1
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Elhatisari S, Bovermann L, Ma YZ, Epelbaum E, Frame D, Hildenbrand F, Kim M, Kim Y, Krebs H, Lähde TA, Lee D, Li N, Lu BN, Meißner UG, Rupak G, Shen S, Song YH, Stellin G. Wavefunction matching for solving quantum many-body problems. Nature 2024; 630:59-63. [PMID: 38750357 PMCID: PMC11153134 DOI: 10.1038/s41586-024-07422-z] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/23/2022] [Accepted: 04/15/2024] [Indexed: 06/07/2024]
Abstract
Ab initio calculations have an essential role in our fundamental understanding of quantum many-body systems across many subfields, from strongly correlated fermions1-3 to quantum chemistry4-6 and from atomic and molecular systems7-9 to nuclear physics10-14. One of the primary challenges is to perform accurate calculations for systems where the interactions may be complicated and difficult for the chosen computational method to handle. Here we address the problem by introducing an approach called wavefunction matching. Wavefunction matching transforms the interaction between particles so that the wavefunctions up to some finite range match that of an easily computable interaction. This allows for calculations of systems that would otherwise be impossible owing to problems such as Monte Carlo sign cancellations. We apply the method to lattice Monte Carlo simulations15,16 of light nuclei, medium-mass nuclei, neutron matter and nuclear matter. We use high-fidelity chiral effective field theory interactions17,18 and find good agreement with empirical data. These results are accompanied by insights on the nuclear interactions that may help to resolve long-standing challenges in accurately reproducing nuclear binding energies, charge radii and nuclear-matter saturation in ab initio calculations19,20.
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Affiliation(s)
- Serdar Elhatisari
- Faculty of Natural Sciences and Engineering, Gaziantep Islam Science and Technology University, Gaziantep, Turkey
- Helmholtz-Institut für Strahlen- und Kernphysik and Bethe Center for Theoretical Physics, Universität Bonn, Bonn, Germany
| | - Lukas Bovermann
- Institut für Theoretische Physik II, Ruhr-Universität Bochum, Bochum, Germany
| | - Yuan-Zhuo Ma
- Facility for Rare Isotope Beams and Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA
- Guangdong Provincial Key Laboratory of Nuclear Science, Institute of Quantum Matter, South China Normal University, Guangzhou, China
| | - Evgeny Epelbaum
- Institut für Theoretische Physik II, Ruhr-Universität Bochum, Bochum, Germany
| | - Dillon Frame
- Institut für Kernphysik, Institute for Advanced Simulation, Jülich Center for Hadron Physics, Jülich, Germany
- Center for Advanced Simulation and Analytics (CASA), Forschungszentrum Jülich, Jülich, Germany
| | - Fabian Hildenbrand
- Institut für Kernphysik, Institute for Advanced Simulation, Jülich Center for Hadron Physics, Jülich, Germany
- Center for Advanced Simulation and Analytics (CASA), Forschungszentrum Jülich, Jülich, Germany
| | - Myungkuk Kim
- Center for Exotic Nuclear Studies, Institute for Basic Science, Daejeon, Korea
| | - Youngman Kim
- Center for Exotic Nuclear Studies, Institute for Basic Science, Daejeon, Korea
| | - Hermann Krebs
- Institut für Theoretische Physik II, Ruhr-Universität Bochum, Bochum, Germany
| | - Timo A Lähde
- Institut für Kernphysik, Institute for Advanced Simulation, Jülich Center for Hadron Physics, Jülich, Germany
- Center for Advanced Simulation and Analytics (CASA), Forschungszentrum Jülich, Jülich, Germany
| | - Dean Lee
- Facility for Rare Isotope Beams and Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA.
