Relativistic equation of state of nuclear matter for supernova and neutron star |
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| Affiliation: | 1. Research Center for Nuclear Physics(RCNP), Osaka University, Ibaraki, Osaka 567, Japan;2. Department of Physics, Nankai University, Tianjin 300071, China;3. The Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351, Japan;4. Department of Energy Engineering and Science, Nagoya University, Nagoya 464-01, Japan;1. State Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100190, China;2. School of Physics, University of Chinese Academy of Sciences, Beijing 100049, China;3. Theoretical Physics Center for Science Facilities, Institute of High Energy Physics, Beijing 100049, China;4. Synergetic Innovation Center for Quantum Effects and Application, Hunan Normal University, Changsha 410081, China;5. Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator, Lanzhou 730000, China;1. Institut für Kernphysik, Fachbereich Physik, Technische Universität Darmstadt, 64289 Darmstadt, Germany;2. ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany;3. Department of Physics, University of Idaho, Moscow, ID 83844, USA;1. Shanghai Advanced Research Institute, Chinese Academy of Sciences, Shanghai 201210, China;2. Shanghai Institute of Applied Physics, Chinese Academy of Sciences, Shanghai 201800, China;3. University of Chinese Academy of Sciences, Beijing 100049, China;4. Sino-French Institute of Nuclear Engineering and Technology, Sun Yat-Sen University, Zhuhai 519082, China;5. Department of Physics, Yuncheng University, Yuncheng 044000, China;6. Department of Physics and Astronomy, Texas A&M University-Commerce, Commerce, TX 75429, USA;1. School of Science, Qingdao Technological University, Qingdao 266000, China;2. School of Nuclear Science and Technology, University of South China, 421001 Hengyang, China;3. Cooperative Innovation Center for Nuclear Fuel Cycle Technology & Equipment, University of South China, 421001 Hengyang, China;1. GSI Helmholtzzentrum für Schwerionenforschung GmbH, Darmstadt, Germany;2. SUBATECH, UMR 6457, Ecole des Mines de Nantes – IN2P3/CNRS – Université de Nantes, France;1. Department of Physics, University of Maryland, College Park, MD 20742, United States;2. Institute for Nuclear Theory, University of Washington, Seattle, WA, United States |
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| Abstract: | We construct the equation of state (EOS) of nuclear matter using the relativistic mean field (RMF) theory in the wide density, temperature range with various proton fractions for the use of supernova simulation and the neutron star calculations. We first construct the EOS of homogeneous nuclear matter. We use then the Thomas-Fermi approximation to describe inhomogeneous matter, where heavy nuclei are formed together with free nucleon gas. We discuss the results on free energy, pressure and entropy in the wide range of astrophysical interest. As an example, we apply the resulting EOS on the neutron star properties by using the Oppenheimer-Volkoff equation. |
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