  We study time evolution of rotating, axisymmetric, two dimensional inviscid
accretion flows around black holes using a grid based finite difference method.
We do not use reflection symmetry on the equatorial plane in order to inspect
if the disk along with the centrifugal barrier oscillated vertically. In the
inviscid limit, we find that the CENtrifugal pressure supported BOundary Layer
(CENBOL) is oscillating vertically, more so, when the specific angular momentum
is higher. As a result, the rate of outflow produced from the CENBOL, also
oscillates. Indeed, the outflow rates in the upper half and the lower half are
found to be anti-correlated. We repeat the exercise for a series of specific
angular momentum {\lambda} of the flow in order to demonstrate effects of the
centrifugal force on this interesting behaviour. We find that, as predicted in
theoretical models of disks in vertical equilibrium, the CENBOL is produced
only when the centrifugal force is significant and more specifically, when
{\lambda} > 1.5. Outflow rate itself is found to increase with {\lambda} as
well and so is the oscillation amplitude. The cause of oscillation appears to
be due to the interaction among the back flow from the centrifugal barrier, the
outflowing winds and the inflow. For low angular momentum, the back flow as
well as the oscillation are missing. To our knowledge, this is the first time
that such an oscillating solution is found with an well-tested grid based
finite difference code and such a solution could be yet another reason of why
Quasi-Periodic Oscillations should be observed in black hole candidates which
are accreting low angular momentum transonic flows.