| | - Ning Li
- School of Physics, Sun Yat-Sen University, Guangzhou, China
| | - Bing-Nan Lu
- Graduate School of China Academy of Engineering Physics, Beijing, China
| | - Ulf-G Meißner
- Helmholtz-Institut für Strahlen- und Kernphysik and Bethe Center for Theoretical Physics, Universität Bonn, Bonn, Germany
- Institut für Kernphysik, Institute for Advanced Simulation, Jülich Center for Hadron Physics, Jülich, Germany
- Center for Advanced Simulation and Analytics (CASA), Forschungszentrum Jülich, Jülich, Germany
- Tbilisi State University, Tbilisi, Georgia
| | - Gautam Rupak
- Department of Physics and Astronomy and HPC2 Center for Computational Sciences, Mississippi State University, Mississippi State, MI, USA
| | - Shihang Shen
- Institut für Kernphysik, Institute for Advanced Simulation, Jülich Center for Hadron Physics, Jülich, Germany
- Center for Advanced Simulation and Analytics (CASA), Forschungszentrum Jülich, Jülich, Germany
| | - Young-Ho Song
- Institute for Rare Isotope Science, Institute for Basic Science (IBS), Daejeon, Korea
| | - Gianluca Stellin
- ESNT, DRF/IRFU/DPhN/LENA, CEA Paris-Saclay and Université Paris-Saclay, Gif-sur-Yvette, France
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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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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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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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5
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Raithel CA, Most ER. Degeneracy in the Inference of Phase Transitions in the Neutron Star Equation of State from Gravitational Wave Data. PHYSICAL REVIEW LETTERS 2023; 130:201403. [PMID: 37267559 DOI: 10.1103/physrevlett.130.201403] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/08/2022] [Revised: 12/19/2022] [Accepted: 04/10/2023] [Indexed: 06/04/2023]
Abstract
Gravitational wave (GW) detections of binary neutron star inspirals will be crucial for constraining the dense matter equation of state (EOS). We demonstrate a new degeneracy in the mapping from tidal deformability data to the EOS, which occurs for models with strong phase transitions. We find that there exists a new family of EOS with phase transitions that set in at different densities and that predict neutron star radii that differ by up to ∼500 m but that produce nearly identical tidal deformabilities for all neutron star masses. Next-generation GW detectors and advances in nuclear theory may be needed to resolve this degeneracy.
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Affiliation(s)
- Carolyn A Raithel
- School of Natural Sciences, Institute for Advanced Study, 1 Einstein Drive, Princeton, New Jersey 08540, USA; Princeton Center for Theoretical Science, Jadwin Hall, Princeton University, Princeton, New Jersey 08544, USA and Princeton Gravity Initiative, Jadwin Hall, Princeton University, Princeton, New Jersey 08544, USA
| | - Elias R Most
- School of Natural Sciences, Institute for Advanced Study, 1 Einstein Drive, Princeton, New Jersey 08540, USA; Princeton Center for Theoretical Science, Jadwin Hall, Princeton University, Princeton, New Jersey 08544, USA and Princeton Gravity Initiative, Jadwin Hall, Princeton University, Princeton, New Jersey 08544, USA
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6
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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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7
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Fujimoto Y, Fukushima K, Hotokezaka K, Kyutoku K. Gravitational Wave Signal for Quark Matter with Realistic Phase Transition. PHYSICAL REVIEW LETTERS 2023; 130:091404. [PMID: 36930907 DOI: 10.1103/physrevlett.130.091404] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/17/2022] [Revised: 12/21/2022] [Accepted: 02/09/2023] [Indexed: 06/18/2023]
Abstract
The cores of neutron stars (NSs) near the maximum mass can realize a transitional change to quark matter (QM). Gravitational waves from binary NS mergers are expected to convey information about the equation of state (EOS) sensitive to the QM transition. Here, we present the first results of gravitational wave simulation with the realistic EOS that is consistent with ab initio approaches of χEFT and pQCD and is assumed to go through smooth crossover. We compare them to results obtained with another EOS with a first-order hadron-quark phase transition. Our results suggest that early collapse to a black hole in the post-merger stage after NS merger robustly signifies softening of the EOS associated with the QM onset in the crossover scenario. The nature of the hadron-quark phase transition can be further constrained by the condition that electromagnetic counterparts should be energized by the material left outside the remnant black hole.
