We have computed quasiequilibrium sequences of synchronously rotating compact binary star systems with constant rest masses .
This computation has been carried out by using the numerical scheme which is different from the scheme based on the conformally flat assumption about the space .

Stars are assumed to be polytropes with polytropic indices of N = 0.5 , N = 1.0 , and N = 1.5 .
Since we have computed binary star sequences with a constant rest mass , they provide approximate evolutionary tracks of binary star systems .
For relatively stiff equations of state ( N < 1.0 ) , there appear turning points along the quasiequilibrium sequences plotted in the angular momentum — angular velocity plane .
Consequently secular instability against exciting internal motion sets in at those points .
Qualitatively , these results agree with those of Baumgarte et al . who employed the conformally flat condition .

We further discuss the effect of different equations of state and different strength of gravity by introducing two kinds of dimensionless quantities which represent the angular momentum and the angular velocity .
Strength of gravity is renormalized in these quantities so that the quantities are transformed to values around unity .
Therefore we can clearly see relations among quasiequilibrium sequences for a wide variety of strength of gravity and for different compressibility .