Disk population synthesis

2018-11-16T05:58:41Z (GMT) by Zormpas, Apostolos
Based on recent surveys of protoplanetary disks in dust continuum, with observed dust disk life times, we reproduce observational results and more specifically, the size-luminosity relation from Tripathi et al. 2017. Using 1-D simulations we simulate disks with gas and dust evolution, for cases with and without an axisymmetric stationary pressure bump and we let them evolve up to 3 Myr. We vary a broad range of different initial conditions on alpha, characteristic radius, disk mass and fragmentation velocity and we calculate the disk emission using dust opacities and simple one-zone models. Choosing only the disks that lie within one standard deviation from the size-luminosity relation, we find that both cases have a subset that agrees with the observations and favor higher luminosities. Moreover, we manage to constrain the parameter range for both bump cases. Furthermore, we expect to use pressure bumps with finite life time and improve upon previous works (e.g. Pinilla et al. 2012a). By comparing with observational data, we plan to constrain bump amplitudes, bump sizes and life times. By using parameterized models of planetesimal formation (Drazkowska & Dullemond 2014), we plan to calculate how much dust is transformed into planetesimals. This will allow us to investigate how the planetesimal formation can affect the existing results.