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Affiliation(s)
- Yuki Fujimoto
- Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
- Institute for Nuclear Theory, University of Washington, Seattle, Washington 98195, USA
| | - Kenji Fukushima
- Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan
| | - Kenta Hotokezaka
- Research Center for the Early Universe (RESCEU), The University of Tokyo, Tokyo 113-0033, Japan
| | - Koutarou Kyutoku
- Department of Physics, Kyoto University, Kyoto 606-8502, Japan
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
- Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS), RIKEN, Saitama 351-0198, Japan
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8
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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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9
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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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10
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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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11
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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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12
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Komoltsev O, Kurkela A. How Perturbative QCD Constrains the Equation of State at Neutron-Star Densities. PHYSICAL REVIEW LETTERS 2022; 128:202701. [PMID: 35657894 DOI: 10.1103/physrevlett.128.202701] [Citation(s) in RCA: 8] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/22/2021] [Revised: 03/14/2022] [Accepted: 04/25/2022] [Indexed: 06/15/2023]
Abstract
We demonstrate in a general and analytic way how high-density information about the equation of state (EOS) of strongly interacting matter obtained using perturbative quantum chromodynamics constrains the same EOS at densities reachable in physical neutron stars. Our approach is based on utilizing the full information of the thermodynamic potentials at the high-density limit together with thermodynamic stability and causality. This requires considering the pressure as a function of chemical potential p(μ) instead of the commonly used pressure as a function of energy density p(ε). The results can be used to propagate the perturbative quantum chromodynamics calculations reliable around 40n_{s} to lower densities in the most conservative way possible. We constrain the EOS starting from only a few times the nuclear saturation density n≳2.2n_{s}, and at n=5n_{s} we exclude at least 65% of otherwise allowed area in the ε-p plane. This provides information complementary to astrophysical observations that should be taken into account in any complete statistical inference study of the EOS. These purely theoretical results are independent of astrophysical neutron-star input, and hence, they can also be used to test theories of modified gravity and beyond the standard model physics in neutron stars.
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Affiliation(s)
- 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
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13
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The Equation of State of Neutron-Rich Matter at Fourth Order of Chiral Effective Field Theory and the Radius of a Medium-Mass Neutron Star. UNIVERSE 2022. [DOI: 10.3390/universe8020133] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
We report neutron star predictions based on our most recent equations of state. These are derived from chiral effective field theory, which allows for a systematic development of nuclear forces, order by order. We utilize high-quality two-nucleon interactions and include all three-nucleon forces up to fourth order in the chiral expansion. Our ab initio predictions are restricted to the domain of applicability of chiral effective field theory. However, stellar matter in the interior of neutron stars can be up to several times denser than normal nuclear matter at saturation, and its composition is essentially unknown. Following established practices, we extend our microscopic predictions to higher densities matching piecewise polytropes. The radius of the average-size neutron star, about 1.4 solar masses, is sensitive to the pressure at normal densities, and thus it is suitable to constrain ab initio theories of the equation of state. For this reason, we focus on the radius of medium-mass stars. We compare our results with other theoretical predictions and recent constraints.
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14
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Järvinen M. Holographic dense QCD in the Veneziano limit. EPJ WEB OF CONFERENCES 2022. [DOI: 10.1051/epjconf/202227408006] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/24/2022] Open
Abstract
Solving the properties of dense QCD matter is an extremely challenging problem because standard theoretical tools do not work at intermediate densities. The gauge/gravity duality may help to provide answers in this region. I give a brief review of recent progress in this field, focusing on the V-QCD model, which is one of the most sophisticated holographic models of QCD. I discuss predictions for the phase diagram, the equation of state, and properties of baryons. I apply these results to analyze the properties of neutron stars and to quark matter production in neutron star mergers.
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15
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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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16
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Whitehead TR, Lim Y, Holt JW. Global Microscopic Description of Nucleon-Nucleus Scattering with Quantified Uncertainties. PHYSICAL REVIEW LETTERS 2021; 127:182502. [PMID: 34767381 DOI: 10.1103/physrevlett.127.182502] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/18/2020] [Revised: 08/25/2021] [Accepted: 09/28/2021] [Indexed: 06/13/2023]
Abstract
We develop for the first time a microscopic global nucleon-nucleus optical potential with quantified uncertainties suitable for analyzing nuclear reaction experiments at next-generation rare-isotope beam facilities. Within the improved local density approximation and without any adjustable parameters, we begin by computing proton-nucleus and neutron-nucleus optical potentials from a set of five nuclear forces from chiral effective field theory for 1800 target nuclei in the mass range 12≤A≤242 for energies between 0 MeV<E≲150 MeV. We then parameterize a global optical potential for each chiral force that depends smoothly on the projectile energy as well as the target nucleus mass number and isospin asymmetry. Uncertainty bands for elastic scattering observables are generated from a full covariance analysis of the parameters entering in the description of our global optical potential and benchmarked against existing experimental data for stable target nuclei. Since our approach is purely microscopic, we anticipate a similar quality of the model for nucleon scattering on unstable isotopes.
