  We consider Bondi's radiating metric in the context of the teleparallel
equivalent of general relativity (TEGR). This metric describes the asymptotic
form of a radiating solution of Einstein's equations. The total gravitational
energy for this solution can be calculated by means of pseudo-tensors in the
static case. In the nonstatic case, Bondi defines the {\it mass aspect} $m(u)$,
which describes the mass of an isolated system. In this paper we express
Bondi's solution in asymptotically spherical 3+1 coordinates, not in radiation
coordinates, and obtain Bondi's energy in the static limit by means of the
expression for the gravitational energy in the framework of the TEGR. We can
either obtain the total energy or the energy inside a large (but finite)
portion of the three-dimensional spacelike hypersurface, whose boundary is far
away from the source. The relationship of the present energy expression with
Moller's energy is established.
