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Pang PTH, Dietrich T, Coughlin MW, Bulla M, Tews I, Almualla M, Barna T, Kiendrebeogo RW, Kunert N, Mansingh G, Reed B, Sravan N, Toivonen A, Antier S, VandenBerg RO, Heinzel J, Nedora V, Salehi P, Sharma R, Somasundaram R, Van Den Broeck C. An updated nuclear-physics and multi-messenger astrophysics framework for binary neutron star mergers. Nat Commun 2023; 14:8352. [PMID: 38123551 PMCID: PMC10733434 DOI: 10.1038/s41467-023-43932-6] [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: 02/23/2023] [Accepted: 11/24/2023] [Indexed: 12/23/2023] Open
Abstract
The multi-messenger detection of the gravitational-wave signal GW170817, the corresponding kilonova AT2017gfo and the short gamma-ray burst GRB170817A, as well as the observed afterglow has delivered a scientific breakthrough. For an accurate interpretation of all these different messengers, one requires robust theoretical models that describe the emitted gravitational-wave, the electromagnetic emission, and dense matter reliably. In addition, one needs efficient and accurate computational tools to ensure a correct cross-correlation between the models and the observational data. For this purpose, we have developed the Nuclear-physics and Multi-Messenger Astrophysics framework NMMA. The code allows incorporation of nuclear-physics constraints at low densities as well as X-ray and radio observations of isolated neutron stars. In previous works, the NMMA code has allowed us to constrain the equation of state of supranuclear dense matter, to measure the Hubble constant, and to compare dense-matter physics probed in neutron-star mergers and in heavy-ion collisions, and to classify electromagnetic observations and perform model selection. Here, we show an extension of the NMMA code as a first attempt of analyzing the gravitational-wave signal, the kilonova, and the gamma-ray burst afterglow simultaneously. Incorporating all available information, we estimate the radius of a 1.4M⊙ neutron star to be [Formula: see text] km.
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Affiliation(s)
- Peter T H Pang
- Nikhef, Science Park 105, 1098 XG, Amsterdam, The Netherlands
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Princetonplein 1, 3584 CC, Utrecht, The Netherlands
| | - Tim Dietrich
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany.
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476, Potsdam, Germany.
| | - Michael W Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Mattia Bulla
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-106 91, Stockholm, Sweden
- Department of Physics and Earth Science, University of Ferrara, Via Saragat 1, I-44122, Ferrara, Italy
- INFN, Sezione di Ferrara, Via Saragat 1, I-44122, Ferrara, Italy
- INAF, Osservatorio Astronomico d'Abruzzo, Via Mentore Maggini snc, 64100, Teramo, Italy
| | - Ingo Tews
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, 87545, USA
| | - Mouza Almualla
- Department of Physics, American University of Sharjah, PO Box 26666, Sharjah, UAE
| | - Tyler Barna
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Ramodgwendé Weizmann Kiendrebeogo
- Laboratoire de Physique et de Chimie de l'Environnement, Université Joseph KI-ZERBO, Ouagadougou, Burkina Faso
- Observatoire de la Côte d'Azur, Université Côte d'Azur, CNRS, 96 Boulevard de l'Observatoire, F06304, Nice Cedex 4, France
| | - Nina Kunert
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany
| | - Gargi Mansingh
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
- Department of Physics, American University, Washington, DC, 20016, USA
| | - Brandon Reed
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
- Department of Physics and Astronomy, University of Minnesota-Duluth, Duluth, MN, 55812, USA
| | - Niharika Sravan
- Department of Physics, Drexel University, Philadelphia, PA, 19104, USA
| | - Andrew Toivonen
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Sarah Antier
- Observatoire de la Côte d'Azur, Université Côte d'Azur, CNRS, 96 Boulevard de l'Observatoire, F06304, Nice Cedex 4, France
| | - Robert O VandenBerg
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Jack Heinzel
- Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Ave, Cambridge, MA, 02139, USA
| | - Vsevolod Nedora
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476, Potsdam, Germany
| | - Pouyan Salehi
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany
| | - Ritwik Sharma
- Department of Physics, Deshbandhu College, University of Delhi, New Delhi, India
| | - Rahul Somasundaram
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, 87545, USA
- Université Lyon, Université Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, F-69622, Villeurbanne, France
- Department of Physics, Syracuse University, Syracuse, NY, 13244, USA
| | - Chris Van Den Broeck
- Nikhef, Science Park 105, 1098 XG, Amsterdam, The Netherlands
