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We present the first computations of quasiequilibrium binary neutron starswith different mass components in general relativity, within theIsenberg-Wilson-Mathews approximation. We consider both cases of synchronizedrotation and irrotational motion. A polytropic equation of state is used withthe adiabatic index gamma=2. The computations have been performed for thefollowing combinations of stars: (M/R)_{star 1} vs. (M/R)_{star 2} = 0.12 vs.(0.12, 0.13, 0.14), 0.14 vs. (0.14, 0.15, 0.16), 0.16 vs. (0.16, 0.17, 0.18),and 0.18 vs. 0.18, where (M/R) denotes the compactness parameter of infinitelyseparated stars of the same baryon number. It is found that for identical massbinary systems there is no turning point of the binding energy (ADM mass)before the end point of the sequence (mass shedding point) in the irrotationalcase, while there is one before the end point of the sequence (contact point)in the synchronized case. On the other hand, in the different mass case, thesequence ends by the tidal disruption of the less massive star (mass sheddingpoint). It is then more difficult to find a turning point in the ADM mass.Furthermore, we find that the deformation of each star depends mainly on theorbital separation and the mass ratio and very weakly on its compactness. Onthe other side, the decrease of the central energy density depends on thecompactness of the star and not on that of the companion.Comment: 17 pages, revtex file with 14 figures and 4 tables, accepted for  publication in Phys. Rev.

physical review. d. particles, fields, gravitation, and cosmology/physical review. d. particles and fields

Quasiequilibrium sequences of synchronized and irrotational binary neutron stars in general relativity. III. Identical and different mass stars with<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>γ</mml:mi><mml:mo>=</mml:mo><mml:mn>2</mml:mn><mml:mn /></mml:math>

Quasiequilibrium sequences of synchronized and irrotational binary neutron stars in general relativity. III. Identical and different mass stars withγ=2