  For the origin of the radially concentrated solar system's terrestrial
planets, planet formation from a ring of solids at about 1 au from the Sun with
convergent/suppressed type I migration is preferred. On the other hand, many
super-Earths and sub-Neptunes are found in the close-in region with orbital
periods of 10-100 days, so that planet formation from rings in the 1-au region
would require some degree of inward migration. One way to realize these
different formation scenarios is to use different gas disk models. In this
study we investigate whether different scenarios can be realized within a
single framework. We consider a disk model that evolves via disk winds and
develops a density peak, and study planet formation and orbital evolution using
N-body simulations. Planets with masses less than an Earth mass formed from a
low-mass ring resembling the solar system do not migrate inward even in the
evolving disk and remain near 1-au orbits, maintaining a high radial mass
concentration. On the other hand, planets with masses greater than an Earth
mass formed from a massive ring slowly migrate inward above the outward
migration region. As a result, the innermost planet can move to an orbit of
about 10 days. The simulation results also reproduce the characteristics (e.g.,
mass distribution, eccentricity, orbital separation) of the solar system and
super-Earth/sub-Neptune systems. Our model predicts that Earths and sub-Earths
formed by migration from rings at near the 1-au region are less abundant in the
close-in region.
