Equation of State of Neutron Star Matter and Neutron Star Models

概要

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The energy of neutron star matter is calculated by using the Brueckner theory for three different-type nuclear potentials in the range of densities 5×10^<13>IsimρIsim1.14×10^<15>(g cm^<-3>). In this calculation, contributions from higher partial waves, three-body clusters and mixture of protons are included. Contribution from three-body clusters becomes about 10 per cent to the kinetic energy in a density region higher than 7×10^<14> g cm^<-3> in the case of a potential with strong hard core. The relative proton number is about 5〜7 per cent to the neutron number, and energy gain by mixture of protons is about 10 per cent to the total energy in higher densities. Using these results, equations of state are determined and extended by several methods to density regions higher than 1.14×10^<15> g cm^<-3>. Neutron star models are constructed based on the derived equations of state. These models show that the maximum mass of the stable neutron star lies between 1 Mxodoi and 3 Mxodoi. The ^<3>P_2-pairing superfluidity is investigated and the energy gap of half a MeV has been obtained. Some physical effects by this superfluidity are discussed in relation to the pulsar and the thermal history.
理論物理学刊行会の論文
1971-07-25