Toward a population synthesis of disks and planets

Abstract

Context. Millimeter astronomy provides valuable information on the birthplaces of planetary systems. In order to compare theoretical models with observations, the dust component has to be carefully calculated. Aims. Here, we aim to study the effects of dust entrainment in photoevaporative winds, and the ejection and drag of dust due to the effects caused by radiation from the central star. Methods. We improved and extended the existing implementation of a two-population dust and pebble description in the global Bern/Heidelberg planet formation and evolution model. Modern prescriptions for photoevaporative winds were used and we accounted for settling and advection of dust when calculating entrainment rates. In order to prepare for future population studies with varying conditions, we explored a wide range of disk, photoevaporation, and dust parameters. Results. If dust can grow to pebble sizes, that is, if they are resistant to fragmentation or turbulence is weak, drift dominates and the entrained mass is small but larger than under the assumption of no vertical advection of grains with the gas flow. For the case of fragile dust shattering at velocities of 1m s−1 – as indicated in laboratory experiments –, an order of magnitude more dust is entrained, which becomes the main dust removal process. Radiation pressure effects disperse massive, dusty disks on timescales of a few hundred Myr. Conclusions. These results highlight the importance of dust entrainment in winds as a solid-mass removal process. Furthermore, this model extension lays the foundations for future statistical studies of the formation of planets in their birth environment.