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Aumann T, Bertulani CA, Duer M, Galatyuk T, Obertelli A, Panin V, Rodríguez-Sánchez JL, Roth R, Stroth J. Nuclear structure opportunities with GeV radioactive beams at FAIR. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2024; 382:20230121. [PMID: 38910400 DOI: 10.1098/rsta.2023.0121] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/19/2023] [Accepted: 04/10/2024] [Indexed: 06/25/2024]
Abstract
The Facility for Antiproton and Ion Research (FAIR) is in its final construction stage next to the campus of the Gesellschaft für Schwerionenforschung Helmholtzzentrum for heavy-ion research in Darmstadt, Germany. Once it starts its operation, it will be the main nuclear physics research facility in many basic sciences and their applications in Europe for the coming decades. Owing to the ability of the new fragment separator, Super-FRagment Separator, to produce high-intensity radioactive ion beams in the energy range up to about 2 GeV/nucleon, these can be used in various nuclear reactions. This opens a unique opportunity for various nuclear structure studies across a range of fields and scales: from low-energy physics via the investigation of multi-neutron systems and halos to high-density nuclear matter and the equation of state, following heavy-ion collisions, fission and study of short-range correlations in nuclei and hypernuclei. The newly developed reactions with relativistic radioactive beams (R3B) set up at FAIR would be the most suitable and versatile for such studies. An overview of highlighted physics cases foreseen at R3B is given, along with possible future opportunities, at FAIR. This article is part of the theme issue 'The liminal position of Nuclear Physics: from hadrons to neutron stars'.
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Affiliation(s)
- T Aumann
- Institut für Kernphysik, Technische Universität Darmstadt , Darmstadt 64289, Germany
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Planckstraße 1 , Darmstadt 64291, Germany
- Helmholtz Forschungsakademie Hessen für FAIR (HFHF) , Darmstadt 64291, Germany
| | - C A Bertulani
- Helmholtz Forschungsakademie Hessen für FAIR (HFHF) , Darmstadt 64291, Germany
- Texas A&M University-Commerce , Commerce, TX 75429, USA
| | - M Duer
- Institut für Kernphysik, Technische Universität Darmstadt , Darmstadt 64289, Germany
| | - T Galatyuk
- Institut für Kernphysik, Technische Universität Darmstadt , Darmstadt 64289, Germany
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Planckstraße 1 , Darmstadt 64291, Germany
- Helmholtz Forschungsakademie Hessen für FAIR (HFHF) , Darmstadt 64291, Germany
| | - A Obertelli
- Institut für Kernphysik, Technische Universität Darmstadt , Darmstadt 64289, Germany
- Helmholtz Forschungsakademie Hessen für FAIR (HFHF) , Darmstadt 64291, Germany
| | - V Panin
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Planckstraße 1 , Darmstadt 64291, Germany
| | | | - R Roth
- Institut für Kernphysik, Technische Universität Darmstadt , Darmstadt 64289, Germany
- Helmholtz Forschungsakademie Hessen für FAIR (HFHF) , Darmstadt 64291, Germany
| | - J Stroth
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Planckstraße 1 , Darmstadt 64291, Germany
- Helmholtz Forschungsakademie Hessen für FAIR (HFHF) , Darmstadt 64291, Germany
- Institut für Kernphysik, Johann Wolfgang Goethe-Universität , Frankfurt 60438, Germany
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2
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Chaudhary SS, Toivonen A, Waratkar G, Mo G, Chatterjee D, Antier S, Brockill P, Coughlin MW, Essick R, Ghosh S, Morisaki S, Baral P, Baylor A, Adhikari N, Brady P, Cabourn Davies G, Dal Canton T, Cavaglia M, Creighton J, Choudhary S, Chu YK, Clearwater P, Davis L, Dent T, Drago M, Ewing B, Godwin P, Guo W, Hanna C, Huxford R, Harry I, Katsavounidis E, Kovalam M, Li AK, Magee R, Marx E, Meacher D, Messick C, Morice-Atkinson X, Pace A, De Pietri R, Piotrzkowski B, Roy S, Sachdev S, Singer LP, Singh D, Szczepanczyk M, Tang D, Trevor M, Tsukada L, Villa-Ortega V, Wen L, Wysocki D. Low-latency gravitational wave alert products and their performance at the time of the fourth LIGO-Virgo-KAGRA observing run. Proc Natl Acad Sci U S A 2024; 121:e2316474121. [PMID: 38652749 PMCID: PMC11067028 DOI: 10.1073/pnas.2316474121] [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: 09/25/2023] [Accepted: 03/16/2024] [Indexed: 04/25/2024] Open
Abstract
Multimessenger searches for binary neutron star (BNS) and neutron star-black hole (NSBH) mergers are currently one of the most exciting areas of astronomy. The search for joint electromagnetic and neutrino counterparts to gravitational wave (GW)s has resumed with ALIGO's, AdVirgo's and KAGRA's fourth observing run (O4). To support this effort, public semiautomated data products are sent in near real-time and include localization and source properties to guide complementary observations. In preparation for O4, we have conducted a study using a simulated population of compact binaries and a mock data challenge (MDC) in the form of a real-time replay to optimize and profile the software infrastructure and scientific deliverables. End-toend performance was tested, including data ingestion, running online search pipelines, performing annotations, and issuing alerts to the astrophysics community. We present an overview of the low-latency infrastructure and the performance of the data products that are now being released during O4 based on the MDC. We report the expected median latency for the preliminary alert of full bandwidth searches (29.5 s) and show consistency and accuracy of released data products using the MDC. We report the expected median latency for triggers from early warning searches (-3.1 s), which are new in O4 and target neutron star mergers during inspiral phase. This paper provides a performance overview for LIGO-Virgo-KAGRA (LVK) low-latency alert infrastructure and data products using theMDCand serves as a useful reference for the interpretation of O4 detections.