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Princetonplein 1, 3584 CC, Utrecht, The Netherlands
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Kiuchi K, Fujibayashi S, Hayashi K, Kyutoku K, Sekiguchi Y, Shibata M. Self-Consistent Picture of the Mass Ejection from a One Second Long Binary Neutron Star Merger Leaving a Short-Lived Remnant in a General-Relativistic Neutrino-Radiation Magnetohydrodynamic Simulation. PHYSICAL REVIEW LETTERS 2023; 131:011401. [PMID: 37478426 DOI: 10.1103/physrevlett.131.011401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/21/2022] [Revised: 05/22/2023] [Accepted: 06/02/2023] [Indexed: 07/23/2023]
Abstract
We perform a general-relativistic neutrino-radiation magnetohydrodynamic simulation of a one second-long binary neutron star merger on the Japanese supercomputer Fugaku using about 85 million CPU hours with 20 736 CPUs. We consider an asymmetric binary neutron star merger with masses of 1.2M_{⊙} and 1.5M_{⊙} and a "soft" equation of state SFHo. It results in a short-lived remnant with the lifetime of ≈0.017 s, and subsequent massive torus formation with the mass of ≈0.05M_{⊙} after the remnant collapses to a black hole. For the first time, we find that after the dynamical mass ejection, which drives the fast tail and mildly relativistic components, the postmerger mass ejection from the massive torus takes place due to the magnetorotational instability-driven turbulent viscosity in a single simulation and the two ejecta components are seen in the distributions of the electron fraction and velocity with distinct features.
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Affiliation(s)
- Kenta Kiuchi
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg, Potsdam-Golm 14476, Germany
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
| | - Sho Fujibayashi
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg, Potsdam-Golm 14476, Germany
| | - Kota Hayashi
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
| | - Koutarou Kyutoku
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
- Department of Physics, Kyoto University, Kyoto 606-8502, Japan
- Interdisciplinary Theoretical and Mathematical Science Program (iTHEMS), RIKEN, Wako, Saitama 351-0198, Japan
| | - Yuichiro Sekiguchi
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
- Department of Physics, Toho University, Funabashi, Chiba 274-8510, Japan
| | - Masaru Shibata
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg, Potsdam-Golm 14476, Germany
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
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Johnson JA, Fields BD, Thompson TA. The origin of the elements: a century of progress. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2020; 378:20190301. [PMID: 32811358 DOI: 10.1098/rsta.2019.0301] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 06/02/2020] [Indexed: 06/11/2023]
Abstract
This review assesses the current state of knowledge of how the elements were produced in the Big Bang, in stellar lives and deaths, and by interactions in interstellar gas. We begin with statements of fact and discuss the evidence that convinced astronomers that the Sun is fusing hydrogen, that low-mass stars produce heavy elements through neutron capture, that massive stars can explode as supernovae and that supernovae of all types produce new elements. Nucleosynthesis in the Big Bang, through cosmic ray spallation, and in exploding white dwarfs is only ranked below the above facts in certainty because the evidence, while overwhelming, is so far circumstantial. Next, we highlight the flaws in our current understanding of the predictions for lithium production in the Big Bang and/or its destruction in stars and for the production of the elements with atomic number [Formula: see text]. While the theory that neutron star mergers produce elements through neutron-capture has powerful circumstantial evidence, we are unconvinced that they produce all of the elements past nickel. Also in dispute is the exact mechanism or mechanisms that cause the white dwarfs to explode. It is difficult to determine the origin of rare isotopes because signatures of their production are weak. We are uncertain about the production sites of some lithium and nitrogen isotopes and proton-rich heavy nuclei. Finally, Betelgeuse is probably not the next star to become a supernovae in the Milky Way, in part because Betelgeuse may collapse directly to a black hole instead. The accumulated evidence in this review shows that we understand the major production sites for the elements, but islands of uncertainty in the periodic table exist. Resolving these uncertainties requires in particular understanding explosive events with compact objects and understanding the nature of the first stars and is therefore primed for new discoveries in the next decades. This article is part of the theme issue 'Mendeleev and the periodic table'.
