  We study rapidly rotating hybrid stars with the Dyson-Schwinger model for
quark matter and the Brueckner-Hartree-Fock many-body theory with realistic
two-body and three-body forces for nuclear matter. We determine the maximum
gravitational mass, equatorial radius, and rotation frequency of stable stellar
configurations by considering the constraints of the Keplerian limit and the
secular axisymmetric instability, and compare with observational data. We also
discuss the rotational evolution for constant baryonic mass, and find a spinup
phenomenon for supramassive stars before they collapse to black holes.