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Affiliation(s)
- Sushant Sharma Chaudhary
- Institute of Multi-messenger Astrophysics and Cosmology, Missouri University of Science and Technology, Rolla, MO65409
| | - Andrew Toivonen
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN55455
| | | | - Geoffrey Mo
- MIT Kavli Institute for Astrophysics, Massachusetts Institute of Technology, Cambridge, MA02139
- MIT Laser Interferometer Gravitational-Wave Observatory Laboratory, Massachusetts Institute of Technology, Cambridge, MA02139
| | - Deep Chatterjee
- MIT Kavli Institute for Astrophysics, Massachusetts Institute of Technology, Cambridge, MA02139
- MIT Laser Interferometer Gravitational-Wave Observatory Laboratory, Massachusetts Institute of Technology, Cambridge, MA02139
| | - Sarah Antier
- Artemis, Observatoire de la Côte d’Azur, Université Côte d’Azur, Nice06304, France
| | - Patrick Brockill
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Michael W. Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN55455
| | - Reed Essick
- Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ONM5S 3H8, Canada
- Department of Physics, University of Toronto, Toronto, ONM5S 1A7, Canada
- David A. Dunlap Department of Astronomy, University of Toronto, Toronto, ONM5S 3H4, Canada
| | - Shaon Ghosh
- Department of Physics and Astronomy, Montclair State University, NJ07043
| | - Soichiro Morisaki
- Institute for Cosmic Ray Research, The University of Tokyo, Chiba277-8582, Japan
| | - Pratyusava Baral
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Amanda Baylor
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Naresh Adhikari
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Patrick Brady
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | | | - Tito Dal Canton
- Université Paris-Saclay, CNRS/IN2P3, IJCLab, Orsay91405, France
| | - Marco Cavaglia
- Institute of Multi-messenger Astrophysics and Cosmology, Missouri University of Science and Technology, Rolla, MO65409
| | | | - Sunil Choudhary
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Yu-Kuang Chu
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Patrick Clearwater
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Luke Davis
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Thomas Dent
- Instituto Galego de Física de Altas Enerxías, Universidade de Santiago de Compostela, 15705Santiago de Compostela, Spain
| | - Marco Drago
- Universitá di Roma La Sapienza and INFN, Sezione di Roma, RomaI-00133, Italy
| | - Becca Ewing
- Department of Physics, The Pennsylvania State University, University Park, PA16802
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
| | - Patrick Godwin
- Laser Interferometer Gravitational-Wave Observatory (LIGO) Laboratory, California Institute of Technology, Pasadena, CA91125
| | - Weichangfeng Guo
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Chad Hanna
- Department of Physics, The Pennsylvania State University, University Park, PA16802
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA16802
- Institute for Computational and Data Sciences, The Pennsylvania State University, University Park, PA16802
| | - Rachael Huxford
- Department of Physics, The Pennsylvania State University, University Park, PA16802
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
| | - Ian Harry
- University of Portsmouth, PortsmouthPO1 3FX, United Kingdom
| | - Erik Katsavounidis
- MIT Kavli Institute for Astrophysics, Massachusetts Institute of Technology, Cambridge, MA02139
- MIT Laser Interferometer Gravitational-Wave Observatory Laboratory, Massachusetts Institute of Technology, Cambridge, MA02139
| | - Manoj Kovalam
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Alvin K.Y. Li
- Laser Interferometer Gravitational-Wave Observatory (LIGO) Laboratory, California Institute of Technology, Pasadena, CA91125
| | - Ryan Magee
- Laser Interferometer Gravitational-Wave Observatory (LIGO) Laboratory, California Institute of Technology, Pasadena, CA91125
| | - Ethan Marx
- MIT Kavli Institute for Astrophysics, Massachusetts Institute of Technology, Cambridge, MA02139
- MIT Laser Interferometer Gravitational-Wave Observatory Laboratory, Massachusetts Institute of Technology, Cambridge, MA02139
| | - Duncan Meacher
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Cody Messick
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | | | - Alexander Pace
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
| | - Roberto De Pietri
- Dipartimento di Scienze Matematiche, Fisiche e Informatiche, Universitá di Parma, ParmaI-43124, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Milano Bicocca, Gruppo Collegato di Parma, ParmaI-43124, Italy
| | - Brandon Piotrzkowski
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
| | - Soumen Roy
- Nikhef, Amsterdam1098 XG, The Netherlands
- Institute for Gravitational and Subatomic Physics, Utrecht University, Utrecht3584 CC, The Netherlands
| | - Surabhi Sachdev
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
- School of Physics, Georgia Institute of Technology, Atlanta, GW30332
| | - Leo P. Singer
- Astrophysics Science Division, NASA Goddard Space Flight Center, Code 661, Greenbelt, MD20771
- Joint Space-Science Institute, University of Maryland, College Park, MD20742
| | - Divya Singh
- Department of Physics, The Pennsylvania State University, University Park, PA16802
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
| | | | - Daniel Tang
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Max Trevor
- Department of Physics, University of Maryland, College Park, MD20742
| | - Leo Tsukada
- Department of Physics, The Pennsylvania State University, University Park, PA16802
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA16802
| | - Verónica Villa-Ortega
- Instituto Galego de Física de Altas Enerxías, Universidade de Santiago de Compostela, 15705Santiago de Compostela, Spain
| | - Linqing Wen
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery, HawthornVIC3122, Australia
- Department of Physics, University of Western Australia, CrawleyWA6009, Australia
| | - Daniel Wysocki
- Leonard E. Parker Center for Gravitation, Cosmology, and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee, WI53201
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3
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Blanchard PK, Villar VA, Chornock R, Laskar T, Li Y, Leja J, Pierel J, Berger E, Margutti R, Alexander KD, Barnes J, Cendes Y, Eftekhari T, Kasen D, LeBaron N, Metzger BD, Muzerolle Page J, Rest A, Sears H, Siegel DM, Yadavalli SK. JWST detection of a supernova associated with GRB 221009A without an r-process signature. NATURE ASTRONOMY 2024; 8:774-785. [PMID: 38912294 PMCID: PMC11189819 DOI: 10.1038/s41550-024-02237-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 08/26/2023] [Accepted: 03/05/2024] [Indexed: 06/25/2024]
Abstract
Identifying the sites of r-process nucleosynthesis, a primary mechanism of heavy element production, is a key goal of astrophysics. The discovery of the brightest gamma-ray burst (GRB) to date, GRB 221009A, presented an opportunity to spectroscopically test the idea that r-process elements are produced following the collapse of rapidly rotating massive stars. Here we present James Webb Space Telescope observations of GRB 221009A obtained +168 and +170 rest-frame days after the gamma-ray trigger, and demonstrate that they are well described by a SN 1998bw-like supernova (SN) and power-law afterglow, with no evidence for a component from r-process emission. The SN, with a nickel mass of approximately 0.09 M ⊙, is only slightly fainter than the brightness of SN 1998bw at this phase, which indicates that the SN is not an unusual GRB-SN. This demonstrates that the GRB and SN mechanisms are decoupled and that highly energetic GRBs are not likely to produce significant quantities of r-process material, which leaves open the question of whether explosions of massive stars are key sources of r-process elements. Moreover, the host galaxy of GRB 221009A has a very low metallicity of approximately 0.12 Z ⊙ and strong H2 emission at the explosion site, which is consistent with recent star formation, hinting that environmental factors are responsible for its extreme energetics.
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Affiliation(s)
- Peter K. Blanchard
- Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL USA
| | - V. Ashley Villar
- Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA USA
| | - Ryan Chornock
- Department of Astronomy, University of California, Berkeley, CA USA
| | - Tanmoy Laskar
- Department of Physics & Astronomy, University of Utah, Salt Lake City, UT USA
- Department of Astrophysics/IMAPP, Radboud University, Nijmegen, The Netherlands
| | - Yijia Li
- Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA USA
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA USA
| | - Joel Leja
- Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA USA
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA USA
- Institute for Computational & Data Sciences, The Pennsylvania State University, University Park, PA USA
| | - Justin Pierel
- Space Telescope Science Institute, Baltimore, MD USA
| | - Edo Berger
- Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA USA
| | - Raffaella Margutti
- Department of Astronomy, University of California, Berkeley, CA USA
- Department of Physics, University of California, Berkeley, CA USA
| | | | - Jennifer Barnes
- Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA USA
| | - Yvette Cendes
- Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA USA
| | - Tarraneh Eftekhari
- Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL USA
| | - Daniel Kasen
- Department of Physics, University of California, Berkeley, CA USA
| | - Natalie LeBaron
- Department of Astronomy, University of California, Berkeley, CA USA
| | - Brian D. Metzger
- Department of Physics and Columbia Astrophysics Laboratory, Columbia University, New York, NY USA
- Center for Computational Astrophysics, Flatiron Institute, New York, NY USA
| | | | - Armin Rest
- Space Telescope Science Institute, Baltimore, MD USA
| | - Huei Sears
- Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL USA
- Department of Physics and Astronomy, Northwestern University, Evanston, IL USA
| | - Daniel M. Siegel
- Institute of Physics, University of Greifswald, Greifswald, Germany
- Department of Physics, University of Guelph, Guelph, Ontario Canada
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4
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Vassh N, Wang X, Larivière M, Sprouse T, Mumpower MR, Surman R, Liu Z, McLaughlin GC, Denissenkov P, Herwig F. Thallium-208: A Beacon of In Situ Neutron Capture Nucleosynthesis. PHYSICAL REVIEW LETTERS 2024; 132:052701. [PMID: 38364162 DOI: 10.1103/physrevlett.132.052701] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/30/2023] [Revised: 10/30/2023] [Accepted: 11/15/2023] [Indexed: 02/18/2024]
Abstract
We demonstrate that the well-known 2.6 MeV gamma-ray emission line from thallium-208 could serve as a real-time indicator of astrophysical heavy element production, with both rapid (r) and intermediate (i) neutron capture processes capable of its synthesis. We consider the r process in a Galactic neutron star merger and show Tl-208 to be detectable from ∼12 hours to ∼ten days, and again ∼1-20 years postevent. Detection of Tl-208 represents the only identified prospect for a direct signal of lead production (implying gold synthesis), arguing for the importance of future MeV telescope missions which aim to detect Galactic events but may also be able to reach some nearby galaxies in the Local Group.
