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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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Pang PTH, Dietrich T, Coughlin MW, Bulla M, Tews I, Almualla M, Barna T, Kiendrebeogo RW, Kunert N, Mansingh G, Reed B, Sravan N, Toivonen A, Antier S, VandenBerg RO, Heinzel J, Nedora V, Salehi P, Sharma R, Somasundaram R, Van Den Broeck C. An updated nuclear-physics and multi-messenger astrophysics framework for binary neutron star mergers. Nat Commun 2023; 14:8352. [PMID: 38123551 PMCID: PMC10733434 DOI: 10.1038/s41467-023-43932-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/23/2023] [Accepted: 11/24/2023] [Indexed: 12/23/2023] Open
Abstract
The multi-messenger detection of the gravitational-wave signal GW170817, the corresponding kilonova AT2017gfo and the short gamma-ray burst GRB170817A, as well as the observed afterglow has delivered a scientific breakthrough. For an accurate interpretation of all these different messengers, one requires robust theoretical models that describe the emitted gravitational-wave, the electromagnetic emission, and dense matter reliably. In addition, one needs efficient and accurate computational tools to ensure a correct cross-correlation between the models and the observational data. For this purpose, we have developed the Nuclear-physics and Multi-Messenger Astrophysics framework NMMA. The code allows incorporation of nuclear-physics constraints at low densities as well as X-ray and radio observations of isolated neutron stars. In previous works, the NMMA code has allowed us to constrain the equation of state of supranuclear dense matter, to measure the Hubble constant, and to compare dense-matter physics probed in neutron-star mergers and in heavy-ion collisions, and to classify electromagnetic observations and perform model selection. Here, we show an extension of the NMMA code as a first attempt of analyzing the gravitational-wave signal, the kilonova, and the gamma-ray burst afterglow simultaneously. Incorporating all available information, we estimate the radius of a 1.4M⊙ neutron star to be [Formula: see text] km.
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Affiliation(s)
- Peter T H Pang
- Nikhef, Science Park 105, 1098 XG, Amsterdam, The Netherlands
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Princetonplein 1, 3584 CC, Utrecht, The Netherlands
| | - Tim Dietrich
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany.
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476, Potsdam, Germany.
| | - Michael W Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Mattia Bulla
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-106 91, Stockholm, Sweden
- Department of Physics and Earth Science, University of Ferrara, Via Saragat 1, I-44122, Ferrara, Italy
- INFN, Sezione di Ferrara, Via Saragat 1, I-44122, Ferrara, Italy
- INAF, Osservatorio Astronomico d'Abruzzo, Via Mentore Maggini snc, 64100, Teramo, Italy
| | - Ingo Tews
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, 87545, USA
| | - Mouza Almualla
- Department of Physics, American University of Sharjah, PO Box 26666, Sharjah, UAE
| | - Tyler Barna
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Ramodgwendé Weizmann Kiendrebeogo
- Laboratoire de Physique et de Chimie de l'Environnement, Université Joseph KI-ZERBO, Ouagadougou, Burkina Faso
- Observatoire de la Côte d'Azur, Université Côte d'Azur, CNRS, 96 Boulevard de l'Observatoire, F06304, Nice Cedex 4, France
| | - Nina Kunert
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany
| | - Gargi Mansingh
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
- Department of Physics, American University, Washington, DC, 20016, USA
| | - Brandon Reed
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
- Department of Physics and Astronomy, University of Minnesota-Duluth, Duluth, MN, 55812, USA
| | - Niharika Sravan
- Department of Physics, Drexel University, Philadelphia, PA, 19104, USA
| | - Andrew Toivonen
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Sarah Antier
- Observatoire de la Côte d'Azur, Université Côte d'Azur, CNRS, 96 Boulevard de l'Observatoire, F06304, Nice Cedex 4, France
| | - Robert O VandenBerg
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, 55455, USA
| | - Jack Heinzel
- Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Ave, Cambridge, MA, 02139, USA
| | - Vsevolod Nedora
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476, Potsdam, Germany
| | - Pouyan Salehi
- Institut für Physik und Astronomie, Universität Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany
| | - Ritwik Sharma
- Department of Physics, Deshbandhu College, University of Delhi, New Delhi, India
| | - Rahul Somasundaram
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, 87545, USA
- Université Lyon, Université Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, F-69622, Villeurbanne, France
- Department of Physics, Syracuse University, Syracuse, NY, 13244, USA
| | - Chris Van Den Broeck
- Nikhef, Science Park 105, 1098 XG, Amsterdam, The Netherlands
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Princetonplein 1, 3584 CC, Utrecht, The Netherlands
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Annala E, Gorda T, Hirvonen J, Komoltsev O, Kurkela A, Nättilä J, Vuorinen A. Strongly interacting matter exhibits deconfined behavior in massive neutron stars. Nat Commun 2023; 14:8451. [PMID: 38114461 PMCID: PMC10730725 DOI: 10.1038/s41467-023-44051-y] [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: 05/03/2023] [Accepted: 11/28/2023] [Indexed: 12/21/2023] Open
Abstract
Neutron-star cores contain matter at the highest densities in our Universe. This highly compressed matter may undergo a phase transition where nuclear matter melts into deconfined quark matter, liberating its constituent quarks and gluons. Quark matter exhibits an approximate conformal symmetry, predicting a specific form for its equation of state (EoS), but it is currently unknown whether the transition takes place inside at least some physical neutron stars. Here, we quantify this likelihood by combining information from astrophysical observations and theoretical calculations. Using Bayesian inference, we demonstrate that in the cores of maximally massive stars, the EoS is consistent with quark matter. We do this by establishing approximate conformal symmetry restoration with high credence at the highest densities probed and demonstrating that the number of active degrees of freedom is consistent with deconfined matter. The remaining likelihood is observed to correspond to EoSs exhibiting phase-transition-like behavior, treated as arbitrarily rapid crossovers in our framework.