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Affiliation(s)
- T R Whitehead
- Cyclotron Institute, Texas A&M University, College Station, Texas 77843, USA
- Department of Physics and Astronomy, Texas A&M University, College Station, Texas 77843, USA
- Facility for Rare Isotope Beams, Michigan State University, Michigan 48824, USA
| | - Y Lim
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
- Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
- Department of Science Education, Ewha Womans University, Seoul 120-750, Korea
| | - J W Holt
- Cyclotron Institute, Texas A&M University, College Station, Texas 77843, USA
- Department of Physics and Astronomy, Texas A&M University, College Station, Texas 77843, USA
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17
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Abstract
I review the issues related to the appearance of hyperons in neutron star matter, focusing in particular on the problem of the maximum mass supported by hyperonic equations of state. I discuss the general mechanism that leads to the formation of hyperons in the core of neutron stars and I review the main techniques and many-body methods used to construct an appropriate equation of state to describe the strongly interacting system of hadrons hosted in the core of neutron stars. I outline the consequences on the structure and internal composition of neutron stars and also discuss the possible signatures of the presence of hyperons in astrophysical dynamical systems like supernova explosions and binary neutron star mergers. Finally, I briefly report about the possible important role played by hyperons in the transport properties of neutron star matter and on the consequences of neutron star cooling and gravitational wave instabilities induced by the presence of hyperons.
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18
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Abstract
The effective Gogny interactions of the D1 family were established by D. Gogny more than forty years ago with the aim to describe simultaneously the mean field and the pairing field corresponding to the nuclear interaction. The most popular Gogny parametrizations, namely D1S, D1N and D1M, describe accurately the ground-state properties of spherical and deformed finite nuclei all across the mass table obtained with Hartree–Fock–Bogoliubov (HFB) calculations. However, these forces produce a rather soft equation of state (EoS) in neutron matter, which leads to predict maximum masses of neutron stars well below the observed value of two solar masses. To remove this limitation, we built new Gogny parametrizations by modifying the density dependence of the symmetry energy predicted by the force in such a way that they can be applied to the neutron star domain and can also reproduce the properties of finite nuclei as good as their predecessors. These new parametrizations allow us to obtain stiffer EoS’s based on the Gogny interactions, which predict maximum masses of neutron stars around two solar masses. Moreover, other global properties of the star, such as the moment of inertia and the tidal deformability, are in harmony with those obtained with other well tested EoSs based on the SLy4 Skyrme force or the Barcelona–Catania–Paris–Madrid (BCPM) energy density functional. Properties of the core-crust transition predicted by these Gogny EoSs are also analyzed. Using these new Gogny forces, the EoS in the inner crust is obtained with the Wigner–Seitz approximation in the Variational Wigner–Kirkwood approach along with the Strutinsky integral method, which allows one to estimate in a perturbative way the proton shell and pairing corrections. For the outer crust, the EoS is determined basically by the nuclear masses, which are taken from the experiments, wherever they are available, or by HFB calculations performed with these new forces if the experimental masses are not known.
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19
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Brady J, Wen P, Holt JW. Normalizing Flows for Microscopic Many-Body Calculations: An Application to the Nuclear Equation of State. PHYSICAL REVIEW LETTERS 2021; 127:062701. [PMID: 34420311 DOI: 10.1103/physrevlett.127.062701] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/08/2021] [Revised: 05/21/2021] [Accepted: 06/29/2021] [Indexed: 06/13/2023]
Abstract
Normalizing flows are a class of machine learning models used to construct a complex distribution through a bijective mapping of a simple base distribution. We demonstrate that normalizing flows are particularly well suited as a Monte Carlo integration framework for quantum many-body calculations that require the repeated evaluation of high-dimensional integrals across smoothly varying integrands and integration regions. As an example, we consider the finite-temperature nuclear equation of state. An important advantage of normalizing flows is the ability to build highly expressive models of the target integrand, which we demonstrate enables precise evaluations of the nuclear free energy and its derivatives. Furthermore, we show that a normalizing flow model trained on one target integrand can be used to efficiently calculate related integrals when the temperature, density, or nuclear force is varied. This work will support future efforts to build microscopic equations of state for numerical simulations of supernovae and neutron star mergers that employ state-of-the-art nuclear forces and many-body methods.
