  Aims. We aim to describe the pre-main sequence and main-sequence evolution of
X-ray and extreme-ultaviolet radiation of a solar mass star based on its
rotational evolution starting with a realistic range of initial rotation rates.
  Methods. We derive evolutionary tracks of X-ray radiation based on a
rotational evolution model for solar mass stars and the rotation-activity
relation. We compare these tracks to X-ray luminosity distributions of stars in
clusters with different ages.
  Results. We find agreement between the evolutionary tracks derived from
rotation and the X-ray luminosity distributions from observations. Depending on
the initial rotation rate, a star might remain at the X-ray saturation level
for very different time periods, approximately from 10 Myr to 300 Myr for slow
and fast rotators, respectively.
  Conclusions. Rotational evolution with a spread of initial conditions leads
to a particularly wide distribution of possible X-ray luminosities in the age
range of 20 to 500 Myrs, before rotational convergence and therefore X-ray
luminosity convergence sets in. This age range is crucial for the evolution of
young planetary atmospheres and may thus lead to very different planetary
evolution histories.