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Affiliation(s)
- Eemeli Annala
- Department of Physics and Helsinki Institute of Physics, University of Helsinki, P.O. Box 64, FI-00014, University of Helsinki, Finland
| | - Tyler Gorda
- Technische Universität Darmstadt, Department of Physics, 64289, Darmstadt, Germany.
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291, Darmstadt, Germany.
| | - Joonas Hirvonen
- Department of Physics and Helsinki Institute of Physics, University of Helsinki, P.O. Box 64, FI-00014, University of Helsinki, Finland.
| | - Oleg Komoltsev
- Faculty of Science and Technology, University of Stavanger, 4036, Stavanger, Norway.
| | - Aleksi Kurkela
- Faculty of Science and Technology, University of Stavanger, 4036, Stavanger, Norway.
| | - Joonas Nättilä
- Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY, 10010, USA.
- Physics Department and Columbia Astrophysics Laboratory, Columbia University, 538 West 120th Street, New York, NY, 10027, USA.
| | - Aleksi Vuorinen
- Department of Physics and Helsinki Institute of Physics, University of Helsinki, P.O. Box 64, FI-00014, University of Helsinki, Finland.
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5
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Wu Z, Fan J, Zhang X, Qi J, Wu H. Signatures of Prethermalization in a Quenched Cavity-Mediated Long-Range Interacting Fermi Gas. PHYSICAL REVIEW LETTERS 2023; 131:243401. [PMID: 38181153 DOI: 10.1103/physrevlett.131.243401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/11/2023] [Revised: 11/14/2023] [Accepted: 11/16/2023] [Indexed: 01/07/2024]
Abstract
The coupling of ultracold quantum gases to an optical cavity provides an ideal system for studying the novel long-range interacting nonequilibrium dynamics. Here we report an experimental observation of the out-of-equilibrium dynamics of a degenerate Fermi gas in the cavity after quenching the pump strength over a superradiant quantum phase transition. The relaxation dynamics exhibits impressively different stages of a delay, violent relaxation, long-lifetime prethermalization, and slowly final thermalization due to the photon-mediated long-range interaction with dissipation. Importantly, we reveal that the lifetime of the system stayed on the prethermalization exhibits the superlinear scaling of the atom number. Furthermore, we show that the backaction of the superradiant cavity field on the gas causes the exchange of atoms between the normal and superradiant state in the early evolution and then induces the prethermalization. This work opens an avenue to explore complex nonequilibrium dynamics of the dissipatively long-range interacting Fermi gases.