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Affiliation(s)
- Nicole Vassh
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - Xilu Wang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, People's Republic of China
| | - Maude Larivière
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia V6T 1Z1, Canada
| | - Trevor Sprouse
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - Matthew R Mumpower
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - Rebecca Surman
- Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - Zhenghai Liu
- Department of Physics, North Carolina State University, Raleigh, North Carolina 27695, USA
| | - Gail C McLaughlin
- Department of Physics, North Carolina State University, Raleigh, North Carolina 27695, USA
| | - Pavel Denissenkov
- Department of Physics and Astronomy, University of Victoria, Victoria, British Columbia V8W 2Y2, Canada
- CaNPAN (Canadian Nuclear Physics for Astrophysics Network) Collaboration
- NuGrid Collaboration
| | - Falk Herwig
- Department of Physics and Astronomy, University of Victoria, Victoria, British Columbia V8W 2Y2, Canada
- CaNPAN (Canadian Nuclear Physics for Astrophysics Network) Collaboration
- NuGrid Collaboration
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5
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Ho AYQ, Perley DA, Chen P, Schulze S, Dhillon V, Kumar H, Suresh A, Swain V, Bremer M, Smartt SJ, Anderson JP, Anupama GC, Awiphan S, Barway S, Bellm EC, Ben-Ami S, Bhalerao V, de Boer T, Brink TG, Burruss R, Chandra P, Chen TW, Chen WP, Cooke J, Coughlin MW, Das KK, Drake AJ, Filippenko AV, Freeburn J, Fremling C, Fulton MD, Gal-Yam A, Galbany L, Gao H, Graham MJ, Gromadzki M, Gutiérrez CP, Hinds KR, Inserra C, A J N, Karambelkar V, Kasliwal MM, Kulkarni S, Müller-Bravo TE, Magnier EA, Mahabal AA, Moore T, Ngeow CC, Nicholl M, Ofek EO, Omand CMB, Onori F, Pan YC, Pessi PJ, Petitpas G, Polishook D, Poshyachinda S, Pursiainen M, Riddle R, Rodriguez AC, Rusholme B, Segre E, Sharma Y, Smith KW, Sollerman J, Srivastav S, Strotjohann NL, Suhr M, Svinkin D, Wang Y, Wiseman P, Wold A, Yang S, Yang Y, Yao Y, Young DR, Zheng W. Minutes-duration optical flares with supernova luminosities. Nature 2023; 623:927-931. [PMID: 37968403 DOI: 10.1038/s41586-023-06673-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/26/2023] [Accepted: 09/25/2023] [Indexed: 11/17/2023]
Abstract
In recent years, certain luminous extragalactic optical transients have been observed to last only a few days1. Their short observed duration implies a different powering mechanism from the most common luminous extragalactic transients (supernovae), whose timescale is weeks2. Some short-duration transients, most notably AT2018cow (ref. 3), show blue optical colours and bright radio and X-ray emission4. Several AT2018cow-like transients have shown hints of a long-lived embedded energy source5, such as X-ray variability6,7, prolonged ultraviolet emission8, a tentative X-ray quasiperiodic oscillation9,10 and large energies coupled to fast (but subrelativistic) radio-emitting ejecta11,12. Here we report observations of minutes-duration optical flares in the aftermath of an AT2018cow-like transient, AT2022tsd (the 'Tasmanian Devil'). The flares occur over a period of months, are highly energetic and are probably nonthermal, implying that they arise from a near-relativistic outflow or jet. Our observations confirm that, in some AT2018cow-like transients, the embedded energy source is a compact object, either a magnetar or an accreting black hole.
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Affiliation(s)
- Anna Y Q Ho
- Department of Astronomy, Cornell University, Ithaca, NY, USA.
| | - Daniel A Perley
- Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK
| | - Ping Chen
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Steve Schulze
- The Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, Stockholm, Sweden
| | - Vik Dhillon
- Department of Physics and Astronomy, University of Sheffield, Sheffield, UK
- Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain
| | - Harsh Kumar
- Indian Institute of Technology Bombay, Powai, Mumbai, India
| | - Aswin Suresh
- Indian Institute of Technology Bombay, Powai, Mumbai, India
| | | | - Michael Bremer
- Institut de Radioastronomie Millimétrique (IRAM), Saint-Martin-d'Hères, France
| | - Stephen J Smartt
- Department of Physics, University of Oxford, Oxford, UK
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, UK
| | - Joseph P Anderson
- European Southern Observatory, Santiago, Chile
- Millennium Institute of Astrophysics (MAS), Santiago, Chile
| | - G C Anupama
- Indian Institute of Astrophysics, Bengaluru, India
| | - Supachai Awiphan
- National Astronomical Research Institute of Thailand, Chiang Mai, Thailand
| | | | - Eric C Bellm
- DiRAC Institute, Department of Astronomy, University of Washington, Seattle, WA, USA
| | - Sagi Ben-Ami
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Varun Bhalerao
- Indian Institute of Technology Bombay, Powai, Mumbai, India
| | - Thomas de Boer
- Institute for Astronomy, University of Hawai'i, Honolulu, HI, USA
| | - Thomas G Brink
- Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA
| | - Rick Burruss
- Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA
| | - Poonam Chandra
- National Radio Astronomy Observatory, Charlottesville, VA, USA
| | - Ting-Wan Chen
- Physik-Department, TUM School of Natural Sciences, Technische Universität München, Garching, Germany
- Max-Planck-Institut für Astrophysik, Garching, Germany
| | - Wen-Ping Chen
- Graduate Institute of Astronomy, National Central University, Taoyuan, Taiwan
| | - Jeff Cooke
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, Australia
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), Hawthorn, Victoria, Australia
- Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Stromlo, Australian Capital Territory, Australia
| | - Michael W Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | - Kaustav K Das
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Andrew J Drake
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Alexei V Filippenko
- Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA
| | - James Freeburn
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, Australia
- Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), Hawthorn, Victoria, Australia
| | - Christoffer Fremling
- Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Michael D Fulton
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, UK
| | - Avishay Gal-Yam
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Lluís Galbany
- Institute of Space Sciences (ICE-CSIC), Barcelona, Spain
- Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain
| | - Hua Gao
- Institute for Astronomy, University of Hawai'i, Honolulu, HI, USA
| | - Matthew J Graham
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | | | - Claudia P Gutiérrez
- Institute of Space Sciences (ICE-CSIC), Barcelona, Spain
- Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain
| | - K-Ryan Hinds
- Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK
| | - Cosimo Inserra
- Cardiff Hub for Astrophysics Research and Technology, School of Physics & Astronomy, Cardiff University, Cardiff, UK
| | - Nayana A J
- Indian Institute of Astrophysics, Bengaluru, India
| | - Viraj Karambelkar
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Mansi M Kasliwal
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Shri Kulkarni
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Tomás E Müller-Bravo
- Institute of Space Sciences (ICE-CSIC), Barcelona, Spain
- Institut d'Estudis Espacials de Catalunya (IEEC), Barcelona, Spain
| | - Eugene A Magnier
- Institute for Astronomy, University of Hawai'i, Honolulu, HI, USA
| | - Ashish A Mahabal
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
- Center for Data-Driven Discovery, California Institute of Technology, Pasadena, CA, USA
| | - Thomas Moore
