  We consider the quasi-black hole limit of a stationary body when its boundary
approaches its own gravitational radius, i.e., its quasi-horizon. It is shown
that there exists a perfect correspondence between the different mass
contributions and the mass formula for quasi-black and black holes in spite of
difference in derivation and meaning of the formulas in both cases. For
extremal quasi-black holes the finite surface stresses give zero contribution
to the total mass. Conclusions similar to those for the properties of mass are
derived for the angular momentum.