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Affiliation(s)
- Zemao Wu
- State Key Laboratory of Precision Spectroscopy, Institute of Quantum Science and Precision Measurement, East China Normal University, Shanghai 200062, China
| | - Jijie Fan
- State Key Laboratory of Precision Spectroscopy, Institute of Quantum Science and Precision Measurement, East China Normal University, Shanghai 200062, China
| | - Xue Zhang
- State Key Laboratory of Precision Spectroscopy, Institute of Quantum Science and Precision Measurement, East China Normal University, Shanghai 200062, China
| | - Jiansheng Qi
- State Key Laboratory of Precision Spectroscopy, Institute of Quantum Science and Precision Measurement, East China Normal University, Shanghai 200062, China
| | - Haibin Wu
- State Key Laboratory of Precision Spectroscopy, Institute of Quantum Science and Precision Measurement, East China Normal University, Shanghai 200062, China
- Shanghai Branch, Hefei National Laboratory, Shanghai 201315, China
- Collaborative Innovation Center of Extreme Optics, Shanxi University, Taiyuan 030006, China
- Shanghai Research Center for Quantum Sciences, Shanghai 201315, China
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6
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Omana Kuttan M, Steinheimer J, Zhou K, Stoecker H. QCD Equation of State of Dense Nuclear Matter from a Bayesian Analysis of Heavy-Ion Collision Data. PHYSICAL REVIEW LETTERS 2023; 131:202303. [PMID: 38039475 DOI: 10.1103/physrevlett.131.202303] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/14/2022] [Revised: 04/24/2023] [Accepted: 10/18/2023] [Indexed: 12/03/2023]
Abstract
Bayesian methods are used to constrain the density dependence of the QCD equation of state (EOS) for dense nuclear matter using the data of mean transverse kinetic energy and elliptic flow of protons from heavy ion collisions (HICs), in the beam energy range sqrt[s_{NN}]=2-10 GeV. The analysis yields tight constraints on the density dependent EOS up to 4 times the nuclear saturation density. The extracted EOS yields good agreement with other observables measured in HIC experiments and constraints from astrophysical observations both of which were not used in the inference. The sensitivity of inference to the choice of observables is also discussed.
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Affiliation(s)
- Manjunath Omana Kuttan
- Frankfurt Institute for Advanced Studies, Ruth-Moufang-Strasse 1, D-60438 Frankfurt am Main, Germany
- Institut für Theoretische Physik, Goethe Universität Frankfurt, Max-von-Laue-Strasse 1, D-60438 Frankfurt am Main, Germany
- Xidian-FIAS International Joint Research Center, Giersch Science Center, D-60438 Frankfurt am Main, Germany
| | - Jan Steinheimer
- Frankfurt Institute for Advanced Studies, Ruth-Moufang-Strasse 1, D-60438 Frankfurt am Main, Germany
| | - Kai Zhou
- Frankfurt Institute for Advanced Studies, Ruth-Moufang-Strasse 1, D-60438 Frankfurt am Main, Germany
| | - Horst Stoecker
- Frankfurt Institute for Advanced Studies, Ruth-Moufang-Strasse 1, D-60438 Frankfurt am Main, Germany
- Institut für Theoretische Physik, Goethe Universität Frankfurt, Max-von-Laue-Strasse 1, D-60438 Frankfurt am Main, Germany
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Planckstrasse 1, D-64291 Darmstadt, Germany
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7
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Jakobus P, Müller B, Heger A, Zha S, Powell J, Motornenko A, Steinheimer J, Stöcker H. Gravitational Waves from a Core g Mode in Supernovae as Probes of the High-Density Equation of State. PHYSICAL REVIEW LETTERS 2023; 131:191201. [PMID: 38000402 DOI: 10.1103/physrevlett.131.191201] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/16/2023] [Revised: 04/18/2023] [Accepted: 09/29/2023] [Indexed: 11/26/2023]
Abstract
Using relativistic supernova simulations of massive progenitor stars with a quark-hadron equation of state (EOS) and a purely hadronic EOS, we identify a distinctive feature in the gravitational-wave signal that originates from a buoyancy-driven mode (g mode) below the proto-neutron star convection zone. The mode frequency lies in the range 200≲f≲800 Hz and decreases with time. As the mode lives in the core of the proto-neutron star, its frequency and power are highly sensitive to the EOS, in particular the sound speed around twice saturation density.
