  We study the effect of spiral arm passages on the evolution of star clusters
on planar and circular orbits around the centres of galaxies. Individual
passages with different relative velocity (V_drift) and arm width are studied
using N-body simulations. When the ratio of the time it takes the cluster to
cross the density wave to the crossing time of stars in the cluster is much
smaller than one, the energy gain of stars can be predicted accurately in the
impulsive approximation. When this ratio is much larger than one, the cluster
is heated adiabatically and the net effect of heating is largely damped. For a
given duration of the perturbation, this ratio is smaller for stars in the
outer parts of the cluster compared to stars in the inner part. The cluster
energy gain due to perturbations of various duration as obtained from our
N-body simulations is in good agreement with theoretical predictions taking
into account the effect of adiabatic damping. Perturbations by the broad
stellar component of the spiral arms on a cluster are in the adiabatic regime
and, therefore, hardly contribute to the energy gain and mass loss of the
cluster. We consider the effect of crossings through the high density shocked
gas in the spiral arms, which result in a more impulsive compression of the
cluster. The time scale of disruption is shortest at ~0.8-0.9 R_CR since there
V_drift is low. This location can be applicable to the solar neighbourhood. In
addition, the four-armed spiral pattern of the Milky Way makes spiral arms
contribute more to the disruption of clusters than in a similar but two-armed
galaxy. Still, the disruption time due to spiral arm perturbations there is
about an order of magnitude higher than what is observed for the solar
neighbourhood.[ABRIDGED]
