  Entangled magnetic fields entering into an accretion flow would very soon be
stretched into a dominant toroidal component due to strong differentially
rotating motion inside the accretion disc. This is particularly true for weakly
viscous, low angular momentum transonic or advective discs. We study the
trajectories of toroidal flux tubes inside a geometrically thick flow which
undergoes a centrifugal force supported shock. We also study effects of these
flux tubes on the dynamics of the inflow and the outflow. We use a finite
difference method (Total Variation Diminishing) for this purpose and
specifically focussed on whether these flux tubes significantly affect the
properties of the outflows such as its collimation and the rate. It is seen
that depending upon the cross-sectional radius of the flux tubes which control
the drag force, these field lines may move towards the central object or
oscillate vertically before eventually escaping out of the funnel wall
(pressure zero surfaces) along the vertical direction. A comparison of results
obtained with and without flux tubes show these flux tubes could play pivotal
role in collimation and acceleration of jets and outflows.
