Speaker
Description
Protoplanetary disks emerge as a consequence of the star formation process, and provide the foundational material for planets. The evolution of these disks is governed by a combination of internal processes linked to the central star, and external influences from the surrounding environment. Both pathways produce photoevaporative winds that drive disk dispersal from opposite directions. In massive star clusters, the UV radiation from massive OB stars irradiates disks externally, strongly affecting disk sizes, masses, and survival timescales. Until recently, the same emission lines were used for studying both internally and externally driven winds. However, their disentanglement is essential for building comprehensive models of disk evolution.
Here I present results based on the IFU data of 12 externally irradiated disks—proplyds, in the Orion Nebula Cluster acquired with VLT/MUSE in Narrow Field Mode. These observations allow us to pinpoint where emission lines of various species and ionization degrees arise from within the proplyd, and determine signatures unique to external photoevaporation. I will also show how these results serve as benchmarks for photoevaporation models. Characterizing the proplyds in relative proximity sets the precedent for future studies in more distant and massive star-forming regions.