1
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König K, Berengut JC, Borschevsky A, Brinson A, Brown BA, Dockery A, Elhatisari S, Eliav E, Ruiz RFG, Holt JD, Hu BS, Karthein J, Lee D, Ma YZ, Meißner UG, Minamisono K, Oleynichenko AV, Pineda SV, Prosnyak SD, Reitsma ML, Skripnikov LV, Vernon A, Zaitsevskii A. Nuclear Charge Radii of Silicon Isotopes. PHYSICAL REVIEW LETTERS 2024; 132:162502. [PMID: 38701465 DOI: 10.1103/physrevlett.132.162502] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/06/2023] [Revised: 01/12/2024] [Accepted: 02/26/2024] [Indexed: 05/05/2024]
Abstract
The nuclear charge radius of ^{32}Si was determined using collinear laser spectroscopy. The experimental result was confronted with ab initio nuclear lattice effective field theory, valence-space in-medium similarity renormalization group, and mean field calculations, highlighting important achievements and challenges of modern many-body methods. The charge radius of ^{32}Si completes the radii of the mirror pair ^{32}Ar-^{32}Si, whose difference was correlated to the slope L of the symmetry energy in the nuclear equation of state. Our result suggests L≤60 MeV, which agrees with complementary observables.
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Affiliation(s)
- Kristian König
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824, USA
- Technische Universtität Darmstadt, 64289 Darmstadt, Germany
| | - Julian C Berengut
- School of Physics, University of New South Wales, NSW 2052, Australia
| | | | - Alex Brinson
- Massachusetts Institute of Technology, Department of Physics, Cambridge, Massachusetts 02139, USA
| | - B Alex Brown
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Astronomy and Physics, Michigan State University, East Lansing, Michigan 48824, USA
| | - Adam Dockery
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Astronomy and Physics, Michigan State University, East Lansing, Michigan 48824, USA
| | - Serdar Elhatisari
- Faculty of Natural Sciences and Engineering, Gaziantep Islam Science and Technology University, Gaziantep 27010, Turkey
- Helmholtz-Institut für Strahlen- und Kernphysik and Bethe Center for Theoretical Physics, Universität Bonn, D-53115 Bonn, Germany
| | - Ephraim Eliav
- School of Chemistry, Tel Aviv University, 69978 Tel Aviv, Israel
| | - Ronald F Garcia Ruiz
- Massachusetts Institute of Technology, Department of Physics, Cambridge, Massachusetts 02139, USA
| | - Jason D Holt
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics, McGill University, Montreal, Quebec H3A 2T8, Canada
| | - Bai-Shan Hu
- National Center for Computational Sciences, Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA
- Physics Division, Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA
| | - Jonas Karthein
- Massachusetts Institute of Technology, Department of Physics, Cambridge, Massachusetts 02139, USA
| | - Dean Lee
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Astronomy and Physics, Michigan State University, East Lansing, Michigan 48824, USA
| | - Yuan-Zhuo Ma
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Astronomy and Physics, Michigan State University, East Lansing, Michigan 48824, USA
| | - Ulf-G Meißner
- Helmholtz-Institut für Strahlen- und Kernphysik and Bethe Center for Theoretical Physics, Universität Bonn, D-53115 Bonn, Germany
| | - Kei Minamisono
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Astronomy and Physics, Michigan State University, East Lansing, Michigan 48824, USA
| | - Alexander V Oleynichenko
- Petersburg Nuclear Physics Institute named by B. P. Konstantinov of NRC "Kurchatov Institute," Gatchina 188300, Russia
- Moscow Institute of Physics and Technology, Institutsky lane 9, Dolgoprudny, Moscow region, 141700, Russia
| | - Skyy V Pineda
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Chemistry, Michigan State University, East Lansing, Michigan 48824, USA
| | - Sergey D Prosnyak
- Petersburg Nuclear Physics Institute named by B. P. Konstantinov of NRC "Kurchatov Institute," Gatchina 188300, Russia
- Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg 199034, Russia
| | | | - Leonid V Skripnikov
- Petersburg Nuclear Physics Institute named by B. P. Konstantinov of NRC "Kurchatov Institute," Gatchina 188300, Russia
- Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg 199034, Russia
| | - Adam Vernon
- Massachusetts Institute of Technology, Department of Physics, Cambridge, Massachusetts 02139, USA
| | - Andréi Zaitsevskii
- Petersburg Nuclear Physics Institute named by B. P. Konstantinov of NRC "Kurchatov Institute," Gatchina 188300, Russia
- Department of Chemistry, M. V. Lomonosov Moscow State University, Leninskie gory 1/3, Moscow 119991, Russia
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2
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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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3
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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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4
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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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5
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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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6
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The Symmetry Energy: Current Status of Ab Initio Predictions vs. Empirical Constraints. Symmetry (Basel) 2023. [DOI: 10.3390/sym15020450] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/10/2023] Open
Abstract
Infinite nuclear matter is a suitable laboratory to learn about nuclear forces in many-body systems. In particular, modern theoretical predictions of neutron-rich matter are timely because of recent and planned experiments aimed at constraining the equation of state of isospin-asymmetric matter. For these reasons, we have taken a broad look at the equation of state of neutron-rich matter and the closely related symmetry energy, which is the focal point of this article. Its density dependence is of paramount importance for a number of nuclear and astrophysical systems, ranging from neutron skins to the structure of neutron stars. We review and discuss ab initio predictions in relation to recent empirical constraints. We emphasize and demonstrate that free-space nucleon–nucleon data pose stringent constraints on the density dependence of the neutron matter equation of state, which essentially determines the slope of the symmetry energy at saturation.
