad de Castilla-La Mancha, 13071 Ciudad Real, Spain and Instituto de Investigaciones Energéticas y Aplicaciones Industriales, Campus Universitario de Ciudad Real, 13071 Ciudad Real, Spain
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Abstract
Gamma-ray Bursts (GRBs) are highly energetic events that can be observed at extremely high redshift. However, inherent bias in GRB data due to selection effects and redshift evolution can significantly skew any subsequent analysis. We correct for important variables related to the GRB emission, such as the burst duration, T90*, the prompt isotropic energy, Eiso, the rest-frame end time of the plateau emission, Ta,radio*, and its correspondent luminosity La,radio, for radio afterglow. In particular, we use the Efron–Petrosian method presented in 1992 for the correction of our variables of interest. Specifically, we correct Eiso and T90* for 80 GRBs, and La,radio and Ta,radio* for a subsample of 18 GRBs that present a plateau-like flattening in their light curve. Upon application of this method, we find strong evolution with redshift in most variables, particularly in La,radio, with values similar to those found in past and current literature in radio, X-ray and optical wavelengths, indicating that these variables are susceptible to observational bias. This analysis emphasizes the necessity of correcting observational data for evolutionary effects to obtain the intrinsic behavior of correlations to use them as discriminators among the most plausible theoretical models and as reliable cosmological tools.
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Spectral index-flux relation for investigating the origins of steep decay in γ-ray bursts. Nat Commun 2021; 12:4040. [PMID: 34234132 PMCID: PMC8263623 DOI: 10.1038/s41467-021-24246-x] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/08/2020] [Accepted: 05/28/2021] [Indexed: 11/09/2022] Open
Abstract
γ-ray bursts (GRBs) are short-lived transients releasing a large amount of energy (1051 - 1053 erg) in the keV-MeV energy range. GRBs are thought to originate from internal dissipation of the energy carried by ultra-relativistic jets launched by the remnant of a massive star's death or a compact binary coalescence. While thousands of GRBs have been observed over the last thirty years, we still have an incomplete understanding of where and how the radiation is generated in the jet. Here we show a relation between the spectral index and the flux found by investigating the X-ray tails of bright GRB pulses via time-resolved spectral analysis. This relation is incompatible with the long standing scenario which invokes the delayed arrival of photons from high-latitude parts of the jet. While the alternative scenarios cannot be firmly excluded, the adiabatic cooling of the emitting particles is the most plausible explanation for the discovered relation, suggesting a proton-synchrotron origin of the GRB emission.
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Abstract
The origin and phenomenology of the Fast Radio Burst (FRB) remains unknown despite more than a decade of efforts. Though several models have been proposed to explain the observed data, none is able to explain alone the variety of events so far recorded. The leading models consider magnetars as potential FRB sources. The recent detection of FRBs from the galactic magnetar SGR J1935+2154 seems to support them. Still, emission duration and energetic budget challenge all these models. Like for other classes of objects initially detected in a single band, it appeared clear that any solution to the FRB enigma could only come from a coordinated observational and theoretical effort in an as wide as possible energy band. In particular, the detection and localisation of optical/NIR or/and high-energy counterparts seemed an unavoidable starting point that could shed light on the FRB physics. Multiwavelength (MWL) search campaigns were conducted for several FRBs, in particular for repeaters. Here we summarize the observational and theoretical results and the perspectives in view of the several new sources accurately localised that will likely be identified by various radio facilities worldwide. We conclude that more dedicated MWL campaigns sensitive to the millisecond–minute timescale transients are needed to address the various aspects involved in the identification of FRB counterparts. Dedicated instrumentation could be one of the key points in this respect. In the optical/NIR band, fast photometry looks to be the only viable strategy. Additionally, small/medium size radiotelescopes co-pointing higher energies telescopes look a very interesting and cheap complementary observational strategy.
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Bragin S, Di Piazza A. Electron-positron annihilation into two photons in an intense plane-wave field. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.102.116012] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Abstract
Neutron stars, and magnetars in particular, are known to host the strongest magnetic fields in the Universe. The origin of these strong fields is a matter of controversy. In this preliminary work, via numerical simulations, we study, for the first time in non-ideal general relativistic magnetohydrodynamic (GRMHD) regime, the growth of the magnetic field due to the action of the mean-field dynamo due to sub-scale, unresolved turbulence. The dynamo process, combined with the differential rotation of the (proto-)star, is able to produce an exponential growth of any initial magnetic seed field up to the values required to explain the observations. By varying the dynamo coefficient we obtain different growth rates. We find a quasi-linear dependence of the growth rates on the intensity of the dynamo. Furthermore, the time interval in which exponential growth occurs and the growth rates also seems to depend on the initial configuration of the magnetic field.