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Affiliation(s)
- Pia Jakobus
- School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia
| | - Bernhard Müller
- School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia
| | - Alexander Heger
- School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia
| | - Shuai Zha
- Yunnan Observatories, Chinese Academy of Sciences (CAS), Kunming 650216, China; Key Laboratory for the Structure and Evolution of Celestial Objects, CAS, Kunming 650216, China; and International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, China
| | - Jade Powell
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia
| | - Anton Motornenko
- Frankfurt Institute for Advanced Studies, Giersch Science Center, Frankfurt am Main, Germany
| | - Jan Steinheimer
- Frankfurt Institute for Advanced Studies, Giersch Science Center, Frankfurt am Main, Germany
| | - Horst Stöcker
- Frankfurt Institute for Advanced Studies, Giersch Science Center, Frankfurt am Main, Germany
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8
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Han MZ, Huang YJ, Tang SP, Fan YZ. Plausible presence of new state in neutron stars with masses above 0.98M TOV. Sci Bull (Beijing) 2023; 68:913-919. [PMID: 37080849 DOI: 10.1016/j.scib.2023.04.007] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/30/2023] [Revised: 04/03/2023] [Accepted: 04/04/2023] [Indexed: 04/22/2023]
Abstract
We investigate the neutron star (NS) equation of state (EOS) by incorporating multi-messenger data of GW170817, PSR J0030 + 0451, PSR J0740 + 6620, and state-of-the-art theoretical progresses, including the information from chiral effective field theory (χEFT) and perturbative quantum chromodynamics (pQCD) calculation. Taking advantage of the various structures sampling by a single-layer feed-forward neural network model embedded in the Bayesian nonparametric inference, the structure of NS matter's sound speed cs is explored in a model-agnostic way. It is found that a peak structure is common in the cs2 posterior, locating at 2.4-4.8ρsat (nuclear saturation density) and cs2 exceeds c2/3 at 90% credibility. The non-monotonic behavior suggests evidence of the state deviating from the hadronic matter inside the very massive NSs. Assuming the new/exotic state is featured as it is softer than typical hadronic models or even with hyperons, we find that a sizable (⩾10-3M⊙) exotic core, likely made of quark matter, is plausible for the NS with a gravitational mass above about 0.98MTOV, where MTOV represents the maximum gravitational mass of a non-rotating cold NS. The inferred MTOV=2.18-0.13+0.27M⊙ (90% credibility) is well consistent with the value of 2.17-0.12+0.15M⊙ estimated independently with GW170817/GRB 170817A/AT2017gfo assuming a temporary supramassive NS remnant formed after the merger. PSR J0740 + 6620, the most massive NS detected so far, may host a sizable exotic core with a probability of ≈0.36.
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Affiliation(s)
- Ming-Zhe Han
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China; School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - Yong-Jia Huang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China; School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China; RIKEN Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS), RIKEN, Wako 351-0198, Japan
| | - Shao-Peng Tang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Yi-Zhong Fan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China; School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China.
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9
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Keller J, Hebeler K, Schwenk A. Nuclear Equation of State for Arbitrary Proton Fraction and Temperature Based on Chiral Effective Field Theory and a Gaussian Process Emulator. PHYSICAL REVIEW LETTERS 2023; 130:072701. [PMID: 36867798 DOI: 10.1103/physrevlett.130.072701] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/05/2022] [Revised: 12/09/2022] [Accepted: 01/12/2023] [Indexed: 06/18/2023]
Abstract
We calculate the equation of state of asymmetric nuclear matter at finite temperature based on chiral effective field theory interactions to next-to-next-to-next-to-leading order. Our results assess the theoretical uncertainties from the many-body calculation and the chiral expansion. Using a Gaussian process emulator for the free energy, we derive the thermodynamic properties of matter through consistent derivatives and use the Gaussian process to access arbitrary proton fraction and temperature. This enables a first nonparametric calculation of the equation of state in beta equilibrium, and of the speed of sound and the symmetry energy at finite temperature. Moreover, our results show that the thermal part of the pressure decreases with increasing densities.
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Affiliation(s)
- J Keller
- Technische Universität Darmstadt, Department of Physics, 64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
| | - K Hebeler
- Technische Universität Darmstadt, Department of Physics, 64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - A Schwenk
- Technische Universität Darmstadt, Department of Physics, 64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
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10
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Kölsch M, Dietrich T, Ujevic M, Brügmann B. Investigating the mass-ratio dependence of the prompt-collapse threshold with numerical-relativity simulations. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.044026] [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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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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12
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Incorporating a Radiative Hydrodynamics Scheme in the Numerical-Relativity Code BAM. UNIVERSE 2022. [DOI: 10.3390/universe8070370] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
To study binary neutron star systems and to interpret observational data such as gravitational-wave and kilonova signals, one needs an accurate description of the processes that take place during the final stages of the coalescence, for example, through numerical-relativity simulations. In this work, we present an updated version of the numerical-relativity code BAM in order to incorporate nuclear-theory-based equations of state and a simple description of neutrino interactions through a neutrino leakage scheme. Different test simulations, for stars undergoing a neutrino-induced gravitational collapse and for binary neutron stars systems, validate our new implementation. For the binary neutron stars systems, we show that we can evolve stably and accurately distinct microphysical models employing the different equations of state: SFHo, DD2, and the hyperonic BHBΛϕ. Overall, our test simulations have good agreement with those reported in the literature.
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13
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Diverse data tighten constraints for neutron stars. Nature 2022; 606:258-259. [PMID: 35676425 DOI: 10.1038/d41586-022-01532-2] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
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