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, UK
| | - Chow-Choong Ngeow
- Graduate Institute of Astronomy, National Central University, Taoyuan, Taiwan
| | - Matt Nicholl
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, UK
| | - Eran O Ofek
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Conor M B Omand
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, Albanova University Center, Stockholm, Sweden
| | | | - Yen-Chen Pan
- Graduate Institute of Astronomy, National Central University, Taoyuan, Taiwan
| | - Priscila J Pessi
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, Albanova University Center, Stockholm, Sweden
| | - Glen Petitpas
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
| | - David Polishook
- Faculty of Physics, Weizmann Institute of Science, Rehovot, Israel
| | - Saran Poshyachinda
- National Astronomical Research Institute of Thailand, Chiang Mai, Thailand
| | - Miika Pursiainen
- DTU Space, National Space Institute, Technical University of Denmark, Kongens Lyngby, Denmark
| | - Reed Riddle
- Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA
| | - Antonio C Rodriguez
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Ben Rusholme
- Infrared Processing and Analysis Center (IPAC), California Institute of Technology, Pasadena, CA, USA
| | - Enrico Segre
- Physics Core Facilities, Weizmann Institute of Science, Rehovot, Israel
| | - Yashvi Sharma
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Ken W Smith
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, UK
| | - Jesper Sollerman
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, Albanova University Center, Stockholm, Sweden
| | - Shubham Srivastav
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, UK
| | - Nora Linn Strotjohann
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Mark Suhr
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, Australia
- Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Stromlo, Australian Capital Territory, Australia
| | | | - Yanan Wang
- Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- School of Physics and Astronomy, University of Southampton, Southampton, UK
| | - Philip Wiseman
- School of Physics and Astronomy, University of Southampton, Southampton, UK
| | - Avery Wold
- Infrared Processing and Analysis Center (IPAC), California Institute of Technology, Pasadena, CA, USA
| | - Sheng Yang
- Henan Academy of Sciences, Zhengzhou, China
| | - Yi Yang
- Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA
| | - Yuhan Yao
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - David R Young
- Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast, UK
| | - WeiKang Zheng
- Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA
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6
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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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7
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Most ER, Philippov AA. Reconnection-Powered Fast Radio Transients from Coalescing Neutron Star Binaries. PHYSICAL REVIEW LETTERS 2023; 130:245201. [PMID: 37390415 DOI: 10.1103/physrevlett.130.245201] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/28/2022] [Revised: 02/28/2023] [Accepted: 04/17/2023] [Indexed: 07/02/2023]
Abstract
It is an open question whether and how gravitational wave events involving neutron stars can be preceded by electromagnetic counterparts. This Letter shows that the collision of two neutron stars with magnetic fields well below magnetar-level strengths can produce millisecond fast-radio-burst-like transients. Using global force-free electrodynamics simulations, we identify the coherent emission mechanism that might operate in the common magnetosphere of a binary neutron star system prior to merger. We predict that the emission show have frequencies in the range of 10-20 GHz for magnetic fields of B^{*}=10^{11} G at the surfaces of the stars.
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Affiliation(s)
- Elias R Most
- Princeton Center for Theoretical Science, Princeton University, Princeton, New Jersey 08544, USA
- Princeton Gravity Initiative, Princeton University, Princeton, New Jersey 08544, USA
- School of Natural Sciences, Institute for Advanced Study, Princeton, New Jersey 08540, USA
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8
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A very luminous jet from the disruption of a star by a massive black hole. Nature 2022; 612:430-434. [PMID: 36450988 DOI: 10.1038/s41586-022-05465-8] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/05/2022] [Accepted: 10/19/2022] [Indexed: 12/02/2022]
Abstract
Tidal disruption events (TDEs) are bursts of electromagnetic energy that are released when supermassive black holes at the centres of galaxies violently disrupt a star that passes too close1. TDEs provide a window through which to study accretion onto supermassive black holes; in some rare cases, this accretion leads to launching of a relativistic jet2-9, but the necessary conditions are not fully understood. The best-studied jetted TDE so far is Swift J1644+57, which was discovered in γ-rays, but was too obscured by dust to be seen at optical wavelengths. Here we report the optical detection of AT2022cmc, a rapidly fading source at cosmological distance (redshift z = 1.19325) the unique light curve of which transitioned into a luminous plateau within days. Observations of a bright counterpart at other wavelengths, including X-ray, submillimetre and radio, supports the interpretation of AT2022cmc as a jetted TDE containing a synchrotron 'afterglow', probably launched by a supermassive black hole with spin greater than approximately 0.3. Using four years of Zwicky Transient Facility10 survey data, we calculate a rate of [Formula: see text] per gigapascals cubed per year for on-axis jetted TDEs on the basis of the luminous, fast-fading red component, thus providing a measurement complementary to the rates derived from X-ray and radio observations11. Correcting for the beaming angle effects, this rate confirms that approximately 1 per cent of TDEs have relativistic jets. Optical surveys can use AT2022cmc as a prototype to unveil a population of jetted TDEs.
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9
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A kilonova following a long-duration gamma-ray burst at 350 Mpc. Nature 2022; 612:223-227. [PMID: 36477128 DOI: 10.1038/s41586-022-05390-w] [Citation(s) in RCA: 8] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/22/2022] [Accepted: 09/27/2022] [Indexed: 12/12/2022]
Abstract
Gamma-ray bursts (GRBs) are divided into two populations1,2; long GRBs that derive from the core collapse of massive stars (for example, ref. 3) and short GRBs that form in the merger of two compact objects4,5. Although it is common to divide the two populations at a gamma-ray duration of 2 s, classification based on duration does not always map to the progenitor. Notably, GRBs with short (≲2 s) spikes of prompt gamma-ray emission followed by prolonged, spectrally softer extended emission (EE-SGRBs) have been suggested to arise from compact object mergers6-8. Compact object mergers are of great astrophysical importance as the only confirmed site of rapid neutron capture (r-process) nucleosynthesis, observed in the form of so-called kilonovae9-14. Here we report the discovery of a possible kilonova associated with the nearby (350 Mpc), minute-duration GRB 211211A. The kilonova implies that the progenitor is a compact object merger, suggesting that GRBs with long, complex light curves can be spawned from merger events. The kilonova of GRB 211211A has a similar luminosity, duration and colour to that which accompanied the gravitational wave (GW)-detected binary neutron star (BNS) merger GW170817 (ref. 4). Further searches for GW signals coincident with long GRBs are a promising route for future multi-messenger astronomy.
