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Planets with masses larger than about 0.1 Earth-masses undergo rapid inwardmigration (type I migration) in a standard protoplanetary disk. Recentmagnetohydrodynamical simulations revealed the presence of magnetically drivendisk winds, which would alter the disk profile and the type I migration in theclose-in region. We investigate orbital evolution of planetary embryos in disksthat viscously evolve under the effects of disk winds. The aim is to discusseffects of altered disk profiles on type I migration. In addition, we aim toexamine whether observed distributions of close-in super-Earths can bereproduced by simulations that include effects of disk winds. We perform N-bodysimulations of super-Earth formation from planetary embryos, in which a recentmodel for disk evolution is used. We explore a wide range of parameters anddraw general trends. We also carry out N-body simulations of close-insuper-Earth formation from embryos in such disks under various conditions. Wefind that the type I migration is significantly suppressed in many cases. Evenin cases in which inward migration occurs, the migration timescale islengthened to 1 Myr, which mitigates the type I migration problem. This isbecause the gas surface density is decreased and has a flatter profile in theclose-in region due to disk winds. We find that when the type I migration issignificantly suppressed, planets undergo late orbital instability during thegas depletion, leading to a non-resonant configuration. We also find thatobserved distributions of close-in super-Earths (e.g., period ratio, massratio) can be reproduced. In addition, we show that in some results ofsimulations, systems with a chain of resonant planets, like the TRAPPIST-1system, form.

Formation of close-in super-Earths in evolving protoplanetary disks due to disk winds