  We present a model for the gamma-ray emission of pulsars in terms of
curvature radiation by highly relativistic particles. It is shown that the
injection of power-law primary particles from an outer gap and subsequent
cooling by curvature radiation losses reproduces the high energy spectrum and
the luminosity of pulsars. As a result a spectral break is to be expected at a
photon energy of $\sim 1\thinspace{\rm GeV}$. This value does not depend on the
surface magnetic field strength or on the period of the neutron star, but only
involves a geometric factor. The predicted change of the spectral index by 1
explains in particular the spectral shape of PSR B1706--44. We find that
according to this model the luminosity of pulsars in the high energy band
varies according to $L_{\gamma}\propto B_0/P^{5/3}$, which is in good agreement
with the observations.
  A model for the infrared, optical and soft X-ray emission of pulsar is also
presented. It is based on anisotropic synchrotron emission by relativistic
particles in an outer gap scenario with a single energy distribution
$N(\gamma)\propto \gamma^{-2}$. It is shown that this synchrotron model is able
to reproduce the spectral shape between the infrared and soft X-rays and also
the corresponding luminosities for the Crab pulsar. In particular, the long
standing problem of the rapid spectral decline towards infrared frequencies is
understandable as emission at very small pitch angles from low energy particles
with $\gamma\ga 10$. It is also shown that the scaling of the synchrotron model
explains the observed correlation between the X-ray luminosity and the
spin-down luminosity of the neutron star $L_{\rm x} \sim 10^{-3} {\dot E}$.
