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Constraints on the symmetry energy and neutron skins from experiments and theory

M. B. TsangNational Superconducting Cyclotron Laboratory and Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USAJ. R. StoneDepartment of Physics, University of Oxford, OX1 3PU Oxford, United Kingdom and Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USAF. CameraINFN, Sezione di Milano, via Celoria 16, I-20133 Milano, ItalyPaweł DanielewiczNational Superconducting Cyclotron Laboratory and Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USAStefano GandolfiTheoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USAK. HebelerDepartment of Physics, The Ohio State University, Columbus, Ohio 43210, USAC. J. HorowitzCenter for Exploration of Energy and Matter and Physics Department, Indiana University, Bloomington, Indiana 47405, USAJenny LeeRIKEN Nishina Center, Hirosawa 2-1, Wako, Saitama 351-0198, JapanW. G. LynchNational Superconducting Cyclotron Laboratory and Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USAZ. KohleyNational Superconducting Cyclotron Laboratory and Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USAR. C. LemmonNuclear Physics Group, STFC Daresbury Laboratory, Daresbury, Warrington WA4 4AD, United KingdomP. MöllerTheoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USAT. MurakamiDepartment of Physics, Kyoto University, Kyoto 606-8502, JapanS. RiordanUniversity of Massachusetts Amherst, Amherst, Massachusetts 01003, USAX. Roca-MazaINFN, Sezione di Milano, via Celoria 16, I-20133 Milano, ItalyFrancesca SammarrucaPhysics Department, University of Idaho, Moscow, Idaho 83844-0903, USAAndrew W. SteinerInstitute for Nuclear Theory, University of Washington, Seattle, Washington 98195, USAIsaac VidañaCentro de Física Computacional, Department of Physics, University of Coimbra, PT-3004-516 Coimbra, PortugalS. J. YennelloCyclotron Institute and Chemistry Department, Texas A&M University, College Station, Texas 77843, USA

2012en

ABI

Annotatsiya

The symmetry energy contribution to the nuclear equation of state impacts various phenomena in nuclear astrophysics, nuclear structure, and nuclear reactions. Its determination is a key objective of contemporary nuclear physics, with consequences for the understanding of dense matter within neutron stars. We examine the results of laboratory experiments that have provided initial constraints on the nuclear symmetry energy and on its density dependence at and somewhat below normal nuclear matter density. Even though some of these constraints have been derived from properties of nuclei while others have been derived from the nuclear response to electroweak and hadronic probes, within experimental uncertainties-they are consistent with each other. We also examine the most frequently used theoretical models that predict the symmetry energy and its slope parameter. By comparing existing constraints on the symmetry pressure to theories, we demonstrate how contributions of three-body forces, which are essential ingredients in neutron matter models, can be determined.

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DOI: 10.1103/physrevc.86.015803

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