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Affiliation(s)
- Jack Brady
- Texas A&M University, College Station, Texas 77843, USA
| | - Pengsheng Wen
- Cyclotron Institute, Texas A&M University, College Station, Texas 77843, USA
- Department of Physics and Astronomy, Texas A&M University, College Station, Texas 77843, USA
| | - Jeremy W Holt
- Cyclotron Institute, Texas A&M University, College Station, Texas 77843, USA
- Department of Physics and Astronomy, Texas A&M University, College Station, Texas 77843, USA
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20
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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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21
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Stroberg SR, Holt JD, Schwenk A, Simonis J. Ab Initio Limits of Atomic Nuclei. PHYSICAL REVIEW LETTERS 2021; 126:022501. [PMID: 33512176 DOI: 10.1103/physrevlett.126.022501] [Citation(s) in RCA: 19] [Impact Index Per Article: 6.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/25/2019] [Revised: 10/05/2020] [Accepted: 11/18/2020] [Indexed: 06/12/2023]
Abstract
We predict the limits of existence of atomic nuclei, the proton and neutron drip lines, from the light through medium-mass regions. Starting from a chiral two- and three-nucleon interaction with good saturation properties, we use the valence-space in-medium similarity renormalization group to calculate ground-state and separation energies from helium to iron, nearly 700 isotopes in total. We use the available experimental data to quantify the theoretical uncertainties for our ab initio calculations towards the drip lines. Where the drip lines are known experimentally, our predictions are consistent within the estimated uncertainty. For the neutron-rich sodium to chromium isotopes, we provide predictions to be tested at rare-isotope beam facilities.
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Affiliation(s)
- S R Stroberg
- Department of Physics, University of Washington, Seattle, Washington 98195, USA
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
| | - J D Holt
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics, McGill University, 3600 Rue University, Montréal, Quebec H3A 2T8, Canada
| | - A Schwenk
- Institut für Kernphysik, Technische Universität Darmstadt, 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
| | - J Simonis
- Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
- Institut für Kernphysik and PRISMA Cluster of Excellence, Johannes Gutenberg-Universität, 55099 Mainz, Germany
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22
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Drischler C, Furnstahl RJ, Melendez JA, Phillips DR. How Well Do We Know the Neutron-Matter Equation of State at the Densities Inside Neutron Stars? A Bayesian Approach with Correlated Uncertainties. PHYSICAL REVIEW LETTERS 2020; 125:202702. [PMID: 33258658 DOI: 10.1103/physrevlett.125.202702] [Citation(s) in RCA: 17] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/25/2020] [Revised: 07/28/2020] [Accepted: 09/25/2020] [Indexed: 06/12/2023]
Abstract
We introduce a new framework for quantifying correlated uncertainties of the infinite-matter equation of state derived from chiral effective field theory (χEFT). Bayesian machine learning via Gaussian processes with physics-based hyperparameters allows us to efficiently quantify and propagate theoretical uncertainties of the equation of state, such as χEFT truncation errors, to derived quantities. We apply this framework to state-of-the-art many-body perturbation theory calculations with nucleon-nucleon and three-nucleon interactions up to fourth order in the χEFT expansion. This produces the first statistically robust uncertainty estimates for key quantities of neutron stars. We give results up to twice nuclear saturation density for the energy per particle, pressure, and speed of sound of neutron matter, as well as for the nuclear symmetry energy and its derivative. At nuclear saturation density, the predicted symmetry energy and its slope are consistent with experimental constraints.
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Affiliation(s)
- C Drischler
- Department of Physics, University of California, Berkeley, California 94720, USA
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
| | - R J Furnstahl
- Department of Physics, The Ohio State University, Columbus, Ohio 43210, USA
| | - J A Melendez
- Department of Physics, The Ohio State University, Columbus, Ohio 43210, USA
| | - D R Phillips
- Department of Physics and Astronomy and Institute of Nuclear and Particle Physics, Ohio University, Athens, Ohio 45701, USA
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23
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Leonhardt M, Pospiech M, Schallmo B, Braun J, Drischler C, Hebeler K, Schwenk A. Symmetric Nuclear Matter from the Strong Interaction. PHYSICAL REVIEW LETTERS 2020; 125:142502. [PMID: 33064516 DOI: 10.1103/physrevlett.125.142502] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/22/2019] [Revised: 06/12/2020] [Accepted: 08/10/2020] [Indexed: 06/11/2023]
Abstract
We study the equation of state of symmetric nuclear matter at zero temperature over a wide range of densities using two complementary theoretical approaches. At low densities, up to twice nuclear saturation density, we compute the energy per particle based on modern nucleon-nucleon and three-nucleon interactions derived within chiral effective field theory. For higher densities, we derive for the first time constraints in a Fierz-complete setting directly based on quantum chromodynamics using functional renormalization group techniques. We find remarkable consistency of the results obtained from both approaches as they come together in density and the natural emergence of a maximum in the speed of sound c_{S} at supranuclear densities. The presence of this maximum appears tightly connected to the formation of a diquark gap. Notably, this maximum is observed to exceed the asymptotic value c_{S}^{2}=1/3 while its exact position in terms of the density cannot yet be determined conclusively.
