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An equation of state (EOS) for uniform asymmetric nuclear matter (ANM) isconstructed at zero and finite temperatures by the variational method startingfrom the nuclear Hamiltonian that is composed of the Argonne v18 and Urbana IXpotentials. At zero temperature, the two-body energy is calculated with theJastrow wave function in the two-body cluster approximation which issupplemented by Mayer's condition and the healing-distance condition so as toreproduce the result by Akmal, Pandharipande and Ravenhall. The energy causedby the three-body force is treated somewhat phenomenologically so that thetotal energy reproduces the empirical saturation conditions. The masses andradii of neutron stars obtained with the EOS are consistent with recentobservational data. At finite temperatures, thermodynamic quantities such asfree energy, internal energy, entropy, pressure and chemical potentials arecalculated with an extension of the method by Schmidt and Pandharipande. Thevalidity of the frozen-correlation approximation employed in this work isconfirmed as compared with the result of the fully minimized calculation. Thequadratic proton-fraction-dependence of the energy of ANM is confirmed at zerotemperature, whereas the free energy of ANM deviates from the quadraticproton-fraction-dependence markedly at finite temperatures. The obtained EOS ofANM will be an important ingredient of a new nuclear EOS for supernovanumerical simulations.

Variational study for the equation of state of asymmetric nuclear matter at finite temperatures