  We model and interpret the Kilohertz QPOs from the hydrodynamical description
of accretion disk around a rapidly rotating compact strange star. The higher
QPO frequency is described by the viscous effects of accretion disk leading to
shocks, while the lower one is taken to be the Keplerian motion of the
accreting matter. Comparing our results with the observations for two of the
fastest rotating compact stellar candidates namely, 4U~1636-53 and KS 1731-260,
we find that they match to a very good approximation, thus interpreting them as
strange stars.
