  A spinning fluid embedded in a space section flat Friedmann model is used to
compute the cosmological density perturbation of the model.The spinning fluid
obeys the Einstein-Cartan field equations while the Friedmann embedded model is
assumed to obey the general the Friedmann equation in General Relativity.It is
shown that at the early epochs of the Universe the spin-torsion contribution to
the density perturbation on the matter phase dominates over the radiation
perturbation.On the other hand at the present epochs of the Universe the
spin-torsion contribution is more efficient in the matter
perturbation.Stability of the Friedmann solution in Einstein-Cartan cosmology
is also discussed.