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7
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Hu B, Jiang W, Miyagi T, Sun Z, Ekström A, Forssén C, Hagen G, Holt JD, Papenbrock T, Stroberg SR, Vernon I. Ab initio predictions link the neutron skin of 208Pb to nuclear forces. NATURE PHYSICS 2022; 18:1196-1200. [PMID: 36217363 PMCID: PMC9537109 DOI: 10.1038/s41567-022-01715-8] [Citation(s) in RCA: 8] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/23/2021] [Accepted: 07/11/2022] [Indexed: 05/14/2023]
Abstract
Heavy atomic nuclei have an excess of neutrons over protons, which leads to the formation of a neutron skin whose thickness is sensitive to details of the nuclear force. This links atomic nuclei to properties of neutron stars, thereby relating objects that differ in size by orders of magnitude. The nucleus 208Pb is of particular interest because it exhibits a simple structure and is experimentally accessible. However, computing such a heavy nucleus has been out of reach for ab initio theory. By combining advances in quantum many-body methods, statistical tools and emulator technology, we make quantitative predictions for the properties of 208Pb starting from nuclear forces that are consistent with symmetries of low-energy quantum chromodynamics. We explore 109 different nuclear force parameterizations via history matching, confront them with data in select light nuclei and arrive at an importance-weighted ensemble of interactions. We accurately reproduce bulk properties of 208Pb and determine the neutron skin thickness, which is smaller and more precise than a recent extraction from parity-violating electron scattering but in agreement with other experimental probes. This work demonstrates how realistic two- and three-nucleon forces act in a heavy nucleus and allows us to make quantitative predictions across the nuclear landscape.
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Affiliation(s)
- Baishan Hu
- TRIUMF, Vancouver, British Columbia Canada
| | - Weiguang Jiang
- Department of Physics, Chalmers University of Technology, Gothenburg, Sweden
| | - Takayuki Miyagi
- TRIUMF, Vancouver, British Columbia Canada
- Department of Physics, Technische Universität Darmstadt, Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - Zhonghao Sun
- Department of Physics and Astronomy, University of Tennessee, Knoxville, TN USA
- Physics Division, Oak Ridge National Laboratory, Oak Ridge, TN USA
| | - Andreas Ekström
- Department of Physics, Chalmers University of Technology, Gothenburg, Sweden
| | - Christian Forssén
- Department of Physics, Chalmers University of Technology, Gothenburg, Sweden
| | - Gaute Hagen
- TRIUMF, Vancouver, British Columbia Canada
- Department of Physics and Astronomy, University of Tennessee, Knoxville, TN USA
- Physics Division, Oak Ridge National Laboratory, Oak Ridge, TN USA
| | - Jason D. Holt
- TRIUMF, Vancouver, British Columbia Canada
- Department of Physics, McGill University, Montreal, Quebec Canada
| | - Thomas Papenbrock
- Department of Physics and Astronomy, University of Tennessee, Knoxville, TN USA
- Physics Division, Oak Ridge National Laboratory, Oak Ridge, TN USA
| | - S. Ragnar Stroberg
- Department of Physics, University of Washington, Seattle, WA USA
- Physics Division, Argonne National Laboratory, Lemont, IL USA
| | - Ian Vernon
- Department of Mathematical Sciences, Durham University, Durham, UK
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8
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Lourenço O, Lenzi C, Frederico T, Dutra M. Dark matter effects on tidal deformabilities and moment of inertia in a hadronic model with short-range correlations. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043010] [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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9
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Huth S, Pang PTH, Tews I, Dietrich T, Le Fèvre A, Schwenk A, Trautmann W, Agarwal K, Bulla M, Coughlin MW, Van Den Broeck C. Constraining neutron-star matter with microscopic and macroscopic collisions. Nature 2022; 606:276-280. [PMID: 35676430 PMCID: PMC9177417 DOI: 10.1038/s41586-022-04750-w] [Citation(s) in RCA: 11] [Impact Index Per Article: 5.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/13/2021] [Accepted: 04/11/2022] [Indexed: 11/16/2022]
