Given the variety of properties found in planetary systems in our Galaxy, to understand disk evolution and planet formation, we must analyze general disk and host star properties measured in a large statistical sample of systems at different evolutionary stages and environments. Disks in nearby regions, without the presence of massive stars, evolve differently from disks in highly irradiated environments, where the Far-UV fields from OB-type stars disperse the closest protoplanetary disks from the outside in. Since the majority of (exo)planet host stars (including our Solar System) form in dense and massive stellar clusters in which the presence of OB-type stars dominates the radiation field, disk evolution studies must consider internal as well as external factors shaping the evolutionary path of protoplanetary disks in a complementary way.
During this talk, I will focus first on disks in the sigma-Orionis cluster. I will show the potential of using optical forbidden lines to study both internally and externally driven disk winds. In the case of sigma-Orionis, the innermost regions of the cluster are clearly affected by external irradiation from the massive system sigma-Ori, suggesting a coevolution of internal and external winds in these disks. I will then discuss the evolution of disks in more extreme environments, showing recent results obtained using VLT/MUSE observations of the Orion proplyds.