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10
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Ujevic M, Rashti A, Gieg H, Tichy W, Dietrich T. High-accuracy high-mass-ratio simulations for binary neutron stars and their comparison to existing waveform models. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.023029] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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11
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Thinking Outside the Box: Numerical Relativity with Particles. Symmetry (Basel) 2022. [DOI: 10.3390/sym14061280] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022] Open
Abstract
The observation of gravitational waves from compact objects has now become an active part of observational astronomy. For a sound interpretation, one needs to compare such observations against detailed Numerical Relativity simulations, which are essential tools to explore the dynamics and physics of compact binary mergers. To date, essentially all simulation codes that solve the full set of Einstein’s equations are performed in the framework of Eulerian hydrodynamics. The exception is our recently developed Numerical Relativity code SPHINCS_BSSN which solves the commonly used BSSN formulation of the Einstein equations on a structured mesh and the matter equations via Lagrangian particles. We show here, for the first time, SPHINCS_BSSN neutron star merger simulations with piecewise polytropic approximations to four nuclear matter equations of state. In this set of neutron star merger simulations, we focus on perfectly symmetric binary systems that are irrotational and have 1.3 M⊙ masses. We introduce some further methodological refinements (a new way of steering dissipation, an improved particle–mesh mapping), and we explore the impact of the exponent that enters in the calculation of the thermal pressure contribution. We find that it leaves a noticeable imprint on the gravitational wave amplitude (calculated via both quadrupole approximation and the Ψ4 formalism) and has a noticeable impact on the amount of dynamic ejecta. Consistent with earlier findings, we only find a few times 10−3M⊙ as dynamic ejecta in the studied equal mass binary systems, with softer equations of state (which are more prone to shock formation) ejecting larger amounts of matter. In all of the cases, we see a credible high-velocity (∼0.5…0.7c) ejecta component of ∼10−4M⊙ that is launched at contact from the interface between the two neutron stars. Such a high-velocity component has been suggested to produce an early, blue precursor to the main kilonova emission, and it could also potentially cause a kilonova afterglow.
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12
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Abstract
In recent years, shell model studies have significantly contributed in improving the nuclear input, required in simulations of the dynamics of astrophysical objects and their associated nucleosynthesis. This review highlights a few examples such as electron capture rates and neutrino-nucleus cross sections, important for the evolution and nucleosynthesis of supernovae. For simulations of rapid neutron-capture (r-process) nucleosynthesis, shell model studies have contributed to an improved understanding of half lives of neutron-rich nuclei with magic neutron numbers and of the nuclear level densities and γ-strength functions that are both relevant for neutron capture rates.
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13
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Abstract
The neutron star properties are generally determined by the equation of state of β-equilibrated dense matter. In this work, we consider the interaction of fermionic dark matter (DM) particles with nucleons via Higgs exchange and investigate the effect on the neutron star properties with the relativistic mean-field model equation of state coupled with DM. We deduce that DM significantly affects the neutron star properties, such as considerably reducing the maximum mass of the star, which depends on the percentage of the DM considered inside the neutron star. The tidal Love numbers both for electric and magnetic cases and surficial Love numbers are also studied for DM admixed NS. We observed that the magnitude of tidal and surficial Love numbers increases with a greater DM percentage. Further, we present post-Newtonian tidal corrections to gravitational waves decreased by increasing the DM percentage. The DM effect on the GW signal is significant during the late inspiral and merger stages of binary evolution for GW frequencies >500 Hz.
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14
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Probing Gamma-Ray Burst VHE Emission with the Southern Wide-Field-of-View Gamma-Ray Observatory. GALAXIES 2021. [DOI: 10.3390/galaxies9040098] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
Recent observations have confirmed that Gamma-Ray Burst (GRB) afterglows produce Very High-Energy radiation (VHE, E>100GeV). This highly anticipated discovery opens new scenarios in the interpretation of GRBs and in their role as probes of Extragalactic Background Light (EBL) and Lorentz Invariance Violation (LIV). However, some fundamental questions about the actual nature of VHE emission in GRBs and its evolution during the burst are still unsolved. These questions will be difficult to address, even with future imaging Cherenkov telescopes, such as the Cherenkov Telescope Array (CTA). Here we investigate the prospects of gamma-ray sky monitoring with Extensive Air Showers arrays (EAS) to address these problems. We discuss the theoretical aspects connected with VHE radiation emission and the implications that its temporal evolution properties have on the interpretation of GRBs. By revisiting the high-energy properties of some Fermi-LAT detected GRBs, we estimate the typical fluxes expected in the VHE band and compare them with a range of foreseeable instrument performances, based on the Southern Wide Field-of-view Gamma-ray Observatory concept (SWGO). We focus our analysis on how different instrument capabilities affect the chances to explore the burst onset and early evolution in VHE, providing invaluable complementary information with respect to Cherenkov telescope observations. We show that under the assumption of conditions already observed in historical events, the next-generation ground monitoring detectors can actually contribute to answer several key questions.
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15
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Abstract
A neutron star was first detected as a pulsar in 1967. It is one of the most mysterious compact objects in the universe, with a radius of the order of 10 km and masses that can reach two solar masses. In fact, neutron stars are star remnants, a kind of stellar zombie (they die, but do not disappear). In the last decades, astronomical observations yielded various contraints for neutron star masses, and finally, in 2017, a gravitational wave was detected (GW170817). Its source was identified as the merger of two neutron stars coming from NGC 4993, a galaxy 140 million light years away from us. The very same event was detected in γ-ray, X-ray, UV, IR, radio frequency and even in the optical region of the electromagnetic spectrum, starting the new era of multi-messenger astronomy. To understand and describe neutron stars, an appropriate equation of state that satisfies bulk nuclear matter properties is necessary. GW170817 detection contributed with extra constraints to determine it. On the other hand, magnetars are the same sort of compact object, but bearing much stronger magnetic fields that can reach up to 1015 G on the surface as compared with the usual 1012 G present in ordinary pulsars. While the description of ordinary pulsars is not completely established, describing magnetars poses extra challenges. In this paper, I give an overview on the history of neutron stars and on the development of nuclear models and show how the description of the tiny world of the nuclear physics can help the understanding of the cosmos, especially of the neutron stars.
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16
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Nuclear Physics and Astrophysics Constraints on the High Density Matter Equation of State. UNIVERSE 2021. [DOI: 10.3390/universe7080257] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
(1) This review has been written in memory of Steven Moszkowski who unexpectedly passed away in December 2020. It has been inspired by our many years of discussions. Steven’s enthusiasm, drive and determination to understand atomic nuclei in simple terms of basic laws of physics was infectious. He sought the fundamental origin of nuclear forces in free space, and their saturation and modification in nuclear medium. His untimely departure left our job unfinished but his legacy lives on. (2) Focusing on the nuclear force acting in nuclear matter of astrophysical interest and its equation of state (EoS), we take several typical snapshots of evolution of the theory of nuclear forces. We start from original ideas in the 1930s moving through to its overwhelming diversity today. The development is supported by modern observational and terrestrial data and their inference in the multimessenger era, as well as by novel mathematical techniques and computer power. (3) We find that, despite the admirable effort both in theory and measurement, we are facing multiple models dependent on a large number of variable correlated parameters which cannot be constrained by data, which are not yet accurate, nor sensitive enough, to identify the theory closest to reality. The role of microphysics in the theories is severely limited or neglected, mostly deemed to be too difficult to tackle. (4) Taking the EoS of high-density matter as an example, we propose to develop models, based, as much as currently possible, on the microphysics of the nuclear force, with a minimal set of parameters, chosen under clear physical guidance. Still somewhat phenomenological, such models could pave the way to realistic predictions, not tracing the measurement, but leading it.
