  In the teleparallel equivalent of general relativity the energy density of
asymptoticaly flat gravitational fields can be naturally defined as a scalar
density restricted to a three dimensional spacelike hypersurface. The scalar
density has simple expression in terms of the trace of the torsion tensor. Here
we obtain the formal expression of the localized energy for a Kerr black hole.
The energy inside a surface of constant radius can be explicitly calculated in
the limit of small $a$, the specific angular momentum. Such expression turns
out to be exactly the same as the one obtained by means of the method recently
proposed by Brown and York.
