  We study how structural properties of globular clusters and dwarf galaxies
are linked to their orbits in the Milky Way halo. From the inner to the outer
halo, orbital energy increases and stellar-systems gradually move out of
internal equilibrium: in the inner halo, high-surface brightness globular
clusters are at pseudo-equilibrium, while further away, low-surface brightness
clusters and dwarfs appear more tidally disturbed. Dwarf galaxies are the
latest to arrive into the halo as indicated by their large orbital energies and
pericenters, and have no time for more than one orbit. Their (gas-rich)
progenitors likely lost their gas during their recent arrival in the Galactic
halo. If dwarfs are at equilibrium with their dark matter (DM) content, the DM
density should anti-correlate with pericenter. However, the transformation of
DM dominated dwarfs from gas-rich rotation-supported into gas-poor
dispersion-supported systems is unlikely accomplished during a single orbit. We
suggest instead that the above anti-correlation is brought by the combination
of ram-pressure stripping and of Galactic tidal shocks. Recent gas removal
leads to an expansion of their stellar content caused by the associated gravity
loss, making them sufficiently fragile to be transformed near pericenter
passage. Out of equilibrium dwarfs would explain the observed anti-correlation
of kinematics-based DM density with pericenter without invoking DM density
itself, questioning its previous estimates. Ram-pressure stripping and tidal
shocks may contribute to the dwarf velocity dispersion excess. It predicts the
presence of numerous stars in their outskirts and a few young stars in their
cores.
