  Radial migration is an important process in the Galactic disk. A few open
clusters show some evidence on this mechanism but there is no systematic study.
In this work, we investigate the role of radial migration on the Galactic disk
based on a large sample of 146 open clusters with homogeneous metallicity and
age from Netopil et al. and kinematics calculated from Gaia DR2. The birth site
Rb, guiding radius Rg and other orbital parameters are calculated, and the
migration distance |Rg-Rb| is obtained, which is a combination of metallicity,
kinematics and age information. It is found that 44% open clusters have
|Rg-Rb|< 1 kpc, for which radial migration (churning) is not significant. Among
the remaining 56% open clusters with |Rg-Rb|> 1 kpc, young ones with t<1.0 Gyr
tend to migrate inward, while older clusters usually migrate outward. Different
mechanisms of radial migration between young and old clusters are suggested
based on their different migration rates, Galactic locations and orbital
parameters. For the old group, we propose a plausible way to estimate migration
rate and obtain a reasonable value of 1.5(+-0.5) kpc/Gyr based on ten
intermediate-age clusters at the outer disk, where the existence of several
special clusters implies its complicate formation history.
