  We study the formation of hot spheroidal systems within the frame of a
scenario where galaxy formation and evolution is related to the gentle mass
aggregation history and primordial angular momentum of protogalaxies, both
defined by the cosmological initial conditions. We explore two cases: (1) the
hot spheroidal system forms from the dynamical instabilities of the stellar
disks, and (2) the spheroidal systems are formed during the dissipative
collapse of the gas before falling to the disk in centrifugal equilibrium. In
the former case a good agreement with observations for late type galaxies is
found. In the second case, contrary to recent claims, we find that the tidal
stability criterion is not easily reached. The gas that dissipatively collapses
within the dark matter halos should be very clumpy, and the clumps very dense,
in order to avoid the tidal destruction of the star formation unities.