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17
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Abstract
Gravitational waves are ripples in spacetime generated by the acceleration of astrophysical objects; a direct consequence of general relativity, they were first directly observed in 2015. Here, I review the first 5 years of gravitational-wave detections. More than 50 gravitational-wave events have been found, emitted by pairs of merging compact objects such as neutron stars and black holes. These signals yield insights into the formation of compact objects and their progenitor stars, enable stringent tests of general relativity, and constrain the behavior of matter at densities higher than that of an atomic nucleus. Mergers that emit both gravitational and electromagnetic waves probe the formation of short gamma-ray bursts and the nucleosynthesis of heavy elements, and they measure the local expansion rate of the Universe.
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Affiliation(s)
- Salvatore Vitale
- Laser Interferometer Gravitational-Wave Observatory Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139, USA.,Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
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18
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Baltus G, Janquart J, Lopez M, Reza A, Caudill S, Cudell JR. Convolutional neural networks for the detection of the early inspiral of a gravitational-wave signal. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.103.102003] [Citation(s) in RCA: 9] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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19
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Côté B, Eichler M, Yagüe López A, Vassh N, Mumpower MR, Világos B, Soós B, Arcones A, Sprouse TM, Surman R, Pignatari M, Pető MK, Wehmeyer B, Rauscher T, Lugaro M. 129I and 247Cm in meteorites constrain the last astrophysical source of solar r-process elements. Science 2021; 371:945-948. [PMID: 33632846 DOI: 10.1126/science.aba1111] [Citation(s) in RCA: 20] [Impact Index Per Article: 6.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/07/2019] [Accepted: 01/25/2021] [Indexed: 11/03/2022]
Abstract
The composition of the early Solar System can be inferred from meteorites. Many elements heavier than iron were formed by the rapid neutron capture process (r-process), but the astrophysical sources where this occurred remain poorly understood. We demonstrate that the near-identical half-lives [Formula: see text] of the radioactive r-process nuclei iodine-129 and curium-247 preserve their ratio, irrespective of the time between production and incorporation into the Solar System. We constrain the last r-process source by comparing the measured meteoritic ratio 129I/247Cm = 438 ± 184 with nucleosynthesis calculations based on neutron star merger and magneto-rotational supernova simulations. Moderately neutron-rich conditions, often found in merger disk ejecta simulations, are most consistent with the meteoritic value. Uncertain nuclear physics data limit our confidence in this conclusion.
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Affiliation(s)
- Benoit Côté
- Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network, Konkoly Observatory, 1121 Budapest, Hungary. .,Institute of Physics, Eötvös Loránd University, 1117 Budapest, Hungary.,National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA
| | - Marius Eichler
- Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany
| | - Andrés Yagüe López
- Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network, Konkoly Observatory, 1121 Budapest, Hungary
| | - Nicole Vassh
- Department of Physics, University of Notre Dame, Notre Dame, IN 46556, USA
| | - Matthew R Mumpower
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA.,Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
| | - Blanka Világos
- Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network, Konkoly Observatory, 1121 Budapest, Hungary.,Institute of Physics, Eötvös Loránd University, 1117 Budapest, Hungary
| | - Benjámin Soós
- Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network, Konkoly Observatory, 1121 Budapest, Hungary.,Institute of Physics, Eötvös Loránd University, 1117 Budapest, Hungary
| | - Almudena Arcones
- Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany.,GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
| | - Trevor M Sprouse
- Department of Physics, University of Notre Dame, Notre Dame, IN 46556, USA.,Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
| | - Rebecca Surman
- Department of Physics, University of Notre Dame, Notre Dame, IN 46556, USA
| | - Marco Pignatari
- E.A. Milne Centre for Astrophysics, University of Hull, Hull HU6 7RX, UK.,Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network, Konkoly Observatory, 1121 Budapest, Hungary
| | - Mária K Pető
- Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network, Konkoly Observatory, 1121 Budapest, Hungary
| | - Benjamin Wehmeyer
- Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network, Konkoly Observatory, 1121 Budapest, Hungary.,Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK
| | - Thomas Rauscher
- Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK.,Department of Physics, University of Basel, 4056 Basel, Switzerland
| | - Maria Lugaro
- Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network, Konkoly Observatory, 1121 Budapest, Hungary.,Institute of Physics, Eötvös Loránd University, 1117 Budapest, Hungary.,Monash Centre for Astrophysics, School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia
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20
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Dietrich T, Coughlin MW, Pang PTH, Bulla M, Heinzel J, Issa L, Tews I, Antier S. Multimessenger constraints on the neutron-star equation of state and the Hubble constant. Science 2020; 370:1450-1453. [PMID: 33335061 DOI: 10.1126/science.abb4317] [Citation(s) in RCA: 32] [Impact Index Per Article: 8.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/24/2020] [Accepted: 10/27/2020] [Indexed: 11/02/2022]
Abstract
Observations of neutron-star mergers with distinct messengers, including gravitational waves and electromagnetic signals, can be used to study the behavior of matter denser than an atomic nucleus and to measure the expansion rate of the Universe as quantified by the Hubble constant. We performed a joint analysis of the gravitational-wave event GW170817 with its electromagnetic counterparts AT2017gfo and GRB170817A, and the gravitational-wave event GW190425, both originating from neutron-star mergers. We combined these with previous measurements of pulsars using x-ray and radio observations, and nuclear-theory computations using chiral effective field theory, to constrain the neutron-star equation of state. We found that the radius of a 1.4-solar mass neutron star is [Formula: see text] km at 90% confidence and the Hubble constant is [Formula: see text] at 1σ uncertainty.
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Affiliation(s)
- Tim Dietrich
- Institut für Physik und Astronomie, Universität Potsdam, 14476 Potsdam, Germany. .,Nikhef, 1098 XG Amsterdam, Netherlands
| | - Michael W Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA
| | - Peter T H Pang
- Nikhef, 1098 XG Amsterdam, Netherlands.,Department of Physics, Utrecht University, 3584 CC Utrecht, Netherlands
| | - Mattia Bulla
- Nordic Institute for Theoretical Physics (Nordita), 106 91 Stockholm, Sweden
| | - Jack Heinzel
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA.,Department of Physics and Astronomy, Carleton College, Northfield, MN 55057, USA.,Artemis, Université Côte d'Azur, Centre National de la Recherche Scientifique, F-06304 Nice, France
| | - Lina Issa
- Nordic Institute for Theoretical Physics (Nordita), 106 91 Stockholm, Sweden.,École normale supérieure, Université Paris-Saclay, 91190 Gif-sur-Yvette, France
| | - Ingo Tews
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
| | - Sarah Antier
- Astroparticule et Cosmologie, Université de Paris, Centre National de la Recherche Scientifique, F-75013 Paris, France
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Ruiz M, Paschalidis V, Tsokaros A, Shapiro SL. Black hole-neutron star coalescence: Effects of the neutron star spin on jet launching and dynamical ejecta mass. PHYSICAL REVIEW. D. (2016) 2020; 102:124077. [PMID: 34595362 PMCID: PMC8477222 DOI: 10.1103/physrevd.102.124077] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Black hole-neutron star (BHNS) mergers are thought to be sources of gravitational waves (GWs) with coincident electromagnetic (EM) counterparts. To further probe whether these systems are viable progenitors of short gamma-ray bursts (SGRBs) and kilonovas, and how one may use (the lack of) EM counterparts associated with LIGO/Virgo candidate BHNS GW events to sharpen parameter estimation, we study the impact of neutron star spin in BHNS mergers. Using dynamical spacetime magnetohydrodynamic simulations of BHNSs initially on a quasicircular orbit, we survey configurations that differ in the BH spin (a BH/M BH = 0 and 0.75), the NS spin (a NS/M NS = -0.17, 0, 0.23, and 0.33), and the binary mass ratio (q = M BH:M NS = 3:1 and 5:1). The general trend we find is that increasing the NS prograde spin increases both the rest mass of the accretion disk onto the remnant black hole, and the rest mass of dynamically ejected matter. By a time Δt ~ 3500-5500M ~ 88-138(M NS/1.4 M ⊙) ms after the peak gravitational-wave amplitude, a magnetically driven jet is launched only for q = 3:1 regardless of the initial NS spin. The lifetime of the jets [Δt ~ 0.5-0.8(M NS/1.4 M ⊙) s] and their outgoing Poynting luminosity [L Poyn ~ 1051.5±0.5 erg/s] are consistent with typical SGRBs' luminosities and expectations from the Blandford-Znajek mechanism. By the time we terminate our simulations, we do not observe either an outflow or a large-scale magnetic-field collimation for the other systems we consider. The mass range of dynamically ejected matter is 10-4.5-10-2(M NS/1.4 M ⊙) M ⊙, which can power kilonovas with peak bolometric luminosities L knova ~ 1040-1041.4 erg/s with rise times ≲6.5 h and potentially detectable by the LSST.
