  Deviations from geodesic motion caused by gravitational radiation have been
discussed in the last decades to describe the motion of particles or photons in
strong fields around collapsed objects. On cosmological scale this effect,
which in the first order is caused by the finite speed of gravitational
interaction, is important also in the weak field limit. In this paper the
energy loss by transfer to the gravitational potential is determined in a
quasi-Newtonian approximation for the examples of a static Einstein universe
and for an expanding universe with flat metric. In both cases the resulting red
shift is a considerable fraction of the total red shift and requires an
adjustment of the age and the matter composition in our models of the universe.