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Enoto T, Kisaka S, Shibata S. Observational diversity of magnetized neutron stars. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2019; 82:106901. [PMID: 31549688 DOI: 10.1088/1361-6633/ab3def] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
Young and rotation-powered neutron stars (NSs) are commonly observed as rapidly-spinning pulsars. They dissipate their rotational energy by emitting pulsar wind with electromagnetic radiation and spin down at a steady rate, according to the simple steadily-rotating magnetic dipole model. In reality, however, multiwavelength observations of radiation from the NS surface and magnetosphere have revealed that the evolution and properties of NSs are highly diverse, often dubbed as 'NS zoo'. In particular, many of young and highly magnetized NSs show a high degree of activities, such as sporadic electromagnetic outbursts and irregular changes in pulse arrival times. Importantly, their magnetic field, which are the strongest in the universe, makes them ideal laboratories for fundamental physics. A class of highly-magnetized isolated NSs is empirically divided into several subclasses. In a broad classification, they are, in the order of the magnetic field strength (B) from the highest, 'magnetars' (historically recognized as soft gamma-ray repeaters and/or anomalous x-ray pulsars), 'high-B pulsars', and (nearby) x-ray isolated NSs. This article presents an introductory review for non-astrophysicists about the observational properties of highly-magnetized NSs, and their implications. The observed dynamic nature of NSs must be interpreted in conjunction with transient magnetic activities triggered during magnetic-energy dissipation process. In particular, we focus on how the five fundamental quantities of NSs, i.e. mass, radius, spin period, surface temperature, and magnetic fields, as observed with modern instruments, change with evolution of, and vary depending on the class of, the NSs. They are the foundation for a future unified theory of NSs.
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Affiliation(s)
- Teruaki Enoto
- Department of Astronomy and The Hakubi Center for Advanced Research, Kyoto University, Kyoto 606-8302, Japan
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Xiao D, Peng ZK, Zhang BB, Dai ZG. Prompt Emission of Gamma-Ray Bursts from the Wind of Newborn Millisecond Magnetars: A Case Study of GRB 160804A. THE ASTROPHYSICAL JOURNAL 2018; 867:52. [DOI: 10.3847/1538-4357/aae52f] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/01/2023]
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Ho WCG. Gravitational waves from neutron stars and asteroseismology. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2018; 376:rsta.2017.0285. [PMID: 29661975 PMCID: PMC5915648 DOI: 10.1098/rsta.2017.0285] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 01/08/2018] [Indexed: 06/08/2023]
Abstract
Neutron stars are born in the supernova explosion of massive stars. Neutron stars rotate as stably as atomic clocks and possess densities exceeding that of atomic nuclei and magnetic fields millions to billions of times stronger than those created in laboratories on the Earth. The physical properties of neutron stars are determined by many areas of fundamental physics, and detection of gravitational waves can provide invaluable insights into our understanding of these areas. Here, we describe some of the physics and astrophysics of neutron stars and how traditional electromagnetic wave observations provide clues to the sorts of gravitational waves we expect from these stars. We pay particular attention to neutron star fluid oscillations, examining their impact on electromagnetic and gravitational wave observations when these stars are in a wide binary or isolated system, then during binary inspiral right before merger, and finally at times soon after merger.This article is part of a discussion meeting issue 'The promises of gravitational-wave astronomy'.
