  Exact models of uniformly rotating strange stars, built of self bound quark
matter, are calculated within the framework of general relativity. This is made
possible thanks to a new numerical technique capable to handle the strong
density discontinuity at the surface of these stars. Numerical calculations are
done for a simple MIT bag model equation of state of strange quark matter.
Evolutionary sequences of models of rotating strange stars at constant baryon
mass are calculated. Maximally rotating configurations of strange stars are
determined, assuming that the rotation frequency is limited by the mass
shedding and the secular instability with respect to axisymmetric
perturbations. Exact formulae which give the dependence of the maximum rotation
frequency, and of the maximum mass and corresponding radius of rotating
configurations, on the value of the bag constant, are obtained. The values of
T/W for rapidly rotating massive strange stars are significantly higher than
those for ordinary neutron stars. This might indicate particular susceptibility
of rapidly rotating strange stars to triaxial instabilities.