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Affiliation(s)
- M Leonhardt
- Institut für Kernphysik, Technische Universität Darmstadt, D-64289 Darmstadt, Germany
| | - M Pospiech
- Institut für Kernphysik, Technische Universität Darmstadt, D-64289 Darmstadt, Germany
| | - B Schallmo
- Institut für Kernphysik, Technische Universität Darmstadt, D-64289 Darmstadt, Germany
| | - J Braun
- Institut für Kernphysik, Technische Universität Darmstadt, D-64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, D-64291 Darmstadt, Germany
| | - C Drischler
- Department of Physics, University of California, Berkeley, California 94720, USA
- Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
| | - K Hebeler
- Institut für Kernphysik, Technische Universität Darmstadt, D-64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, D-64291 Darmstadt, Germany
| | - A Schwenk
- Institut für Kernphysik, Technische Universität Darmstadt, D-64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, D-64291 Darmstadt, Germany
- Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
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24
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Yao JM, Bally B, Engel J, Wirth R, Rodríguez TR, Hergert H. Ab Initio Treatment of Collective Correlations and the Neutrinoless Double Beta Decay of ^{48}Ca. PHYSICAL REVIEW LETTERS 2020; 124:232501. [PMID: 32603157 DOI: 10.1103/physrevlett.124.232501] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/20/2019] [Revised: 02/04/2020] [Accepted: 05/06/2020] [Indexed: 06/11/2023]
Abstract
Working with Hamiltonians from chiral effective field theory, we develop a novel framework for describing arbitrary deformed medium-mass nuclei by combining the in-medium similarity renormalization group with the generator coordinate method. The approach leverages the ability of the first method to capture dynamic correlations and the second to include collective correlations without violating symmetries. We use our scheme to compute the matrix element that governs the neutrinoless double beta decay of ^{48}Ca to ^{48}Ti, and find it to have the value 0.61, near or below the predictions of most phenomenological methods. The result opens the door to ab initio calculations of the matrix elements for the decay of heavier nuclei such as ^{76}Ge, ^{130}Te, and ^{136}Xe.
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Affiliation(s)
- J M Yao
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824-1321, USA
| | - B Bally
- Department of Physics and Astronomy, University of North Carolina, Chapel Hill, North Carolina 27516-3255, USA
| | - J Engel
- Department of Physics and Astronomy, University of North Carolina, Chapel Hill, North Carolina 27516-3255, USA
| | - R Wirth
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824-1321, USA
| | - T R Rodríguez
- Departamento de Física Teórica y Centro de Investigación Avanzada en Física Fundamental, Universidad Autónoma de Madrid, E-28049 Madrid, Spain
| | - H Hergert
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824-1321, USA
- Department of Physics & Astronomy, Michigan State University, East Lansing, Michigan 48824-1321, USA
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25
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Yasin H, Schäfer S, Arcones A, Schwenk A. Equation of State Effects in Core-Collapse Supernovae. PHYSICAL REVIEW LETTERS 2020; 124:092701. [PMID: 32202885 DOI: 10.1103/physrevlett.124.092701] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/05/2018] [Revised: 03/05/2019] [Accepted: 02/11/2020] [Indexed: 06/10/2023]
Abstract
We investigate the impact of different properties of the nuclear equation of state in core-collapse supernovae, with a focus on the proto-neutron-star contraction and its impact on the shock evolution. To this end, we introduce a range of equations of state that vary the nucleon effective mass, incompressibility, symmetry energy, and nuclear saturation point. This allows us to point to the different effects in changing these properties from the Lattimer and Swesty to the Shen et al. equations of state, the two most commonly used equations of state in simulations. In particular, we trace the contraction behavior to the effective mass, which determines the thermal nucleonic contributions to the equation of state. Larger effective masses lead to lower pressures at nuclear densities and a lower thermal index. This results in a more rapid contraction of the proto-neutron star and consequently higher neutrino energies, which aids the shock evolution to a faster explosion.