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Affiliation(s)
- Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Vasileios Paschalidis
- Departments of Astronomy and Physics, University of Arizona, Tucson, Arizona 85719, USA
| | - Antonios Tsokaros
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy and NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
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Bernuzzi S. Neutron star merger remnants. GENERAL RELATIVITY AND GRAVITATION 2020; 52:108. [PMID: 39247669 PMCID: PMC11377492 DOI: 10.1007/s10714-020-02752-5] [Citation(s) in RCA: 9] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/21/2020] [Accepted: 10/09/2020] [Indexed: 09/10/2024]
Abstract
Binary neutron star mergers observations are a unique way to constrain fundamental physics and astrophysics at the extreme. The interpretation of gravitational-wave events and their electromagnetic counterparts crucially relies on general-relativistic models of the merger remnants. Quantitative models can be obtained only by means of numerical relativity simulations in 3 + 1 dimensions including detailed input physics for the nuclear matter, electromagnetic and weak interactions. This review summarizes the current understanding of merger remnants focusing on some of the aspects that are relevant for multimessenger observations.
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Affiliation(s)
- Sebastiano Bernuzzi
- Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universität Jena, Max-Wien-Platz 1, 07743 Jena, Germany
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Morisaki S, Raymond V. Rapid parameter estimation of gravitational waves from binary neutron star coalescence using focused reduced order quadrature. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.102.104020] [Citation(s) in RCA: 16] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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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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Asymmetric mass ratios for bright double neutron-star mergers. Nature 2020; 583:211-214. [PMID: 32641814 DOI: 10.1038/s41586-020-2439-x] [Citation(s) in RCA: 22] [Impact Index Per Article: 5.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/19/2019] [Accepted: 04/14/2020] [Indexed: 11/09/2022]
Abstract
The discovery of a radioactively powered kilonova associated with the binary neutron-star merger GW170817 remains the only confirmed electromagnetic counterpart to a gravitational-wave event1,2. Observations of the late-time electromagnetic emission, however, do not agree with the expectations from standard neutron-star merger models. Although the large measured ejecta mass3,4 could be explained by a progenitor system that is asymmetric in terms of the stellar component masses (that is, with a mass ratio q of 0.7 to 0.8)5, the known Galactic population of merging double neutron-star systems (that is, those that will coalesce within billions of years or less) has until now consisted only of nearly equal-mass (q > 0.9) binaries6. The pulsar PSR J1913+1102 is a double system in a five-hour, low-eccentricity (0.09) orbit, with an orbital separation of 1.8 solar radii7, and the two neutron stars are predicted to coalesce in [Formula: see text] million years owing to gravitational-wave emission. Here we report that the masses of the pulsar and the companion neutron star, as measured by a dedicated pulsar timing campaign, are 1.62 ± 0.03 and 1.27 ± 0.03 solar masses, respectively. With a measured mass ratio of q = 0.78 ± 0.03, this is the most asymmetric merging system reported so far. On the basis of this detection, our population synthesis analysis implies that such asymmetric binaries represent between 2 and 30 per cent (90 per cent confidence) of the total population of merging binaries. The coalescence of a member of this population offers a possible explanation for the anomalous properties of GW170817, including the observed kilonova emission from that event.
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Abstract
Mendeleev's introduction of the periodic table of elements is one of the most important milestones in the history of chemistry, as it brought order into the known chemical and physical behaviour of the elements. The periodic table can be seen as parallel to the Standard Model in particle physics, in which the elementary particles known today can be ordered according to their intrinsic properties. The underlying fundamental theory to describe the interactions between particles comes from quantum theory or, more specifically, from quantum field theory and its inherent symmetries. In the periodic table, the elements are placed into a certain period and group based on electronic configurations that originate from the Pauli and Aufbau principles for the electrons surrounding a positively charged nucleus. This order enables us to approximately predict the chemical and physical properties of elements. Apparent anomalies can arise from relativistic effects, partial-screening phenomena (of type lanthanide contraction) and the compact size of the first shell of every l-value. Further, ambiguities in electron configurations and the breakdown of assigning a dominant configuration, owing to configuration mixing and dense spectra for the heaviest elements in the periodic table. For the short-lived transactinides, the nuclear stability becomes an important factor in chemical studies. Nuclear stability, decay rates, spectra and reaction cross sections are also important for predicting the astrophysical origin of the elements, including the production of the heavy elements beyond iron in supernova explosions or neutron-star mergers. In this Perspective, we critically analyse the periodic table of elements and the current status of theoretical predictions and origins for the heaviest elements, which combine both quantum chemistry and physics.
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GW190814: Gravitational Waves from the Coalescence of a 23 Solar Mass Black Hole with a 2.6 Solar Mass Compact Object. ACTA ACUST UNITED AC 2020. [DOI: 10.3847/2041-8213/ab960f] [Citation(s) in RCA: 725] [Impact Index Per Article: 181.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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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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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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Two Years of Nonthermal Emission from the Binary Neutron Star Merger GW170817: Rapid Fading of the Jet Afterglow and First Constraints on the Kilonova Fastest Ejecta. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/2041-8213/ab5226] [Citation(s) in RCA: 83] [Impact Index Per Article: 16.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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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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Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/2041-8213/ab3800] [Citation(s) in RCA: 442] [Impact Index Per Article: 88.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Wang HT, Jiang Z, Sesana A, Barausse E, Huang SJ, Wang YF, Feng WF, Wang Y, Hu YM, Mei J, Luo J. Science with the TianQin observatory: Preliminary results on massive black hole binaries. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.100.043003] [Citation(s) in RCA: 35] [Impact Index Per Article: 7.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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35
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Follow-up of the Neutron Star Bearing Gravitational-wave Candidate Events S190425z and S190426c with MMT and SOAR. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/2041-8213/ab271c] [Citation(s) in RCA: 45] [Impact Index Per Article: 9.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Collapsars as a major source of r-process elements. Nature 2019; 569:241-244. [PMID: 31068724 DOI: 10.1038/s41586-019-1136-0] [Citation(s) in RCA: 20] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/21/2018] [Accepted: 02/12/2019] [Indexed: 11/08/2022]
Abstract
The production of elements by rapid neutron capture (r-process) in neutron-star mergers is expected theoretically and is supported by multimessenger observations1-3 of gravitational-wave event GW170817: this production route is in principle sufficient to account for most of the r-process elements in the Universe4. Analysis of the kilonova that accompanied GW170817 identified5,6 delayed outflows from a remnant accretion disk formed around the newly born black hole7-10 as the dominant source of heavy r-process material from that event9,11. Similar accretion disks are expected to form in collapsars (the supernova-triggering collapse of rapidly rotating massive stars), which have previously been speculated to produce r-process elements12,13. Recent observations of stars rich in such elements in the dwarf galaxy Reticulum II14, as well as the Galactic chemical enrichment of europium relative to iron over longer timescales15,16, are more consistent with rare supernovae acting at low stellar metallicities than with neutron-star mergers. Here we report simulations that show that collapsar accretion disks yield sufficient r-process elements to explain observed abundances in the Universe. Although these supernovae are rarer than neutron-star mergers, the larger amount of material ejected per event compensates for the lower rate of occurrence. We calculate that collapsars may supply more than 80 per cent of the r-process content of the Universe.