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Affiliation(s)
- Jennifer A Johnson
- Department of Astronomy and Center for Cosmology and AstroParticle Physics, Ohio State University, Columbus, OH 43210, USA
| | - Brian D Fields
- Departments of Astronomy and of Physics, University of Illinois, Urbana, IL 61801, USA
| | - Todd A Thompson
- Department of Astronomy and Center for Cosmology and AstroParticle Physics, Ohio State University, Columbus, OH 43210, USA
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What Constraints on the Neutron Star Maximum Mass Can One Pose from GW170817 Observations? ACTA ACUST UNITED AC 2020. [DOI: 10.3847/1538-4357/ab80bd] [Citation(s) in RCA: 29] [Impact Index Per Article: 7.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Guridi JA, Pertuze JA, Pfotenhauer SM. Natural laboratories as policy instruments for technological learning and institutional capacity building: The case of Chile's astronomy cluster. RESEARCH POLICY 2020. [DOI: 10.1016/j.respol.2019.103899] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/25/2022]
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Abstract
The coalescence of double neutron star (NS-NS) and black hole (BH)-NS binaries are prime sources of gravitational waves (GW) for Advanced LIGO/Virgo and future ground-based detectors. Neutron-rich matter released from such events undergoes rapid neutron capture (r-process) nucleosynthesis as it decompresses into space, enriching our universe with rare heavy elements like gold and platinum. Radioactive decay of these unstable nuclei powers a rapidly evolving, approximately isotropic thermal transient known as a "kilonova", which probes the physical conditions during the merger and its aftermath. Here I review the history and physics of kilonovae, leading to the current paradigm of day-timescale emission at optical wavelengths from lanthanide-free components of the ejecta, followed by week-long emission with a spectral peak in the near-infrared (NIR). These theoretical predictions, as compiled in the original version of this review, were largely confirmed by the transient optical/NIR counterpart discovered to the first NS-NS merger, GW170817, discovered by LIGO/Virgo. Using a simple light curve model to illustrate the essential physical processes and their application to GW170817, I then introduce important variations about the standard picture which may be observable in future mergers. These include ∼ hour-long UV precursor emission, powered by the decay of free neutrons in the outermost ejecta layers or shock-heating of the ejecta by a delayed ultra-relativistic outflow; and enhancement of the luminosity from a long-lived central engine, such as an accreting BH or millisecond magnetar. Joint GW and kilonova observations of GW170817 and future events provide a new avenue to constrain the astrophysical origin of the r-process elements and the equation of state of dense nuclear matter.
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Affiliation(s)
- Brian D. Metzger
- Department of Physics, Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 USA
- Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010 USA
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GROWTH on S190425z: Searching Thousands of Square Degrees to Identify an Optical or Infrared Counterpart to a Binary Neutron Star Merger with the Zwicky Transient Facility and Palomar Gattini-IR. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/2041-8213/ab4ad8] [Citation(s) in RCA: 65] [Impact Index Per Article: 13.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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LSST Target-of-opportunity Observations of Gravitational-wave Events: Essential and Efficient. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/ab07b6] [Citation(s) in RCA: 26] [Impact Index Per Article: 5.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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10
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Foucart F, Duez M, Hinderer T, Caro J, Williamson AR, Boyle M, Buonanno A, Haas R, Hemberger D, Kidder L, Pfeiffer H, Scheel M. Gravitational waveforms from spectral Einstein code simulations: Neutron star-neutron star and low-mass black hole-neutron star binaries. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.044008] [Citation(s) in RCA: 32] [Impact Index Per Article: 6.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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12
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A Long-lived Remnant Neutron Star after GW170817 Inferred from Its Associated Kilonova. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aac6e5] [Citation(s) in RCA: 75] [Impact Index Per Article: 12.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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13
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An Upper Limit on the Linear Polarization Fraction of the GW170817 Radio Continuum. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/2041-8213/aacdfd] [Citation(s) in RCA: 26] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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14
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Three-dimensional GRMHD Simulations of Neutrino-cooled Accretion Disks from Neutron Star Mergers. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aabaec] [Citation(s) in RCA: 118] [Impact Index Per Article: 19.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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16
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Improved Constraints on
H
0
from a Combined Analysis of Gravitational-wave and Electromagnetic Emission from GW170817. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/2041-8213/aaa009] [Citation(s) in RCA: 65] [Impact Index Per Article: 9.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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The Combined Ultraviolet, Optical, and Near-infrared Light Curves of the Kilonova Associated with the Binary Neutron Star Merger GW170817: Unified Data Set, Analytic Models, and Physical Implications. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/2041-8213/aa9c84] [Citation(s) in RCA: 270] [Impact Index Per Article: 38.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Kasen D, Metzger B, Barnes J, Quataert E, Ramirez-Ruiz E. Origin of the heavy elements in binary neutron-star mergers from a gravitational-wave event. Nature 2017; 551:80-84. [PMID: 29094687 DOI: 10.1038/nature24453] [Citation(s) in RCA: 84] [Impact Index Per Article: 12.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/13/2017] [Accepted: 09/25/2017] [Indexed: 11/09/2022]
Abstract
The cosmic origin of elements heavier than iron has long been uncertain. Theoretical modelling shows that the matter that is expelled in the violent merger of two neutron stars can assemble into heavy elements such as gold and platinum in a process known as rapid neutron capture (r-process) nucleosynthesis. The radioactive decay of isotopes of the heavy elements is predicted to power a distinctive thermal glow (a 'kilonova'). The discovery of an electromagnetic counterpart to the gravitational-wave source GW170817 represents the first opportunity to detect and scrutinize a sample of freshly synthesized r-process elements. Here we report models that predict the electromagnetic emission of kilonovae in detail and enable the mass, velocity and composition of ejecta to be derived from observations. We compare the models to the optical and infrared radiation associated with the GW170817 event to argue that the observed source is a kilonova. We infer the presence of two distinct components of ejecta, one composed primarily of light (atomic mass number less than 140) and one of heavy (atomic mass number greater than 140) r-process elements. The ejected mass and a merger rate inferred from GW170817 imply that such mergers are a dominant mode of r-process production in the Universe.
