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We study equilibrium sequences of close binary systems composed of identicalpolytropic stars in Newtonian gravity. The solving method is a multi-domainspectral method which we have recently developed. An improvement is introducedhere for accurate computations of binary systems with stiff equation of state($\gamma > 2$). The computations are performed for both cases of synchronizedand irrotational binary systems with adiabatic indices $\gamma=3,~2.5,~2.25,~2$and 1.8. It is found that the turning points of total energy along aconstant-mass sequence appear only for $\gamma \ge 1.8$ for synchronized binarysystems and $\gamma \ge 2.3$ for irrotational ones. In the synchronized case,the equilibrium sequences terminate by the contact between the two stars. Onthe other hand, for irrotational binaries, it is found that the sequencesterminate at a mass shedding limit which corresponds to a detachedconfiguration.Comment: 27 pages, 2 tables, 34 figures, revtex, added one more figure and its  explanation, accepted to Phys. Rev.

Quasiequilibrium sequences of synchronized and irrotational binary neutron stars in general relativity. II. Newtonian limits