Outward migration from inner regions
Observations tell us that planets should have migrated from the location where they formed to their present
position. This migration process is typically invoked to explain the 'hot' planets close to the parent star, as it was
believed that migration typically occurs inward. Recent studies have opened the possibility of outward
migration depending either on the thermodynamical properties of the disk, or on rapid type III migration. In this contribution I will discuss the possiblity of sustained outward planetary migration in disks in order to explain the observed planets at distances of about 100au.