Abstract
Interpreting high-energy, astrophysical phenomena, such as supernova explosions or neutron-star collisions, requires a robust understanding of matter at supranuclear densities. However, our knowledge about dense matter explored in the cores of neutron stars remains limited. Fortunately, dense matter is not probed only in astrophysical observations, but also in terrestrial heavy-ion collision experiments. Here we use Bayesian inference to combine data from astrophysical multi-messenger observations of neutron stars1-9 and from heavy-ion collisions of gold nuclei at relativistic energies10,11 with microscopic nuclear theory calculations12-17 to improve our understanding of dense matter. We find that the inclusion of heavy-ion collision data indicates an increase in the pressure in dense matter relative to previous analyses, shifting neutron-star radii towards larger values, consistent with recent observations by the Neutron Star Interior Composition Explorer mission5-8,18. Our findings show that constraints from heavy-ion collision experiments show a remarkable consistency with multi-messenger observations and provide complementary information on nuclear matter at intermediate densities. This work combines nuclear theory, nuclear experiment and astrophysical observations, and shows how joint analyses can shed light on the properties of neutron-rich supranuclear matter over the density range probed in neutron stars.
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Affiliation(s)
- Sabrina Huth
- Department of Physics, Technische Universität Darmstadt, Darmstadt, Germany.
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany.
| | - Peter T H Pang
- Nikhef, Amsterdam, The Netherlands.
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Utrecht, The Netherlands.
| | - Ingo Tews
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM, USA
| | - Tim Dietrich
- Institut für Physik und Astronomie, Universität Potsdam, Potsdam, Germany
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Potsdam, Germany
| | - Arnaud Le Fèvre
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
| | - Achim Schwenk
- Department of Physics, Technische Universität Darmstadt, Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany
- Max-Planck-Institut für Kernphysik, Heidelberg, Germany
| | | | - Kshitij Agarwal
- Physikalisches Institut, Eberhard Karls Universität Tübingen, Tübingen, Germany
| | - Mattia Bulla
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden
| | - Michael W Coughlin
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | - Chris Van Den Broeck
- Nikhef, Amsterdam, The Netherlands
- Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Utrecht, The Netherlands
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10
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Sobczyk JE, Roggero A. Spectral density reconstruction with Chebyshev polynomials. Phys Rev E 2022; 105:055310. [PMID: 35706316 DOI: 10.1103/physreve.105.055310] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/15/2021] [Accepted: 05/11/2022] [Indexed: 06/15/2023]
Abstract
Accurate calculations of the spectral density in a strongly correlated quantum many-body system are of fundamental importance to study its dynamics in the linear response regime. Typical examples are the calculation of inclusive and semiexclusive scattering cross sections in atomic nuclei and transport properties of nuclear and neutron star matter. Integral transform techniques play an important role in accessing the spectral density in a variety of nuclear systems. However, their accuracy is in practice limited by the need to perform a numerical inversion which is often ill-conditioned. In the present work we extend a recently proposed quantum algorithm which circumvents this problem. We show how to perform controllable reconstructions of the spectral density over a finite energy resolution with rigorous error estimates. An appropriate expansion in Chebyshev polynomials allows for efficient simulations also on classical computers. We apply our idea to obtain the local density of states for graphene in a magnetic field as a proof of principle. This paves the way for future applications in nuclear and condensed matter physics.