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Affiliation(s)
- Daniel Kasen
- Departments of Physics and Astronomy, and Theoretical Astrophysics Center, University of California, Berkeley, California 94720-7300, USA.,Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720-8169, USA
| | - Brian Metzger
- Department of Physics and Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA
| | - Jennifer Barnes
- Department of Physics and Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA
| | - Eliot Quataert
- Departments of Physics and Astronomy, and Theoretical Astrophysics Center, University of California, Berkeley, California 94720-7300, USA
| | - Enrico Ramirez-Ruiz
- Department of Astronomy, University of Santa Cruz, California, USA.,DARK, Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Denmark
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20
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Shappee BJ, Simon JD, Drout MR, Piro AL, Morrell N, Prieto JL, Kasen D, Holoien TWS, Kollmeier JA, Kelson DD, Coulter DA, Foley RJ, Kilpatrick CD, Siebert MR, Madore BF, Murguia-Berthier A, Pan YC, Prochaska JX, Ramirez-Ruiz E, Rest A, Adams C, Alatalo K, Bañados E, Baughman J, Bernstein RA, Bitsakis T, Boutsia K, Bravo JR, Di Mille F, Higgs CR, Ji AP, Maravelias G, Marshall JL, Placco VM, Prieto G, Wan Z. Early spectra of the gravitational wave source GW170817: Evolution of a neutron star merger. Science 2017; 358:1574-1578. [PMID: 29038374 DOI: 10.1126/science.aaq0186] [Citation(s) in RCA: 28] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/22/2017] [Accepted: 10/11/2017] [Indexed: 11/02/2022]
Abstract
On 17 August 2017, Swope Supernova Survey 2017a (SSS17a) was discovered as the optical counterpart of the binary neutron star gravitational wave event GW170817. We report time-series spectroscopy of SSS17a from 11.75 hours until 8.5 days after the merger. Over the first hour of observations, the ejecta rapidly expanded and cooled. Applying blackbody fits to the spectra, we measured the photosphere cooling from [Formula: see text] to [Formula: see text] kelvin, and determined a photospheric velocity of roughly 30% of the speed of light. The spectra of SSS17a began displaying broad features after 1.46 days and evolved qualitatively over each subsequent day, with distinct blue (early-time) and red (late-time) components. The late-time component is consistent with theoretical models of r-process-enriched neutron star ejecta, whereas the blue component requires high-velocity, lanthanide-free material.
