Astro Seminar: The impact of ionized winds, photoevaporation and stellar multiplicity on the evolution of disks around massive stars

Jets and disk winds originate from material with excess angular momentum that is ejected from the accretion disk of forming stars. However, the mechanisms by which these components are launched, and their impact on the gas in the innermost regions of young stellar objects, remain largely unknown. At the same time, accretion takes place through the infall of the envelope and molecular streamers. Massive stars are also commonly found in multiple systems, which may further influence the structure and evolution of their disks. In this talk, I will present the results of my PhD research, which investigates these processes. The main project involves modeling hydrogen Radio Recombination Line masers observed with ALMA toward the massive star MWC 349A. These observations provide a detailed view of its ionized environment, with positional accuracy down to scales of a few astronomical units. Our analysis of the H30α line and the spatially resolved H26α maser using our non-LTE radiative transfer code, MORELI, has revealed a high-velocity jet embedded within the ionized wind, consistent with magneto-hydrodynamic (MHD) launching models. I will also present evidence for a potential new outflow driven by the Class 0/I binary [BHB2007]11, based on molecular line data obtained with ALMA as part of the FAUST Large Program. Finally, I will present our currently ongoing work, which consists of modeling VLTI/GRAVITY observations of a sample of massive young stellar objects. This work aims to identify stellar companions and disk winds that may influence the dispersal of their inner circumstellar disks."