  Aims. We study the evolution of rotation and high energy X-ray, extreme
ultraviolet (EUV), and Ly-alpha emission for F, G, K, and M dwarfs, with masses
between 0.1 and 1.2 Msun, and provide our evolutionary code and a freely
available set of evolutionary tracks for use in planetary atmosphere studies.
  Methods. We develop a physical rotational evolution model constrained by
observed rotation distributions in young stellar clusters. Using rotation,
X-ray, EUV, and Ly-alpha measurements, we derive empirical relations for the
dependences of high energy emission on stellar parameters. Our description of
X-ray evolution is validated using measurements of X-ray distributions in young
clusters.
  Results. A star's X-ray, EUV, and Ly-alpha evolution is determined by its
mass and initial rotation rate, with initial rotation being less important for
lower mass stars. At all ages, solar mass stars are significantly more X-ray
luminous than lower mass stars and stars that are born as rapid rotators remain
highly active longer than those born as slow rotators. At all evolutionary
stages, habitable zone planets receive higher X-ray and EUV fluxes when
orbiting lower mass stars due to their longer evolutionary timescales. The
rates of flares follow similar evolutionary trends with higher mass stars
flaring more often than lower mass stars at all ages, though habitable zone
planets are likely influenced by flares more when orbiting lower mass stars.
  Conclusions. Our results show that single decay-laws are insufficient to
describe stellar activity evolution and highlight the need for a more
comprehensive description based on the evolution of rotation, including also
the effects of short-term variability. Planets at similar orbital distances
from their host stars receive significantly more X-ray and EUV energy over
their lifetimes when orbiting higher mass stars. (abstract incomplete)