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Affiliation(s)
- B J Shappee
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA. .,Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
| | - J D Simon
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - M R Drout
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - A L Piro
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - N Morrell
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
| | - J L Prieto
- Núcleo de Astronomía de la Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Avenida Ejército 441, Santiago, Chile.,Millennium Institute of Astrophysics, Santiago, Chile
| | - D Kasen
- Departments of Physics and Astronomy, 366 LeConte Hall, University of California---Berkeley, Berkeley, CA 94720, USA.,Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
| | - T W-S Holoien
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - J A Kollmeier
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - D D Kelson
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - D A Coulter
- Department of Astronomy and Astrophysics, University of California-Santa Cruz, Santa Cruz, CA 95064, USA
| | - R J Foley
- Department of Astronomy and Astrophysics, University of California-Santa Cruz, Santa Cruz, CA 95064, USA
| | - C D Kilpatrick
- Department of Astronomy and Astrophysics, University of California-Santa Cruz, Santa Cruz, CA 95064, USA
| | - M R Siebert
- Department of Astronomy and Astrophysics, University of California-Santa Cruz, Santa Cruz, CA 95064, USA
| | - B F Madore
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - A Murguia-Berthier
- Department of Astronomy and Astrophysics, University of California-Santa Cruz, Santa Cruz, CA 95064, USA
| | - Y-C Pan
- Department of Astronomy and Astrophysics, University of California-Santa Cruz, Santa Cruz, CA 95064, USA
| | - J X Prochaska
- Department of Astronomy and Astrophysics, University of California-Santa Cruz, Santa Cruz, CA 95064, USA
| | - E Ramirez-Ruiz
- Department of Astronomy and Astrophysics, University of California-Santa Cruz, Santa Cruz, CA 95064, USA.,Dark Cosmology Center, Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Denmark
| | - A Rest
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA.,Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA
| | - C Adams
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - K Alatalo
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA.,Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - E Bañados
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - J Baughman
- Núcleo de Astronomía de la Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Avenida Ejército 441, Santiago, Chile.,Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - R A Bernstein
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - T Bitsakis
- Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, C.P. 58190, Morelia, Mexico
| | - K Boutsia
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
| | - J R Bravo
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
| | - F Di Mille
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
| | - C R Higgs
- University of Victoria, Victoria, BC V8P 5C2, Canada.,National Research Council (NRC) Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
| | - A P Ji
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA.,Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA
| | - G Maravelias
- Instituto de Física y Astronomía, Universidad de Valparaíso, Valparaíso, Chile
| | - J L Marshall
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA
| | - V M Placco
- Department of Physics and Joint Institute for Nuclear Astrophysics (JINA) Center for the Evolution of the Elements, University of Notre Dame, Notre Dame, IN 46556, USA
| | - G Prieto
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
| | - Z Wan
- Sydney Institute for Astronomy, School of Physics, A28, University of Sydney, NSW 2006, Australia
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Drout MR, Piro AL, Shappee BJ, Kilpatrick CD, Simon JD, Contreras C, Coulter DA, Foley RJ, Siebert MR, Morrell N, Boutsia K, Di Mille F, Holoien TWS, Kasen D, Kollmeier JA, Madore BF, Monson AJ, Murguia-Berthier A, Pan YC, Prochaska JX, Ramirez-Ruiz E, Rest A, Adams C, Alatalo K, Bañados E, Baughman J, Beers TC, Bernstein RA, Bitsakis T, Campillay A, Hansen TT, Higgs CR, Ji AP, Maravelias G, Marshall JL, Bidin CM, Prieto JL, Rasmussen KC, Rojas-Bravo C, Strom AL, Ulloa N, Vargas-González J, Wan Z, Whitten DD. Light curves of the neutron star merger GW170817/SSS17a: Implications for r-process nucleosynthesis. Science 2017; 358:1570-1574. [PMID: 29038375 DOI: 10.1126/science.aaq0049] [Citation(s) in RCA: 384] [Impact Index Per Article: 54.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/20/2017] [Accepted: 10/11/2017] [Indexed: 11/02/2022]
Abstract
On 17 August 2017, gravitational waves (GWs) were detected from a binary neutron star merger, GW170817, along with a coincident short gamma-ray burst, GRB 170817A. An optical transient source, Swope Supernova Survey 17a (SSS17a), was subsequently identified as the counterpart of this event. We present ultraviolet, optical, and infrared light curves of SSS17a extending from 10.9 hours to 18 days postmerger. We constrain the radioactively powered transient resulting from the ejection of neutron-rich material. The fast rise of the light curves, subsequent decay, and rapid color evolution are consistent with multiple ejecta components of differing lanthanide abundance. The late-time light curve indicates that SSS17a produced at least ~0.05 solar masses of heavy elements, demonstrating that neutron star mergers play a role in rapid neutron capture (r-process) nucleosynthesis in the universe.
