  Recent data support the idea that the filaments observed in H_alpha emission
near the centres of some galaxy clusters were shaped by bulk flows within their
intracluster media. We present numerical simulations of evaporated clump
material interacting with impinging winds to investigate this possibility. In
each simulation, a clump falls due to gravity while the drag of a wind retards
the fall of evaporated material leading to elongation of the tail. However, we
find that long filaments can only form if the outflowing wind velocity is
sufficiently large, 10^8 cm s^-1. Otherwise, the tail material sinks almost as
quickly as the cloud. For reasonable values of parameters, the morphological
structure of a tail is qualitatively similar to those observed in clusters.
Under certain conditions, the kinematics of the tail resemble those reported in
Hatch et al.(2006). A comparison of the observations with the numerical results
indicates that the filaments are likely to be a few tens of Myrs old. We also
present arguments which suggest that the momentum transfer, from an outflowing
wind, in the formation of these filaments is probably significant. As a result,
tail formation could play a role in dissipating some of the energy injected by
a central AGN close to the cluster centre where it is needed most. The trapping
of energy by the cold gas may provide an additional feedback mechanism that
helps to regulate the heating of the central regions of galaxy clusters and
couple the AGN to the ICM.