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Affiliation(s)
- Wynn C G Ho
- Mathematical Sciences, Physics and Astronomy, and STAG Research Centre, University of Southampton, Southampton SO17 1BJ, UK
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Zhang BT, Murase K, Kimura SS, Horiuchi S, Mészáros P. Low-luminosity gamma-ray bursts as the sources of ultrahigh-energy cosmic ray nuclei. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.083010] [Citation(s) in RCA: 48] [Impact Index Per Article: 8.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Using Gravitational-wave Observations and Quasi-universal Relations to Constrain the Maximum Mass of Neutron Stars. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/2041-8213/aaa401] [Citation(s) in RCA: 436] [Impact Index Per Article: 72.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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GRB 170817A Associated with GW170817: Multi-frequency Observations and Modeling of Prompt Gamma-Ray Emission. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/2041-8213/aaa2f6] [Citation(s) in RCA: 70] [Impact Index Per Article: 11.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Joshi S, Jain SR. Noncyclic geometric phases and helicity transitions for neutrino oscillations in a magnetic field. Int J Clin Exp Med 2017. [DOI: 10.1103/physrevd.96.096004] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/2041-8213/aa920c] [Citation(s) in RCA: 1795] [Impact Index Per Article: 256.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Schady P. Gamma-ray bursts and their use as cosmic probes. ROYAL SOCIETY OPEN SCIENCE 2017; 4:170304. [PMID: 28791158 PMCID: PMC5541553 DOI: 10.1098/rsos.170304] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/31/2017] [Accepted: 06/28/2017] [Indexed: 06/07/2023]
Abstract
Since the launch of the highly successful and ongoing Swift mission, the field of gamma-ray bursts (GRBs) has undergone a revolution. The arcsecond GRB localizations available within just a few minutes of the GRB alert has signified the continual sampling of the GRB evolution through the prompt to afterglow phases revealing unexpected flaring and plateau phases, the first detection of a kilonova coincident with a short GRB, and the identification of samples of low-luminosity, ultra-long and highly dust-extinguished GRBs. The increased numbers of GRB afterglows, GRB-supernova detections, redshifts and host galaxy associations has greatly improved our understanding of what produces and powers these immense, cosmological explosions. Nevertheless, more high-quality data often also reveal greater complexity. In this review, I summarize some of the milestones made in GRB research during the Swift era, and how previous widely accepted theoretical models have had to adapt to accommodate the new wealth of observational data.
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Affiliation(s)
- Patricia Schady
- Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany
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X-RAY COUNTERPART OF GRAVITATIONAL WAVES DUE TO BINARY NEUTRON STAR MERGERS: LIGHT CURVES, LUMINOSITY FUNCTION, AND EVENT RATE DENSITY. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-4357/835/1/7] [Citation(s) in RCA: 40] [Impact Index Per Article: 5.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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THE SPECTRAL SN-GRB CONNECTION: SYSTEMATIC SPECTRAL COMPARISONS BETWEEN TYPE Ic SUPERNOVAE AND BROAD-LINED TYPE Ic SUPERNOVAE WITH AND WITHOUT GAMMA-RAY BURSTS. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0004-637x/832/2/108] [Citation(s) in RCA: 108] [Impact Index Per Article: 13.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Rea N, Gullón M, Pons JA, Perna R, Dainotti MG, Miralles JA, Torres DF. CONSTRAINING THE GRB-MAGNETAR MODEL BY MEANS OF THE GALACTIC PULSAR POPULATION. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/813/2/92] [Citation(s) in RCA: 45] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Turolla R, Zane S, Watts AL. Magnetars: the physics behind observations. A review. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2015; 78:116901. [PMID: 26473534 DOI: 10.1088/0034-4885/78/11/116901] [Citation(s) in RCA: 18] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/05/2023]
Abstract
Magnetars are the strongest magnets in the present universe and the combination of extreme magnetic field, gravity and density makes them unique laboratories to probe current physical theories (from quantum electrodynamics to general relativity) in the strong field limit. Magnetars are observed as peculiar, burst-active x-ray pulsars, the anomalous x-ray pulsars (AXPs) and the soft gamma repeaters (SGRs); the latter emitted also three 'giant flares', extremely powerful events during which luminosities can reach up to 10(47) erg s(-1) for about one second. The last five years have witnessed an explosion in magnetar research which has led, among other things, to the discovery of transient, or 'outbursting', and 'low-field' magnetars. Substantial progress has been made also on the theoretical side. Quite detailed models for explaining the magnetars' persistent x-ray emission, the properties of the bursts, the flux evolution in transient sources have been developed and confronted with observations. New insight on neutron star asteroseismology has been gained through improved models of magnetar oscillations. The long-debated issue of magnetic field decay in neutron stars has been addressed, and its importance recognized in relation to the evolution of magnetars and to the links among magnetars and other families of isolated neutron stars. The aim of this paper is to present a comprehensive overview in which the observational results are discussed in the light of the most up-to-date theoretical models and their implications. This addresses not only the particular case of magnetar sources, but the more fundamental issue of how physics in strong magnetic fields can be constrained by the observations of these unique sources.
