Planet-forming disc evolution is not independent of the star formation and feedback process
in giant molecular clouds. In particular, OB stars emit UV radiation that heats and disperses …

Context. The growth of dust grains from sub-μm to mm and cm sizes is the first step towards
the formation of planetesimals. Theoretical models of grain growth predict that dust …

Context. The formation of planets strongly depends on the total amount as well as on the
spatial distribution of solids in protoplanetary disks. Thanks to the improvements in …

We estimate the mass-loss rates of photoevaporative winds launched from the outer edge of
protoplanetary discs impinged by an ambient radiation field. We focus on mild/moderate …

We discuss how the range of information available from microparticle analysis can be
extended in a number of applications by measuring a specific set of optical properties of …

The formation of gas giant planets must occur during the first few Myr of a star's lifetime,
when the protoplanetary disc still contains sufficient gas to be accreted on to the planetary …

ABSTRACT A necessary first step for dust removal in protoplanetary disc winds is the
delivery of dust from the disc to the wind. In the case of ionized winds, the disc and wind are …

ABSTRACT We present Very Large Telescope/Multi-Unit Spectroscopic Explorer Narrow
Field Mode observations of a pair of disc-bearing young stellar objects towards the Orion …

Most stars form in a clustered environment. Therefore, it is important to assess how this
environment influences the evolution of protoplanetary discs around young stars. In turn, this …

The first stages of planet formation usually occur when the host star is still in a (relatively)
dense star-forming region, where the effects of the external environment may be important …