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SHEN Hong, WANG Yan-nan. Properties of Dense Matter and Equation of State for Supernovae and Neutron Stars[J]. Nuclear Physics Review, 2012, 29(2): 117-122. doi: 10.11804/NuclPhysRev.29.02.117
Citation: SHEN Hong, WANG Yan-nan. Properties of Dense Matter and Equation of State for Supernovae and Neutron Stars[J]. Nuclear Physics Review, 2012, 29(2): 117-122. doi: 10.11804/NuclPhysRev.29.02.117
shu

Properties of Dense Matter and Equation of State for Supernovae and Neutron Stars

doi: 10.11804/NuclPhysRev.29.02.117

  • School of Physics, Nankai University, Tianjin 300071, China

  • Received Date: 1900-01-01
  • Rev Recd Date: 1900-01-01
  • Publish Date: 2012-06-20
  • The properties of dense matter are studied within the relativistic meanfield theory. The equation of state (EOS) of dense matter are constructed covering a wide range of temperature, proton fraction, and density for the use of supernova simulations. The relativistic meanfield theory is employed to describe the uniform matter, while the ThomasFermi approximation is adopted to describe the nonuniform matter. The EOS of neutron star matter is discussed with the inclusion of hyperons. It is found that the EOS at high density can be significantly softened by the inclusion of hyperons. The 1S0 superfluidity of Λ hyperons may exist in massive neutron stars.
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Properties of Dense Matter and Equation of State for Supernovae and Neutron Stars

doi: 10.11804/NuclPhysRev.29.02.117
  • School of Physics, Nankai University, Tianjin 300071, China
  • Received Date: 1900-01-01
  • Rev Recd Date: 1900-01-01
  • Publish Date: 2012-06-20

Abstract: The properties of dense matter are studied within the relativistic meanfield theory. The equation of state (EOS) of dense matter are constructed covering a wide range of temperature, proton fraction, and density for the use of supernova simulations. The relativistic meanfield theory is employed to describe the uniform matter, while the ThomasFermi approximation is adopted to describe the nonuniform matter. The EOS of neutron star matter is discussed with the inclusion of hyperons. It is found that the EOS at high density can be significantly softened by the inclusion of hyperons. The 1S0 superfluidity of Λ hyperons may exist in massive neutron stars.

SHEN Hong, WANG Yan-nan. Properties of Dense Matter and Equation of State for Supernovae and Neutron Stars[J]. Nuclear Physics Review, 2012, 29(2): 117-122. doi: 10.11804/NuclPhysRev.29.02.117
Citation: SHEN Hong, WANG Yan-nan. Properties of Dense Matter and Equation of State for Supernovae and Neutron Stars[J]. Nuclear Physics Review, 2012, 29(2): 117-122. doi: 10.11804/NuclPhysRev.29.02.117
shu

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