  The multitude of recent multi-point spacecraft observations of solar
energetic particle (SEP) events have made it possible to study the longitudinal
distribution of SEPs in great detail. SEPs, even those accelerated during
impulsive events, show a much wider than expected longitudinal extent, bringing
into question the processes responsible for their transport perpendicular to
the local magnetic field. In this paper we examine some aspects of
perpendicular transport by including perpendicular diffusion into a numerical
SEP transport model that simulates the propagation of impulsively accelerated
SEP electrons in the ecliptic plane. We find that: (i) The pitch-angle
dependence of the perpendicular diffusion coefficient is an important, and
currently mainly overlooked, transport parameter. (ii) SEP intensities are
generally asymmetric in longitude, being enhanced towards the west of optimal
magnetic connection to the acceleration region. (iii) The maximum SEP intensity
may also be shifted (parameter dependently) away from the longitude of best
magnetic connectivity at 1 AU. We also calculate the maximum intensity, the
time of maximum intensity, the onset time and the maximum anisotropy as a
function of longitude at Earth's orbit and compare the results, in a
qualitative fashion, to recent spacecraft observations.
