Characteristic radii of the Milky Way Globular Clusters
  We report on the extent of the effects of the Milky Way's gravitational field
in shaping the structural parameters and internal dynamics of its globular
cluster population. We make use of a homogeneous, up-to-date data set with
kinematics, structural properties, current and initial masses of 156 globular
clusters. In general, cluster radii increase as the Milky Way potential
weakens; with the core and Jacobi radii being those which increase at the
slowest and fastest rate respectively. We interpret this result as the
innermost regions of globular clusters being less sensitive to changes in the
tidal forces with the Galactocentric distance. The Milky Way's gravitational
field also seems to have differentially accelerated the internal dynamical
evolution of individual clusters, with those toward the bulge appearing
dynamically older. Finally we find a sub-population consisting of both compact
and extended globular clusters (as defined by their rh/rJ ratio) beyond 8 kpc
that appear to have lost a large fraction of their initial mass lost via
disruption. Moreover, we identify a third group with rh/rJ > 0.4, which have
lost an even larger fraction of their initial mass by disruption. In both cases
the high fraction of mass lost is likely due to their large orbital
eccentricities and inclination angles, which lead to them experiencing more
tidal shocks at perigalacticon and during disc crossings. Comparing the
structural and orbital parameters of individual clusters allows for constraints
to be placed on whether or not their evolution was relaxation or tidally
dominated.