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Affiliation(s)
- Joanna E Sobczyk
- Institut für Kernphysik and PRISMA+ Cluster of Excellence, Johannes Gutenberg-Universität, 55128 Mainz, Germany
| | - Alessandro Roggero
- Physics Department, University of Trento, Via Sommarive 14, I-38123 Trento, Italy
- INFN-TIFPA Trento Institute of Fundamental Physics and Applications, Trento, Italy
- InQubator for Quantum Simulation (IQuS), Department of Physics, University of Washington, Seattle, Washington 98195, USA
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11
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Translating Neutron Star Observations to Nuclear Symmetry Energy via Deep Neural Networks. GALAXIES 2022. [DOI: 10.3390/galaxies10010016] [Citation(s) in RCA: 5] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/04/2023]
Abstract
One of the most significant challenges involved in efforts to understand the equation of state of dense neutron-rich matter is the uncertain density dependence of the nuclear symmetry energy. In particular, the nuclear symmetry energy is still rather poorly constrained, especially at high densities. On the other hand, detailed knowledge of the equation of state is critical for our understanding of many important phenomena in the nuclear terrestrial laboratories and the cosmos. Because of its broad impact, pinning down the density dependence of the nuclear symmetry energy has been a long-standing goal of both nuclear physics and astrophysics. Recent observations of neutron stars, in both electromagnetic and gravitational-wave spectra, have already constrained significantly the nuclear symmetry energy at high densities. The next generation of telescopes and gravitational-wave observatories will provide an unprecedented wealth of detailed observations of neutron stars, which will improve further our knowledge of the density dependence of nuclear symmetry energy, and the underlying equation of state of dense neutron-rich matter. Training deep neural networks to learn a computationally efficient representation of the mapping between astrophysical observables of neutron stars, such as masses, radii, and tidal deformabilities, and the nuclear symmetry energy allows its density dependence to be determined reliably and accurately. In this work, we use a deep learning approach to determine the nuclear symmetry energy as a function of density directly from observational neutron star data. We show, for the first time, that artificial neural networks can precisely reconstruct the nuclear symmetry energy from a set of available neutron star observables, such as masses and radii as measured by, e.g., the NICER mission, or masses and tidal deformabilities as measured by the LIGO/VIRGO/KAGRA gravitational-wave detectors. These results demonstrate the potential of artificial neural networks to reconstruct the symmetry energy and the equation of state directly from neutron star observational data, and emphasize the importance of the deep learning approach in the era of multi-messenger astrophysics.
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12
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Reinhard PG, Roca-Maza X, Nazarewicz W. Information Content of the Parity-Violating Asymmetry in ^{208}Pb. PHYSICAL REVIEW LETTERS 2021; 127:232501. [PMID: 34936797 DOI: 10.1103/physrevlett.127.232501] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/31/2021] [Accepted: 10/27/2021] [Indexed: 06/14/2023]
Abstract
The parity-violating asymmetry A_{PV} in ^{208}Pb, recently measured by the PREX-2 Collaboration, is studied using modern relativistic (covariant) and nonrelativistic energy density functionals. We first assess the theoretical uncertainty on A_{PV} which is intrinsic to the adopted approach. To this end, we use quantified functionals that are able to accommodate our previous knowledge on nuclear observables such as binding energies, charge radii, and the dipole polarizability α_{D} of ^{208}Pb. We then add the quantified value of A_{PV} together with α_{D} to our calibration dataset to optimize new functionals. Based on these results, we predict a neutron skin thickness in ^{208}Pb r_{skin}=0.19±0.02 fm and the symmetry-energy slope L=54±8 MeV. These values are consistent with other estimates based on astrophysical data and are significantly lower than those recently reported using a particular set of relativistic energy density functionals. We also make a prediction for the A_{PV} value in ^{48}Ca that will be soon available from the CREX measurement.
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Affiliation(s)
| | - Xavier Roca-Maza
- Dipartimento di Fisica "Aldo Pontremoli," Università degli Studi di Milano, 20133 Milano, Italy and INFN, Sezione di Milano, 20133 Milano, Italy
| | - Witold Nazarewicz
- Facility for Rare Isotope Beams and Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
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13
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Essick R, Tews I, Landry P, Schwenk A. Astrophysical Constraints on the Symmetry Energy and the Neutron Skin of ^{208}Pb with Minimal Modeling Assumptions. PHYSICAL REVIEW LETTERS 2021; 127:192701. [PMID: 34797158 DOI: 10.1103/physrevlett.127.192701] [Citation(s) in RCA: 10] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/21/2021] [Revised: 09/03/2021] [Accepted: 09/14/2021] [Indexed: 06/13/2023]
Abstract
The symmetry energy and its density dependence are crucial inputs for many nuclear physics and astrophysics applications, as they determine properties ranging from the neutron-skin thickness of nuclei to the crust thickness and the radius of neutron stars. Recently, PREX-II reported a value of 0.283±0.071 fm for the neutron-skin thickness of ^{208}Pb, implying a slope parameter L=106±37 MeV, larger than most ranges obtained from microscopic calculations and other nuclear experiments. We use a nonparametric equation of state representation based on Gaussian processes to constrain the symmetry energy S_{0}, L, and R_{skin}^{^{208}Pb} directly from observations of neutron stars with minimal modeling assumptions. The resulting astrophysical constraints from heavy pulsar masses, LIGO/Virgo, and NICER clearly favor smaller values of the neutron skin and L, as well as negative symmetry incompressibilities. Combining astrophysical data with PREX-II and chiral effective field theory constraints yields S_{0}=33.0_{-1.8}^{+2.0} MeV, L=53_{-15}^{+14} MeV, and R_{skin}^{^{208}Pb}=0.17_{-0.04}^{+0.04} fm.
