  The radial velocities and direct imaging observations of exoplanets have
suggested that the frequency of giant planets may decrease for
intermediate-mass stars ($2.5-8\,M_\odot$). The key mechanism that could hinder
their formation remains unclear. From a theoretical point of view, planet
formation around intermediate-mass stars may take place on longer timescales,
which -- coupled with fast migration and efficient photoevaporation -- may
prevent planetary formation in these environments. In this letter, we
investigate the temporal evolution of the radial drift for dust particles in
disks when stellar evolution is taken into account. We demonstrate that the
particle drift velocity around intermediate-mass stars sharply increases after
1$-$2 Myr, potentially forming a difficult barrier to overcome in the first
steps of planet formation. This high radial drift could explain the lack of
disk detections around intermediate-mass stars older than 3$-$4 Myr, as opposed
to low-mass stars ($<2.5\,M_\odot$), where the drift may not be the most
impactful factor for the disk evolution. Future high-resolution images of these
disks can help us to explain why planets around intermediate-mass stars may be
rare. In addition, we can explore whether the role of efficient dust radial
drift does in fact hinder planet formation around intermediate-mass stars -- or
otherwise.
