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Properties of dense nucleon matter and the structure of neutron stars arestudied using variational chain summation methods and the new Argonne v18two-nucleon interaction. The neutron star gravitational mass limit obtainedwith this interaction is 1.67 M_{solar}. Boost corrections to the two-nucleoninteraction, which give the leading relativistic effect of order (v/c)^2, aswell as three-nucleon interactions, are also included in the nuclearHamiltonian. Their successive addition increases the mass limit to 1.80 and2.20 M_{solar}. Hamiltonians including a three-nucleon interaction predict atransition in neutron star matter to a phase with neutral pion condensation ata baryon number density of 0.2 fm^{-3}. We also investigate the possibility ofdense nucleon matter having an admixture of quark matter, described using thebag model equation of state. Neutron stars of 1.4 M_{solar} do not appear tohave quark matter admixtures in their cores. However, the heaviest stars arepredicted to have cores consisting of a quark and nucleon matter mixture. Theseadmixtures reduce the maximum mass of neutron stars from 2.20 to 2.02 (1.91)M_{solar} for bag constant B = 200 (122) MeV/fm^3. Stars with pure quark matterin their cores are found to be unstable. We also consider the possibility thatmatter is maximally incompressible above an assumed density, and show thatrealistic models of nuclear forces limit the maximum mass of neutron stars tobe below 2.5 M_{solar}. The effects of the phase transitions on the compositionof neutron star matter and its adiabatic index are discussed.Comment: 39 pages RevTeX including 12 tables. 21 postscript figures. Submitted  to Phys. Rev.

Equation of state of nucleon matter and neutron star structure