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Affiliation(s)
- Reed Essick
- Perimeter Institute for Theoretical Physics, 31 Caroline Street North, Waterloo, Ontario, Canada N2L 2Y5
- Kavli Institute for Cosmological Physics, The University of Chicago, Chicago, Illinois 60637, USA
| | - Ingo Tews
- Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - Philippe Landry
- Gravitational-Wave Physics & Astronomy Center, California State University, Fullerton, 800 N State College Blvd, Fullerton, California 92831, USA
| | - Achim 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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14
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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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15
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Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817. UNIVERSE 2021. [DOI: 10.3390/universe7060182] [Citation(s) in RCA: 47] [Impact Index Per Article: 15.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
The density dependence of nuclear symmetry energy is among the most uncertain parts of the Equation of State (EOS) of dense neutron-rich nuclear matter. It is currently poorly known especially at suprasaturation densities partially because of our poor knowledge about isovector nuclear interactions at short distances. Because of its broad impacts on many interesting issues, pinning down the density dependence of nuclear symmetry energy has been a longstanding and shared goal of both astrophysics and nuclear physics. New observational data of neutron stars including their masses, radii, and tidal deformations since GW170817 have helped improve our knowledge about nuclear symmetry energy, especially at high densities. Based on various model analyses of these new data by many people in the nuclear astrophysics community, while our brief review might be incomplete and biased unintentionally, we learned in particular the following: (1) The slope parameter L of nuclear symmetry energy at saturation density ρ0 of nuclear matter from 24 new analyses of neutron star observables was about L≈57.7±19 MeV at a 68% confidence level, consistent with its fiducial value from surveys of over 50 earlier analyses of both terrestrial and astrophysical data within error bars. (2) The curvature Ksym of nuclear symmetry energy at ρ0 from 16 new analyses of neutron star observables was about Ksym≈−107±88 MeV at a 68% confidence level, in very good agreement with the systematics of earlier analyses. (3) The magnitude of nuclear symmetry energy at 2ρ0, i.e., Esym(2ρ0)≈51±13 MeV at a 68% confidence level, was extracted from nine new analyses of neutron star observables, consistent with the results from earlier analyses of heavy-ion reactions and the latest predictions of the state-of-the-art nuclear many-body theories. (4) While the available data from canonical neutron stars did not provide tight constraints on nuclear symmetry energy at densities above about 2ρ0, the lower radius boundary R2.01=12.2 km from NICER’s very recent observation of PSR J0740+6620 of mass 2.08±0.07M⊙ and radius R=12.2–16.3 km at a 68% confidence level set a tight lower limit for nuclear symmetry energy at densities above 2ρ0. (5) Bayesian inferences of nuclear symmetry energy using models encapsulating a first-order hadron–quark phase transition from observables of canonical neutron stars indicated that the phase transition shifted appreciably both L and Ksym to higher values, but with larger uncertainties compared to analyses assuming no such phase transition. (6) The high-density behavior of nuclear symmetry energy significantly affected the minimum frequency necessary to rotationally support GW190814’s secondary component of mass (2.50–2.67) M⊙ as the fastest and most massive pulsar discovered so far. Overall, thanks to the hard work of many people in the astrophysics and nuclear physics community, new data of neutron star observations since the discovery of GW170817 have significantly enriched our knowledge about the symmetry energy of dense neutron-rich nuclear matter.
