  We study geometrically thick non-self gravitating equilibrium tori orbiting a
Schwarzschild black hole immersed in swirling universes. This solution is
axially symmetric and non-asymptotically flat, and its north and south
hemispheres spin in opposite directions. Due to repulsive effects arising from
the swirl of the background spacetime, the equilibrium torus exists only in the
case with the small swirling parameter. With the increase of the swirling
parameter, the disk structure becomes small and the excretion of matter near
the black hole becomes strong. Moreover, the odd $Z_2$ symmetry of spacetimes
originating from the swirling parameter yields that the orientation of closed
equipotential surfaces deviates away from the horizontal axis and the
corresponding disk does not longer possess the symmetry with respect to the
equatorial plane. These significant features could help to further understand
the equilibrium tori and geometrically thick accretion disks around black holes
in swirling universes.
