  Planets with masses larger than about 0.1 Earth-masses undergo rapid inward
migration (type I migration) in a standard protoplanetary disk. Recent
magnetohydrodynamical simulations revealed the presence of magnetically driven
disk winds, which would alter the disk profile and the type I migration in the
close-in region. We investigate orbital evolution of planetary embryos in disks
that viscously evolve under the effects of disk winds. The aim is to discuss
effects of altered disk profiles on type I migration. In addition, we aim to
examine whether observed distributions of close-in super-Earths can be
reproduced by simulations that include effects of disk winds. We perform N-body
simulations of super-Earth formation from planetary embryos, in which a recent
model for disk evolution is used. We explore a wide range of parameters and
draw general trends. We also carry out N-body simulations of close-in
super-Earth formation from embryos in such disks under various conditions. We
find that the type I migration is significantly suppressed in many cases. Even
in cases in which inward migration occurs, the migration timescale is
lengthened to 1 Myr, which mitigates the type I migration problem. This is
because the gas surface density is decreased and has a flatter profile in the
close-in region due to disk winds. We find that when the type I migration is
significantly suppressed, planets undergo late orbital instability during the
gas depletion, leading to a non-resonant configuration. We also find that
observed distributions of close-in super-Earths (e.g., period ratio, mass
ratio) can be reproduced. In addition, we show that in some results of
simulations, systems with a chain of resonant planets, like the TRAPPIST-1
system, form.