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16
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Reed BT, Fattoyev FJ, Horowitz CJ, Piekarewicz J. Implications of PREX-2 on the Equation of State of Neutron-Rich Matter. PHYSICAL REVIEW LETTERS 2021; 126:172503. [PMID: 33988426 DOI: 10.1103/physrevlett.126.172503] [Citation(s) in RCA: 15] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/24/2021] [Accepted: 03/31/2021] [Indexed: 06/12/2023]
Abstract
Laboratory experiments sensitive to the equation of state of neutron rich matter in the vicinity of nuclear saturation density provide the first rung in a "density ladder" that connects terrestrial experiments to astronomical observations. In this context, the neutron skin thickness of ^{208}Pb (R_{skin}^{208}) provides a stringent laboratory constraint on the density dependence of the symmetry energy. In turn, an improved value of R_{skin}^{208} has been reported recently by the PREX collaboration. Exploiting the strong correlation between R_{skin}^{208} and the slope of the symmetry energy L within a specific class of relativistic energy density functionals, we report a value of L=(106±37) MeV-which systematically overestimates current limits based on both theoretical approaches and experimental measurements. The impact of such a stiff symmetry energy on some critical neutron-star observables is also examined.
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Affiliation(s)
- Brendan T Reed
- Department of Astronomy, Indiana University, Bloomington, Indiana 47405, USA
- Center for Exploration of Energy and Matter and Department of Physics, Indiana University, Bloomington, Indiana 47405, USA
| | - F J Fattoyev
- Department of Physics, Manhattan College, Riverdale, New York 10471, USA
| | - C J Horowitz
- Center for Exploration of Energy and Matter and Department of Physics, Indiana University, Bloomington, Indiana 47405, USA
| | - J Piekarewicz
- Department of Physics, Florida State University, Tallahassee, Florida 32306, USA
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17
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Adhikari D, Albataineh H, Androic D, Aniol K, Armstrong DS, Averett T, Ayerbe Gayoso C, Barcus S, Bellini V, Beminiwattha RS, Benesch JF, Bhatt H, Bhatta Pathak D, Bhetuwal D, Blaikie B, Campagna Q, Camsonne A, Cates GD, Chen Y, Clarke C, Cornejo JC, Covrig Dusa S, Datta P, Deshpande A, Dutta D, Feldman C, Fuchey E, Gal C, Gaskell D, Gautam T, Gericke M, Ghosh C, Halilovic I, Hansen JO, Hauenstein F, Henry W, Horowitz CJ, Jantzi C, Jian S, Johnston S, Jones DC, Karki B, Katugampola S, Keppel C, King PM, King DE, Knauss M, Kumar KS, Kutz T, Lashley-Colthirst N, Leverick G, Liu H, Liyange N, Malace S, Mammei R, Mammei J, McCaughan M, McNulty D, Meekins D, Metts C, Michaels R, Mondal MM, Napolitano J, Narayan A, Nikolaev D, Rashad MNH, Owen V, Palatchi C, Pan J, Pandey B, Park S, Paschke KD, Petrusky M, Pitt ML, Premathilake S, Puckett AJR, Quinn B, Radloff R, Rahman S, Rathnayake A, Reed BT, Reimer PE, Richards R, Riordan S, Roblin Y, Seeds S, Shahinyan A, Souder P, Tang L, Thiel M, Tian Y, Urciuoli GM, Wertz EW, Wojtsekhowski B, Yale B, Ye T, Yoon A, Zec A, Zhang W, Zhang J, Zheng X. Accurate Determination of the Neutron Skin Thickness of ^{208}Pb through Parity-Violation in Electron Scattering. PHYSICAL REVIEW LETTERS 2021; 126:172502. [PMID: 33988387 DOI: 10.1103/physrevlett.126.172502] [Citation(s) in RCA: 31] [Impact Index Per Article: 10.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/22/2021] [Accepted: 03/22/2021] [Indexed: 06/12/2023]
Abstract
We report a precision measurement of the parity-violating asymmetry A_{PV} in the elastic scattering of longitudinally polarized electrons from ^{208}Pb. We measure A_{PV}=550±16(stat)±8(syst) parts per billion, leading to an extraction of the neutral weak form factor F_{W}(Q^{2}=0.00616 GeV^{2})=0.368±0.013. Combined with our previous measurement, the extracted neutron skin thickness is R_{n}-R_{p}=0.283±0.071 fm. The result also yields the first significant direct measurement of the interior weak density of ^{208}Pb: ρ_{W}^{0}=-0.0796±0.0036(exp)±0.0013(theo) fm^{-3} leading to the interior baryon density ρ_{b}^{0}=0.1480±0.0036(exp)±0.0013(theo) fm^{-3}. The measurement accurately constrains the density dependence of the symmetry energy of nuclear matter near saturation density, with implications for the size and composition of neutron stars.
