  The quark hadron phase transition in a rotating compact star has been
studied. The NLZ-model has been used for the hadronic sector and the MIT Bag
model has been used for the quark sector. It has been found that rotating twin
star (third family) solutions are obtained upto $\Omega \approx 4000 s^{-1}$.
Stars which are rotating faster than this limit do not show any twin star
solution. A backbending in moment of inertia is also observed in the
supermassive rest mass sequences. The braking index is found to diverge for a
star having pure quark core.