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Affiliation(s)
- R Turolla
- Department of Physics and Astronomy, University of Padova, via Marzolo 8, 35131 Padova, Italy. Mullard Space Science Laboratory, University College London, Holbury St. Mary, Surrey, RH5 6NT, UK
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Fryer CL, Belczynski K, Ramirez-Ruiz E, Rosswog S, Shen G, Steiner AW. THE FATE OF THE COMPACT REMNANT IN NEUTRON STAR MERGERS. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/812/1/24] [Citation(s) in RCA: 64] [Impact Index Per Article: 7.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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Vreeswijk PM, Savaglio S, Gal-Yam A, De Cia A, Quimby RM, Sullivan M, Cenko SB, Perley DA, Filippenko AV, Clubb KI, Taddia F, Sollerman J, Leloudas G, Arcavi I, Rubin A, Kasliwal MM, Cao Y, Yaron O, Tal D, Ofek EO, Capone J, Kutyrev AS, Toy V, Nugent PE, Laher R, Surace J, Kulkarni SR. THE HYDROGEN-POOR SUPERLUMINOUS SUPERNOVA iPTF 13ajg AND ITS HOST GALAXY IN ABSORPTION AND EMISSION. ACTA ACUST UNITED AC 2014. [DOI: 10.1088/0004-637x/797/1/24] [Citation(s) in RCA: 87] [Impact Index Per Article: 8.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Nakamura T, Kashiyama K, Nakauchi D, Suwa Y, Sakamoto T, Kawai N. SOFT X-RAY EXTENDED EMISSIONS OF SHORT GAMMA-RAY BURSTS AS ELECTROMAGNETIC COUNTERPARTS OF COMPACT BINARY MERGERS: POSSIBLE ORIGIN AND DETECTABILITY. ACTA ACUST UNITED AC 2014. [DOI: 10.1088/0004-637x/796/1/13] [Citation(s) in RCA: 18] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Uzdensky DA, Rightley S. Plasma physics of extreme astrophysical environments. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2014; 77:036902. [PMID: 24595053 DOI: 10.1088/0034-4885/77/3/036902] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/03/2023]
Abstract
Among the incredibly diverse variety of astrophysical objects, there are some that are characterized by very extreme physical conditions not encountered anywhere else in the Universe. Of special interest are ultra-magnetized systems that possess magnetic fields exceeding the critical quantum field of about 44 TG. There are basically only two classes of such objects: magnetars, whose magnetic activity is manifested, e.g., via their very short but intense gamma-ray flares, and central engines of supernovae (SNe) and gamma-ray bursts (GRBs)--the most powerful explosions in the modern Universe. Figuring out how these complex systems work necessarily requires understanding various plasma processes, both small-scale kinetic and large-scale magnetohydrodynamic (MHD), that govern their behavior. However, the presence of an ultra-strong magnetic field modifies the underlying basic physics to such a great extent that relying on conventional, classical plasma physics is often not justified. Instead, plasma-physical problems relevant to these extreme astrophysical environments call for constructing relativistic quantum plasma (RQP) physics based on quantum electrodynamics (QED). In this review, after briefly describing the astrophysical systems of interest and identifying some of the key plasma-physical problems important to them, we survey the recent progress in the development of such a theory. We first discuss the ways in which the presence of a super-critical field modifies the properties of vacuum and matter and then outline the basic theoretical framework for describing both non-relativistic and RQPs. We then turn to some specific astrophysical applications of relativistic QED plasma physics relevant to magnetar magnetospheres and to central engines of core-collapse SNe and long GRBs. Specifically, we discuss the propagation of light through a magnetar magnetosphere; large-scale MHD processes driving magnetar activity and responsible for jet launching and propagation in GRBs; energy-transport processes governing the thermodynamics of extreme plasma environments; micro-scale kinetic plasma processes important in the interaction of intense electric currents flowing through a magnetar magnetosphere with the neutron star surface; and magnetic reconnection of ultra-strong magnetic fields. Finally, we point out that future progress in applying RQP physics to real astrophysical problems will require the development of suitable numerical modeling capabilities.
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Affiliation(s)
- Dmitri A Uzdensky
- Center for Integrated Plasma Studies, Physics Department, University of Colorado, UCB 390, Boulder, CO 80309-0390,USA
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Murase K, Dasgupta B, Thompson TA. Quasithermal neutrinos from rotating protoneutron stars born during core collapse of massive stars. Int J Clin Exp Med 2014. [DOI: 10.1103/physrevd.89.043012] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Abstract
Gamma-ray bursts (GRBs) are bright flashes of gamma rays coming from the cosmos. They occur roughly once per day, typically last for tens of seconds, and are the most luminous events in the universe. More than three decades after their discovery, and after pioneering advances from space and ground experiments, they still remain mysterious. The launch of the Swift and Fermi satellites in 2004 and 2008 brought in a trove of qualitatively new data. In this Review, we survey the interplay between these recent observations and the theoretical models of the prompt GRB emission and the subsequent afterglow.