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Affiliation(s)
- D Adhikari
- Idaho State University, Pocatello, ID 83209, USA
| | - H Albataineh
- Texas A & M University-Kingsville, Kingsville, TX 78363, USA
| | - D Androic
- University of Zagreb, Faculty of Science
| | - K Aniol
- California State University, Los Angeles, Los Angeles, California 90032, USA
| | | | - T Averett
- William & Mary, Williamsburg, Virginia 23185, USA
| | | | - S Barcus
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - V Bellini
- Istituto Nazionale di Fisica Nucleare, Sezione di Catania, 95123 Catania, Italy
| | | | - J F Benesch
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - H Bhatt
- Mississippi State University, Mississippi State, MS 39762, USA
| | | | - D Bhetuwal
- Mississippi State University, Mississippi State, MS 39762, USA
| | - B Blaikie
- University of Manitoba, Winnipeg, MB R3T2N2 Canada
| | - Q Campagna
- William & Mary, Williamsburg, Virginia 23185, USA
| | - A Camsonne
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - G D Cates
- University of Virginia, Charlottesville, VA 22904, USA
| | - Y Chen
- Louisiana Tech University, Ruston, LA 71272 USA
| | - C Clarke
- Stony Brook, State University of New York, NY 11794, USA
| | - J C Cornejo
- Carnegie Mellon University, Pittsburgh, Pennsylvania 15213, USA
| | - S Covrig Dusa
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - P Datta
- University of Connecticut, Storrs, CT 06269, USA
| | - A Deshpande
- Stony Brook, State University of New York, NY 11794, USA
- Center for Frontiers in Nuclear Science, NY 11794, USA
| | - D Dutta
- Mississippi State University, Mississippi State, MS 39762, USA
| | - C Feldman
- Stony Brook, State University of New York, NY 11794, USA
| | - E Fuchey
- University of Connecticut, Storrs, CT 06269, USA
| | - C Gal
- University of Virginia, Charlottesville, VA 22904, USA
- Stony Brook, State University of New York, NY 11794, USA
- Center for Frontiers in Nuclear Science, NY 11794, USA
| | - D Gaskell
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - T Gautam
- Hampton University, Hampton, Virginia 23668, USA
| | - M Gericke
- University of Manitoba, Winnipeg, MB R3T2N2 Canada
| | - C Ghosh
- Stony Brook, State University of New York, NY 11794, USA
- University of Massachusetts Amherst, Amherst, Massachusetts 01003, USA
| | - I Halilovic
- University of Manitoba, Winnipeg, MB R3T2N2 Canada
| | - J-O Hansen
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - F Hauenstein
- Old Dominion University, Norfolk, Virginia 23529, USA
| | - W Henry
- Temple University, Philadelphia, PA 19122, USA
| | - C J Horowitz
- Indiana University, Bloomington, Indiana 47405, USA
| | - C Jantzi
- University of Virginia, Charlottesville, VA 22904, USA
| | - S Jian
- University of Virginia, Charlottesville, VA 22904, USA
| | - S Johnston
- University of Massachusetts Amherst, Amherst, Massachusetts 01003, USA
| | - D C Jones
- Temple University, Philadelphia, PA 19122, USA
| | - B Karki
- Ohio University, Athens, Ohio 45701, USA
| | - S Katugampola
- University of Virginia, Charlottesville, VA 22904, USA
| | - C Keppel
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - P M King
- Ohio University, Athens, Ohio 45701, USA
| | - D E King
- Syracuse University, Syracuse, New York 13244, USA
| | - M Knauss
- Duquesne University, 600 Forbes Avenue, Pittsburgh, PA 15282, USA
| | - K S Kumar
- University of Massachusetts Amherst, Amherst, Massachusetts 01003, USA
| | - T Kutz
- Stony Brook, State University of New York, NY 11794, USA
| | | | - G Leverick
- University of Manitoba, Winnipeg, MB R3T2N2 Canada
| | - H Liu
- University of Massachusetts Amherst, Amherst, Massachusetts 01003, USA
| | - N Liyange
- University of Virginia, Charlottesville, VA 22904, USA
| | - S Malace
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - R Mammei
- University of Winnipeg, Winnipeg, MB R3B2E9 Canada
| | - J Mammei
- University of Manitoba, Winnipeg, MB R3T2N2 Canada
| | - M McCaughan
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - D McNulty
- Idaho State University, Pocatello, ID 83209, USA
| | - D Meekins
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - C Metts
- William & Mary, Williamsburg, Virginia 23185, USA
| | - R Michaels
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - M M Mondal
