  The presence of forming planets embedded in their protoplanetary disks has
been inferred from the detection of multiring structures in such disks. Most of
these suspected planets are undetectable by direct imaging observations at
current measurement sensitivities. Inward migration and accretion might make
these putative planets accessible to the Doppler method, but the actual extent
of growth and orbital evolution remains unconstrained.
  Under the premise that the gaps in the disk around HD 163296 originate from
new-born planets, we investigate if and under which circumstances the
gap-opening planets could represent progenitors of the exoplanet population
detected around A-type stars. In particular, we study the dependence of final
planetary masses and orbital parameters on the viscosity of the disk. The
evolution of the embedded planets was simulated throughout the disk lifetime
and up to 100 Myr after the dispersal of the disk, taking the evolving disk
structure and a likely range of disk lifetimes into account.
  We find that the final configuration of the planets is largely determined by
the $\alpha$ viscosity parameter of the disk and less dependent on the choice
for the disk lifetime and the initial planetary parameters. If we assume that
planets such as those in HD 163296 evolve to form the observed exoplanet
population of A-type stars, a $\alpha$ parameter on the order of $3.16 \times
10^{-4} \lesssim \alpha \lesssim 10^{-3}$ is required for the disks to induce
sufficiently high migration rates. Depending on whether or not future direct
imaging surveys will uncover a larger number of planets with $m_\mathrm{pl}
\lesssim 3 M_\mathrm{Jup}$ and $a_\mathrm{pl} \gtrsim 10 \mathrm{AU}$ we expect
the $\alpha$ parameter to be at the lower or upper end of this range, always
under the assumption that such disks indeed harbor wide orbit planets.