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Affiliation(s)
- Neil Gehrels
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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Suwa Y, Murase K. Probing the central engine of long gamma-ray bursts and hypernovae with gravitational waves and neutrinos. Int J Clin Exp Med 2009. [DOI: 10.1103/physrevd.80.123008] [Citation(s) in RCA: 30] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Magnetism in a cosmic blast. Nature 2009; 462:728-9. [DOI: 10.1038/462728a] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
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Shabad AE, Usov VV. Electric field of a pointlike charge in a strong magnetic field and ground state of a hydrogenlike atom. Int J Clin Exp Med 2008. [DOI: 10.1103/physrevd.77.025001] [Citation(s) in RCA: 54] [Impact Index Per Article: 3.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Bucciantini N, Quataert E, Arons J, Metzger BD, Thompson TA. Relativistic jets and long-duration gamma-ray bursts from the birth of magnetars. ACTA ACUST UNITED AC 2008. [DOI: 10.1111/j.1745-3933.2007.00403.x] [Citation(s) in RCA: 95] [Impact Index Per Article: 5.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/26/2022]
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Liang E, Zhang B, Zhang B. A Comprehensive Analysis of SwiftXRT Data. II. Diverse Physical Origins of the Shallow Decay Segment. THE ASTROPHYSICAL JOURNAL 2007; 670:565-583. [DOI: 10.1086/521870] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/01/2023]
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Woosley SE, Blinnikov S, Heger A. Pulsational pair instability as an explanation for the most luminous supernovae. Nature 2007; 450:390-2. [DOI: 10.1038/nature06333] [Citation(s) in RCA: 440] [Impact Index Per Article: 25.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/04/2007] [Accepted: 09/21/2007] [Indexed: 11/09/2022]
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Zhang B, Liang E, Zhang B. A Comprehensive Analysis of SwiftXRT Data. I. Apparent Spectral Evolution of Gamma‐Ray Burst X‐Ray Tails. THE ASTROPHYSICAL JOURNAL 2007; 666:1002-1011. [DOI: 10.1086/519548] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/01/2023]
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Shabad AE, Usov VV. Modified coulomb law in a strongly magnetized vacuum. PHYSICAL REVIEW LETTERS 2007; 98:180403. [PMID: 17501547 DOI: 10.1103/physrevlett.98.180403] [Citation(s) in RCA: 11] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/24/2006] [Revised: 12/14/2006] [Indexed: 05/15/2023]
Abstract
We study the electric potential of a charge placed in a strong magnetic field B>>B(0) approximately 4.4x10(13) G, as modified by the vacuum polarization. In such a field the electron Larmour radius is much less than its Compton length. At the Larmour distances a scaling law occurs, with the potential determined by a magnetic-field-independent function. The scaling regime implies short-range interaction, expressed by the Yukawa law. The electromagnetic interaction regains its long-range character at distances larger than the Compton length, the potential decreasing across B faster than along. Correction to the nonrelativistic ground-state energy of a hydrogenlike atom is found. In the limit B = infinity, the modified potential becomes the Dirac delta function plus a regular background. With this potential the ground-state energy is finite--the best pronounced effect of the vacuum polarization.
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Kumar P, McMahon E, Panaitescu A, Willingale R, O'Brien P, Burrows D, Cummings J, Gehrels N, Holland S, Pandey SB, Vanden Berk D, Zane S. The nature of the outflow in gamma-ray bursts. ACTA ACUST UNITED AC 2007. [DOI: 10.1111/j.1365-2966.2007.00286.x] [Citation(s) in RCA: 45] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/26/2022]
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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] [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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Shabad AE, Usov VV. Positronium collapse and the maximum magnetic field in pure QED. PHYSICAL REVIEW LETTERS 2006; 96:180401. [PMID: 16712344 DOI: 10.1103/physrevlett.96.180401] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/19/2006] [Indexed: 05/09/2023]
Abstract
A maximum value for the magnetic field is determined, which provides the full compensation of the positronium rest mass by the binding energy in the maximum symmetry state and disappearance of the energy gap separating the electron-positron system from the vacuum. The compensation becomes possible owing to the falling to the center phenomenon. The maximum magnetic field may be related to the vacuum and describe its structure.
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Affiliation(s)
- A E Shabad
- P. N. Lebedev Physics Institute, Moscow 117924, Russia
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Abstract
We report an extremely rapid mechanism for magnetic field amplification during the merger of a binary neutron star system. This has implications for the production of the short class of gamma-ray bursts, which recent observations suggest may originate in such mergers. In detailed magnetohydrodynamic simulations of the merger process, the fields are amplified by Kelvin-Helmholtz instabilities beyond magnetar field strength and may therefore represent the strongest magnetic fields in the universe. The amplification occurs in the shear layer that forms between the neutron stars and on a time scale of only 1 millisecond, that is, long before the remnant can collapse into a black hole.
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Affiliation(s)
- D J Price
- School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL, UK
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