  No planets exist inside the orbit of Mercury and the terrestrial planets of
the solar system exhibit a localized configuration. According to thermal
structure calculation of protoplanetary disks, a silicate condensation line (~
1300 K) is located around 0.1 au from the Sun except for the early phase of
disk evolution, and planetesimals could have formed inside the orbit of
Mercury. A recent study of disk evolution that includes magnetically driven
disk winds showed that the gas disk obtains a positive surface density slope
inside ~ 1 au from the central star. In a region with positive midplane
pressure gradient, planetesimals undergo outward radial drift. We investigate
the radial drift of planetesimals and type I migration of planetary embryos in
a disk that viscously evolves with magnetically driven disk winds. We show a
case in which no planets remain in the close-in region. Radial drifts of
planetesimals are simulated using a recent disk evolution model that includes
effects of disk winds. The late stage of planet formation is also examined by
performing N-body simulations of planetary embryos. We demonstrate that in the
middle stage of disk evolution, planetesimals can undergo convergent radial
drift in a magnetorotational instability (MRI)-inactive disk, in which the
pressure maximum is created, and accumulate in a narrow ring-like region with
an inner edge at ~ 0.7 au from the Sun. We also show that planetary embryos
that may grow from the narrow planetesimal ring do not exhibit significant type
I migration in the late stage of disk evolution. The origin of the localized
configuration of the terrestrial planets of the solar system, in particular the
deficit of close-in planets, can be explained by the convergent radial drift of
planetesimals in disks with a positive pressure gradient in the close-in
region.
