2025/06/12 by Benoît Tabone, Tabone, Benoît, Giovanni Rosotti +51 · 7 citations
Physics and Astronomy · #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #Astronomy and Astrophysical Research
paper · pdf · doi:10.48550/arxiv.2506.10742
The architecture of planetary systems depends on the evolution of the disks in which they form. In this work, we develop a population synthesis approach to interpret the AGE-PRO measurements of disk gas mass and size considering two scenarios: turbulence-driven evolution with photoevaporative winds and MHD disk-wind-driven evolution. A systematic method is proposed to constrain the distribution of disk parameters from the disk fractions, accretion rates, disk gas masses, and CO gas sizes. We find that turbulence-driven accretion with initially compact disks (R0 ≃ 5-20~au), low mass-loss rates, and relatively long viscous timescales (tν,0 ≃ 0.4-3~Myr or αSS ≃ 2-4 × 10-4) can reproduce the disk fraction and gas sizes. However, the distribution of apparent disk lifetime defined as the MD/M_* ratio is severely overestimated by turbulence-driven models. On the other hand, MHD wind-driven accretion can reproduce the bulk properties of the disk populations from Ophiuchus to Upper Sco assuming compact disks with an initial magnetization of about β≃ 105 (αDW ≃ 0.5-1 × 10-3) and a magnetic field that declines with time. More studies are needed to confirm the low masses found by AGE-PRO, notably for compact disks that question turbulence-driven accretion. The constrained synthetic disk populations can now be used for realistic planet population models to interpret the properties of planetary systems on a statistical basis.