
Thursday, 19th February 2026, 12:00 (CET) (Auditorio/Zoom)
Stars form through the accretion of material from circumstellar disks, which, at the same time, are the birthplaces of planetary systems. During the formation and early evolution of the star, the disk is subject to multiple processes that alter its physical and chemical state, hereafter having an impact on the conditions for planet formation. To enable accretion, disks eject winds and jets that enrich the gas-phase chemistry of the circumstellar envelope by sputtering dust grains and by triggering chemical reactions. The envelope provides mass to the disk through infall and streamers, showing a cyclic exchange of material whose kinematics and chemistry are not completely understood to date. At later stages, the ionizing radiation from the star can disperse the disk from the inside out, which is thought to be particularly effective for the most massive stars. Furthermore, as many stars are born in multiple systems, interactions between companions can sweep internal regions of the disk, limiting its ability to form planets. We study these processes by combining observations from state-of-the-art telescopes such as ALMA and the VLTI, in combination with models. Among our sample, we find that disks survive until late stages, keeping material available to form planets even in the most massive systems. Obtaining high-resolution observations at multiple wavelengths and analyzing them with detailed models is essential to fully understand these dispersal processes.
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