  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. Here, we aim to study the
effects of dust entrainment in photoevaporative winds and the ejection and drag
of dust due to effects caused by radiation from the central star. 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 account for
settling and advection of dust when calculating entrainment rates. In order to
prepare for future population studies with varying conditions, we explore a
wide range of disk-, photoevaporation-, and dust-parameters. We find that 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 1 m/s - 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 100 Myr. These
results highlight the importance of dust entrainment in winds as a solid mass
removal process. Furthermore, this model extension lies the basis for future
statistical studies of planet formation in their birth environment.