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Affiliation(s)
- H Yasin
- Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany
| | - S Schäfer
- Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany
- ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
| | - A Arcones
- Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
| | - A Schwenk
- Institut für Kernphysik, Technische Universität Darmstadt, 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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Khanmohamadi S, Moshfegh H, Tehrani SA. Hybrid star within the framework of a lowest-order constraint variational method. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.101.023004] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Ekström A, Hagen G. Global Sensitivity Analysis of Bulk Properties of an Atomic Nucleus. PHYSICAL REVIEW LETTERS 2019; 123:252501. [PMID: 31922790 DOI: 10.1103/physrevlett.123.252501] [Citation(s) in RCA: 11] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/10/2019] [Revised: 11/12/2019] [Indexed: 06/10/2023]
Abstract
We perform a global sensitivity analysis of the binding energy and the charge radius of the nucleus ^{16}O to identify the most influential low-energy constants in the next-to-next-to-leading order chiral Hamiltonian with two- and three-nucleon forces. For this purpose, we develop a subspace-projected coupled-cluster method using eigenvector continuation [Frame D. et al., Phys. Rev. Lett. 121, 032501 (2018)PRLTAO0031-900710.1103/PhysRevLett.121.032501]. With this method, we compute the binding energy and charge radius of ^{16}O at more than 10^{6} different values of the 16 low-energy constants in one hour on a standard laptop computer. For relatively small subspace projections, the root-mean-square error is about 1% compared to full-space coupled-cluster results. We find that 58(1)% of the variance in energy can be apportioned to a single contact term in the ^{3}S_{1} wave, whereas the radius depends sensitively on several low-energy constants and their higher-order correlations. The results identify the most important parameters for describing nuclear saturation and help prioritize efforts for uncertainty reduction of theoretical predictions. The achieved acceleration opens up an array of computational statistics analyses of the underlying description of the strong nuclear interaction in nuclei across the Segrè chart.
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Affiliation(s)
- Andreas Ekström
- Department of Physics, Chalmers University of Technology, SE-412 96 Göteborg, Sweden
| | - Gaute Hagen
- Physics Division, Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA
- Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA
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Zanoli S, Roca-Maza X, Colò G, Shen S. Harmonic Potential Theorem: Extension to Spin-, Velocity-, and Density-Dependent Interactions. PHYSICAL REVIEW LETTERS 2019; 123:112501. [PMID: 31573255 DOI: 10.1103/physrevlett.123.112501] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/03/2019] [Revised: 07/18/2019] [Indexed: 06/10/2023]
Abstract
One of the few exact results for the description of the time evolution of an inhomogeneous, interacting many-particle system is given by the harmonic potential theorem (HPT). The relevance of this theorem is that it sets a tight constraint on time-dependent many-body approximations. In this contribution, we show that the original formulation of the HPT is valid also for the case of spin-, velocity-, and density-dependent interactions. This result is completely general and relevant, among the rest, for nuclear structure theory both in the case of ab initio and of more phenomenological approaches. As an example, we report on a numerical implementation by testing the small-amplitude limit of the time-dependent Hartree-Fock-also known as the random phase approximation-for the translational frequencies of a neutron system trapped in a harmonic potential.
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Affiliation(s)
- S Zanoli
- Dipartimento di Fisica "Aldo Pontremoli", Università degli Studi di Milano, 20133 Milano, Italy and INFN, Sezione di Milano, 20133 Milano, Italy
| | - X Roca-Maza
- Dipartimento di Fisica "Aldo Pontremoli", Università degli Studi di Milano, 20133 Milano, Italy and INFN, Sezione di Milano, 20133 Milano, Italy
| | - G Colò
- Dipartimento di Fisica "Aldo Pontremoli", Università degli Studi di Milano, 20133 Milano, Italy and INFN, Sezione di Milano, 20133 Milano, Italy
| | - Shihang Shen
- Dipartimento di Fisica "Aldo Pontremoli", Università degli Studi di Milano, 20133 Milano, Italy and INFN, Sezione di Milano, 20133 Milano, Italy
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