  The wind of an asymptotic-giant-branch stars is sufficiently strong that if
it is slightly asymmetric, it can propel the star outside of the open cluster
of its birth or significantly alter its trajectory through a globular cluster;
therefore, if these stellar winds are asymmetric, one would expect a deficit of
white dwarfs of all ages in open clusters and for young white dwarfs to be less
radially concentrated than either their progenitors or older white dwarfs in
globular clusters. This latter effect has recently been observed. Hence,
detailed studies of the radial distribution of young white dwarfs in globular
clusters could provide a unique probe of mass loss on the asymptotic giant
branch and during the formation of planetary nebulae both as a function of
metallicity and a limited range of stellar mass.
