Abstract
Using a recent microscopic equation of state (EOS) for neutron star matter, we construct equilibrium sequences of rapidly rotating neutron stars in general relativity. The sequences are the normal and supramassive evolutionary sequences of constant rest mass. Also calculated is the radius of the marginally stable orbit and its dependence on the rotation rate Ω, relevant for modeling of kilo-Hertz quasi-periodic oscillations in X-ray binaries.
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