  The morphology of the X-ray and radio emitting features in the central $\sim$
50 kpc region around the galaxy M87 strongly suggests that buoyant bubbles of
cosmic rays (inflated by an earlier nuclear active phase of the galaxy) rise
through the cooling gas at roughly half the sound speed. In the absence of
strong surface tension, initially spherical bubbles will transform into tori as
they rise through an external medium. Such structures can be identified in the
radio images of the halo of M87. During their rise, bubbles will uplift
relatively cool X-ray emitting gas from the central regions of the cooling flow
to larger distances. This gas is colder than the ambient gas and has a higher
volume emissivity. As a result, rising ``radio'' bubbles may be trailed by
elongated X-ray features as indeed is observed in M87. We performed simple
hydrodynamic simulations to qualitatively illustrate the evolution of buoyant
bubbles in the M87 environment.
