The evolution of protoplanetary disc radii and disc masses in star-forming regions

Protoplanetary discs are crucial to understanding how planets form and evolve, but these objects subject the vagaries of birth environments their host stars. In particular, photoionising radiation from massive stars has been shown be an effective agent in disrupting protoplanetary discs. External photoevaporation leads inward evolution radii discs, whereas internal viscous disc causes evolve outwards. We couple N-body simulations star-forming regions with a post-processing analysis determine radius mass distributions young regions. To consistent observations, we find that initial must order 100au, even though readily destroyed by Furthermore, observed distribution Orion Nebula Cluster is more moderate stellar densities (100M$_\odot$ pc$^{-3}$), tension dynamical models posit much higher inital for ONC. cannot reproduce Lupus region if its external photoevaporation. A detailed comparison not possible due well-documented uncertainties determining ages pre-main sequence (disc-hosting)