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Affiliation(s)
- M R Drout
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA.
| | - A L Piro
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - B J Shappee
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA.,Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
| | - C D Kilpatrick
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - J D Simon
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - C Contreras
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
| | - D A Coulter
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - R J Foley
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - M R Siebert
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - N Morrell
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
| | - K Boutsia
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
| | - F Di Mille
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
| | - T W-S Holoien
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - D Kasen
- Departments of Physics and Astronomy, 366 LeConte Hall, University of California, Berkeley, CA 94720, USA.,Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
| | - J A Kollmeier
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - B F Madore
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - A J Monson
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA.,Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA
| | - A Murguia-Berthier
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - Y-C Pan
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - J X Prochaska
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - E Ramirez-Ruiz
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA.,Dark Cosmology Center, Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Denmark
| | - A Rest
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA.,Department of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA
| | - C Adams
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
| | - K Alatalo
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA.,Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - E Bañados
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - J Baughman
- Massachusetts Institute of Technology, Cambridge, MA, USA.,Núcleo de Astronomía de la Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Avenida Ejército 441, Santiago, Chile
| | - T C Beers
- Department of Physics, University of Notre Dame, Notre Dame, IN 46556, USA.,Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, East Lansing, MI 48824, USA
| | - R A Bernstein
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - T Bitsakis
- Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, C.P. 58190, Morelia, Mexico
| | - A Campillay
- Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile
| | - T T Hansen
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - C R Higgs
- University of Victoria, Victoria, British Columbia, Canada.,National Research Council Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, British Columbia V9E 2E7, Canada
| | - A P Ji
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - G Maravelias
- Instituto de Física y Astronomía, Universidad de Valparaíso, Avenida Gran Bretaña 1111, Casilla 5030, Valparaíso, Chile
| | - J L Marshall
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA
| | - C Moni Bidin
- Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Antofagasta, Chile
| | - J L Prieto
- Núcleo de Astronomía de la Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Avenida Ejército 441, Santiago, Chile.,Millennium Institute of Astrophysics, Santiago, Chile
| | - K C Rasmussen
- Department of Physics, University of Notre Dame, Notre Dame, IN 46556, USA.,Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, East Lansing, MI 48824, USA
| | - C Rojas-Bravo
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - A L Strom
- The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - N Ulloa
- Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile
| | - J Vargas-González
- Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
| | - Z Wan
- Sydney Institute for Astronomy, School of Physics, A28, University of Sydney, NSW 2006, Australia
| | - D D Whitten
- Department of Physics, University of Notre Dame, Notre Dame, IN 46556, USA.,Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, East Lansing, MI 48824, USA
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22
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The Unprecedented Properties of the First Electromagnetic Counterpart to a Gravitational-wave Source. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/2041-8213/aa905e] [Citation(s) in RCA: 27] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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23
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Coulter DA, Foley RJ, Kilpatrick CD, Drout MR, Piro AL, Shappee BJ, Siebert MR, Simon JD, Ulloa N, Kasen D, Madore BF, Murguia-Berthier A, Pan YC, Prochaska JX, Ramirez-Ruiz E, Rest A, Rojas-Bravo C. Swope Supernova Survey 2017a (SSS17a), the optical counterpart to a gravitational wave source. Science 2017; 358:1556-1558. [PMID: 29038368 DOI: 10.1126/science.aap9811] [Citation(s) in RCA: 104] [Impact Index Per Article: 14.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/16/2017] [Accepted: 10/10/2017] [Indexed: 11/02/2022]
Abstract
On 17 August 2017, the Laser Interferometer Gravitational-Wave Observatory (LIGO) and the Virgo interferometer detected gravitational waves (GWs) emanating from a binary neutron star merger, GW170817. Nearly simultaneously, the Fermi and INTEGRAL (INTErnational Gamma-Ray Astrophysics Laboratory) telescopes detected a gamma-ray transient, GRB 170817A. At 10.9 hours after the GW trigger, we discovered a transient and fading optical source, Swope Supernova Survey 2017a (SSS17a), coincident with GW170817. SSS17a is located in NGC 4993, an S0 galaxy at a distance of 40 megaparsecs. The precise location of GW170817 provides an opportunity to probe the nature of these cataclysmic events by combining electromagnetic and GW observations.
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Affiliation(s)
- D A Coulter
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA.
| | - R J Foley
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - C D Kilpatrick
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - M R Drout
- Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - A L Piro
- Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - B J Shappee
- Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA.,Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
| | - M R Siebert
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - J D Simon
- Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA
| | - N Ulloa
- Departamento de Física y Astronomía, Universidad de La Serena, La Serena, Chile
| | - D Kasen
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA.,Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA
| | - B F Madore
- Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA.,Department of Astronomy and Astrophysics, The University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA
| | - A Murguia-Berthier
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - Y-C Pan
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - J X Prochaska
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - E Ramirez-Ruiz
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA.,Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Denmark
| | - A Rest
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA.,Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA
| | - C Rojas-Bravo
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
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