- Stony Brook, State University of New York, NY 11794, USA
- Center for Frontiers in Nuclear Science, NY 11794, USA
| | | | | | - D Nikolaev
- Temple University, Philadelphia, PA 19122, USA
| | - M N H Rashad
- Old Dominion University, Norfolk, Virginia 23529, USA
| | - V Owen
- William & Mary, Williamsburg, Virginia 23185, USA
| | - C Palatchi
- University of Virginia, Charlottesville, VA 22904, USA
- Center for Frontiers in Nuclear Science, NY 11794, USA
| | - J Pan
- University of Manitoba, Winnipeg, MB R3T2N2 Canada
| | - B Pandey
- Hampton University, Hampton, Virginia 23668, USA
| | - S Park
- Stony Brook, State University of New York, NY 11794, USA
| | - K D Paschke
- University of Virginia, Charlottesville, VA 22904, USA
| | - M Petrusky
- Stony Brook, State University of New York, NY 11794, USA
| | - M L Pitt
- Virginia Tech, Blacksburg, Virginia 24061, USA
| | | | | | - B Quinn
- Carnegie Mellon University, Pittsburgh, Pennsylvania 15213, USA
| | - R Radloff
- Ohio University, Athens, Ohio 45701, USA
| | - S Rahman
- University of Manitoba, Winnipeg, MB R3T2N2 Canada
| | - A Rathnayake
- University of Virginia, Charlottesville, VA 22904, USA
| | - B T Reed
- Indiana University, Bloomington, Indiana 47405, USA
| | - P E Reimer
- Physics Division, Argonne National Laboratory, Lemont, Il 60439
| | - R Richards
- Stony Brook, State University of New York, NY 11794, USA
| | - S Riordan
- Physics Division, Argonne National Laboratory, Lemont, Il 60439
| | - Y Roblin
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - S Seeds
- University of Connecticut, Storrs, CT 06269, USA
| | - A Shahinyan
- A. I. Alikhanyan National Science Laboratory (Yerevan Physics Institute), Yerevan 0036, Armenia
| | - P Souder
- Syracuse University, Syracuse, New York 13244, USA
| | - L Tang
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
- Hampton University, Hampton, Virginia 23668, USA
| | - M Thiel
- Institut für Kernphysik, Johannes Gutenberg-Universität, Mainz 55122, Germany
| | - Y Tian
- Syracuse University, Syracuse, New York 13244, USA
| | | | - E W Wertz
- William & Mary, Williamsburg, Virginia 23185, USA
| | - B Wojtsekhowski
- Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606, USA
| | - B Yale
- William & Mary, Williamsburg, Virginia 23185, USA
| | - T Ye
- Stony Brook, State University of New York, NY 11794, USA
| | - A Yoon
- Christopher Newport University, Newport News, Virginia 23606, USA
| | - A Zec
- University of Virginia, Charlottesville, VA 22904, USA
| | - W Zhang
- Stony Brook, State University of New York, NY 11794, USA
| | - J Zhang
- Stony Brook, State University of New York, NY 11794, USA
- Center for Frontiers in Nuclear Science, NY 11794, USA
- Shandong University, Qingdao, Shandong 266237, China
| | - X Zheng
- University of Virginia, Charlottesville, VA 22904, USA
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18
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Abstract
Background: We analyze several constraints on the nuclear equation of state (EOS) currently available from neutron star (NS) observations and laboratory experiments and study the existence of possible correlations among properties of nuclear matter at saturation density with NS observables. Methods: We use a set of different models that include several phenomenological EOSs based on Skyrme and relativistic mean field models as well as microscopic calculations based on different many-body approaches, i.e., the (Dirac–)Brueckner–Hartree–Fock theories, Quantum Monte Carlo techniques, and the variational method. Results: We find that almost all the models considered are compatible with the laboratory constraints of the nuclear matter properties as well as with the largest NS mass observed up to now, 2.14−0.09+0.10M⊙ for the object PSR J0740+6620, and with the upper limit of the maximum mass of about 2.3–2.5M⊙ deduced from the analysis of the GW170817 NS merger event. Conclusion: Our study shows that whereas no correlation exists between the tidal deformability and the value of the nuclear symmetry energy at saturation for any value of the NS mass, very weak correlations seem to exist with the derivative of the nuclear symmetry energy and with the nuclear incompressibility.
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