Studying gaseous disks dissipating in stellar populations

JOSE GOMEZ; OCTAVIO M. GUILLERA; MARCELO M. MILLER BERTOLAMI; MARIA P. RONCO

Santiago de Chile

Workshop; 1st FARGO3D Workshop; 2024

Adolfo Ibáñez University

Protoplanetary disks are the sites of planet formation. For this reason their physical properties determine the planet formation process. A correct modelling of protoplanetary disks is, consequently, key to understanding planetary formation. Here we present a disk population synthesis study aimed at reproducing the available observational data of protoplanetary disks. We consider that disks evolve by viscous accretion and internal photoevaporation. The initial conditions, such as the masses and sizes of the discs, follow statistical distributions inferred from observations. We analyze the impact of stellar mass distributions and star formation rates on the time evolution of the fraction of stars with disks, and on the stellar mass accretion rates observed in young stars clusters. We show that, because massive stars dissipate their disks faster, the observed fraction of stars with disks in star-forming regions is dominated by disks around low-mass stars. From our models, we obtain a median disk lifetime of ~4.2 My, showing a very good agreement with observations.