Most low-mass stars are born in transient OB associations, that is in clusters forming massive stars such as the Orion Nebula Cluster, rather than in low-mass star forming regions (SFRs), such as the Taurus-Auriga complex. The early evolution of our Solar System took place in the vicinity of massive stars. This implies that most low-mass stars and their protoplanetary disks are exposed to significant UV radiation fields and stellar winds from nearby OB stars during the early phases of their lives, when disks are still rich in dust and gas and in the process of forming planets. However, the overall effect of an UV-bright environment on disk chemistry and the planet formation process has not yet been studied in sufficient detail. The external UV radiation sets a photo-evaporative wind from the entire protoplanetary disk surface with a significant mass-loss rate that can dissipate gas and small dust grains shortly (~0.1 Myr), reducing the mass reservoir and timescale available for planet formation (if planets have not already formed). The external far-UV (FUV) radiation also changes the thermo-chemical structure of the disk with direct implications for the process of planet formation and properties of planets potentially forming in these disks. Hence, studies of the physical and chemical properties of young protoplanetary disks in a cluster environment, in the stages of planet formation, are of major importance for our understanding of protoplanetary disk evolution and dissipation, planet formation, and the origin of the Solar System.

As an Assistant Researcher at IA I will continue studying the physical structure, chemical composition (gas, dust, PAHs, ices) and kinematics of the circumstellar environment of young (0.1 – 5 Myr) low-mass stars—protoplanetary disks, winds, jets and outflows—found in massive star forming regions (d > 400 pc). By confronting the results with those for protoplanetary disks found in quiescent low-mass SFRs, we can assess the effects of the external environmental conditions on protoplanetary disk evolution and the implications for planet formation in the different environments. This goal will be achieved by combining multi-wavelength observations with cutting-edge Photodissociation Region (PDRs) 2D and 3D thermo-chemical models of protoplanetary disks. This is a pioneering and timely approach because of the high angular-resolution and sensitivity facilities finally available, operating from the optical to the mm-wavelength range. The project will be supported by ALMA and JWST archival data from SFRs surveys, JWST-ERS, GTO, and GO programs, and future observational campaigns (PI, Co-I) with the JWST, ALMA and the VLT. We will prepare for the arrival of the next generation of high-resolution instruments at the ELT and SKA which is expected for 2028. These will revolutionize proplyd studies in the most distant massive SFRs.