  We report on the Swift observations of the candidate supergiant fast X-ray
transient (SFXT) IGR J16418-4532, which has an orbital period of ~3.7 d. Our
monitoring, for a total of ~43 ks, spans over three orbits and represents the
most intense and complete sampling along the orbital period of the light curve
of this source. If one assumes a circular orbit, the X-ray emission from this
source can be explained by accretion from a spherically symmetric clumpy wind
from a blue supergiant, composed of clumps with different masses, ranging from
~5x10^16 g to 10^21g.
