  The total cosmic-ray luminosity of the Galaxy is an important constraint on
models of cosmic-ray generation. The diffuse high energy $\gamma$-ray and
radio-synchrotron emissions of the Milky Way are used to derive this
luminosity. The result is almost two orders of magnitude larger than the
standard estimate, based on the observed isotopic abundances of cosmic ray
nuclides. We discuss the plausible interpretation of this discrepancy and the
possible origin of such a relatively large luminosity.
