  While many observed debris disks are thought to have gaps suggestive of the
presence of planets, direct imaging surveys do not find many high mass planets
in these systems. We investigate if divergent migration is a viable mechanism
for forming gaps in young debris disks with planets of low enough mass to
currently elude detection. We perform numerical integrations of planet pairs
embedded in planetesimal disks to assess the conditions for which divergent,
planetesimal-driven migration occurs and gaps form within the disk. Gap widths
and the migration rate of planets within a pair depend on both disk mass and
the degree to which the planets share disk material. We find that planet pairs
with planets more massive than Neptune can produce gaps with widths similar to
their orbit distance within 10 Myr at orbit separations probed by direct
imaging campaigns. Pairs of migrating super-Earths likely cannot form
observable gaps on the same time and distance scales, however. Inferring the
responsible planet masses from these gaps while neglecting migration could
overestimate the mass of planets by more than an order of magnitude.