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A nearby neutron-star merger explains the actinide abundances in the early Solar System. Nature 2019; 569:85-88. [PMID: 31043731 DOI: 10.1038/s41586-019-1113-7] [Citation(s) in RCA: 22] [Impact Index Per Article: 4.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/01/2018] [Accepted: 02/11/2019] [Indexed: 11/08/2022]
Abstract
A growing body of evidence indicates that binary neutron-star mergers are the primary origin of heavy elements produced exclusively through rapid neutron capture1-4 (the 'r-process'). As neutron-star mergers occur infrequently, their deposition of radioactive isotopes into the pre-solar nebula could have been dominated by a few nearby events. Although short-lived r-process isotopes-with half-lives shorter than 100 million years-are no longer present in the Solar System, their abundances in the early Solar System are known because their daughter products were preserved in high-temperature condensates found in meteorites5. Here we report that abundances of short-lived r-process isotopes in the early Solar System point to their origin in neutron-star mergers, and indicate substantial deposition by a single nearby merger event. By comparing numerical simulations with the early Solar System abundance ratios of actinides produced exclusively through the r-process, we constrain the rate of occurrence of their Galactic production sites to within about 1-100 per million years. This is consistent with observational estimates of neutron-star merger rates6-8, but rules out supernovae and stellar sources. We further find that there was probably a single nearby merger that produced much of the curium and a substantial fraction of the plutonium present in the early Solar System. Such an event may have occurred about 300 parsecs away from the pre-solar nebula, approximately 80 million years before the formation of the Solar System.
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On Neutron Star Mergers as the Source of r-process-enhanced Metal-poor Stars in the Milky Way. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/ab1341] [Citation(s) in RCA: 20] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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40
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Fu X, Zhou L, Chen J. Testing the cosmic distance-duality relation from future gravitational wave standard sirens. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.083523] [Citation(s) in RCA: 21] [Impact Index Per Article: 4.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Neutron Star Mergers Might Not Be the Only Source of r-process Elements in the Milky Way. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/ab10db] [Citation(s) in RCA: 107] [Impact Index Per Article: 21.4] [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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Wu MR, Barnes J, Martínez-Pinedo G, Metzger BD. Fingerprints of Heavy-Element Nucleosynthesis in the Late-Time Lightcurves of Kilonovae. PHYSICAL REVIEW LETTERS 2019; 122:062701. [PMID: 30822042 DOI: 10.1103/physrevlett.122.062701] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/30/2018] [Revised: 11/15/2018] [Indexed: 06/09/2023]
Abstract
The kilonova emission observed following the binary neutron star merger event GW170817 provided the first direct evidence for the synthesis of heavy nuclei through the rapid neutron capture process (r process). The late-time transition in the spectral energy distribution to near-infrared wavelengths was interpreted as indicating the production of lanthanide nuclei, with atomic mass number A≳140. However, compelling evidence for the presence of even heavier third-peak (A≈195) r-process elements (e.g., gold, platinum) or translead nuclei remains elusive. At early times (∼days) most of the r-process heating arises from a large statistical ensemble of β decays, which thermalize efficiently while the ejecta is still dense, generating a heating rate that is reasonably approximated by a single power law. However, at later times of weeks to months, the decay energy input can also possibly be dominated by a discrete number of α decays, ^{223}Ra (half-life t_{1/2}=11.43 d), ^{225}Ac (t_{1/2}=10.0 d, following the β decay of ^{225}Ra with t_{1/2}=14.9 d), and the fissioning isotope ^{254}Cf (t_{1/2}=60.5 d), which liberate more energy per decay and thermalize with greater efficiency than β-decay products. Late-time nebular observations of kilonovae which constrain the radioactive power provide the potential to identify signatures of these individual isotopes, thus confirming the production of heavy nuclei. In order to constrain the bolometric light to the required accuracy, multiepoch and wideband observations are required with sensitive instruments like the James Webb Space Telescope. In addition, by comparing the nuclear heating rate obtained with an abundance distribution that follows the solar r abundance pattern, to the bolometric lightcurve of AT2017gfo, we find that the yet-uncertain r abundance of ^{72}Ge plays a decisive role in powering the lightcurve, if one assumes that GW170817 has produced a full range of the solar r abundances down to mass number A∼70.
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Affiliation(s)
- Meng-Ru Wu
- Institute of Physics, Academia Sinica, Taipei 11529, Taiwan
- Institute of Astronomy and Astrophysics, Academia Sinica, Taipei 10617, Taiwan
| | - J Barnes
- Department of Physics and Columbia Astrophysics Laboratory, Columbia University, Pupin Hall, New York, New York 10027, USA
| | - G Martínez-Pinedo
- GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany
- Institut für Kernphysik (Theoriezentrum), Technische Universität Darmstadt, Schlossgartenstraße 2, 64289 Darmstadt, Germany
| | - B D Metzger
- Department of Physics and Columbia Astrophysics Laboratory, Columbia University, Pupin Hall, New York, New York 10027, USA
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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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Duez MD, Zlochower Y. Numerical relativity of compact binaries in the 21st century. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2019; 82:016902. [PMID: 30117809 DOI: 10.1088/1361-6633/aadb16] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
We review the dramatic progress in the simulations of compact objects and compact-object binaries that has taken place in the first two decades of the twenty-first century. This includes simulations of the inspirals and violent mergers of binaries containing black holes and neutron stars, as well as simulations of black-hole formation through failed supernovae and high-mass neutron star-neutron star mergers. Modeling such events requires numerical integration of the field equations of general relativity in three spatial dimensions, coupled, in the case of neutron-star containing binaries, with increasingly sophisticated treatment of fluids, electromagnetic fields, and neutrino radiation. However, it was not until 2005 that accurate long-term evolutions of binaries containing black holes were even possible (Pretorius 2005 Phys. Rev. Lett. 95 121101, Campanelli et al 2006 Phys. Rev. Lett. 96 111101, Baker et al 2006 Phys. Rev. Lett. 96 111102). Since then, there has been an explosion of new results and insights into the physics of strongly-gravitating system. Particular emphasis has been placed on understanding the gravitational wave and electromagnetic signatures from these extreme events. And with the recent dramatic discoveries of gravitational waves from merging black holes by the Laser Interferometric Gravitational Wave Observatory and Virgo, and the subsequent discovery of both electromagnetic and gravitational wave signals from a merging neutron star-neutron star binary, numerical relativity became an indispensable tool for the new field of multimessenger astronomy.
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Affiliation(s)
- Matthew D Duez
- Department of Physics and Astronomy, Washington State University, Pullman, WA 99164, United States of America
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46
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Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aaf054] [Citation(s) in RCA: 212] [Impact Index Per Article: 35.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Numerical Simulations of the Jet Dynamics and Synchrotron Radiation of Binary Neutron Star Merger Event GW170817/GRB 170817A. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aacf9c] [Citation(s) in RCA: 69] [Impact Index Per Article: 11.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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