We propose a set of standard assumptions for the modelling of Class II and III protoplanetary
disks, which includes detailed continuum radiative transfer, thermo-chemical modelling of …

The envelopes and disks that surround protostars reflect the initial conditions of star and
planet formation and govern the assembly of stellar masses. Characterizing these structures …

Recent years have seen growing interest in the streaming instability as a candidate
mechanism to produce planetesimals. However, these investigations have been limited to …

Context. Analyzing the properties of dust and its evolution in the early phases of star
formation is crucial to put constraints on the collapse and accretion processes as well as on …

We compute the evolution of interstellar dust in a hydrodynamic simulation of an isolated
disc galaxy. We newly implement the evolution of full grain size distribution by sampling 32 …

We perform numerical simulations of dusty, supersonic turbulence in molecular clouds. We
model 0.1, 1 and 10 μm sized dust grains at an initial dust-to-gas mass ratio of 1: 100 …

Context. Interstellar dust grain growth in dense clouds and protoplanetary disks, even when
moderate, affects the observed interstellar ice profiles as soon as a significant fraction of …

Beyond the snow line of protoplanetary discs and inside the dense core of molecular clouds,
the temperature of gas is low enough for water vapour to condense into amorphous ices on …

We have performed a survey for new members of the Ophiuchus cloud complex using high-
precision astrometry from the second data release of Gaia, proper motions measured with …

Context. Recently discovered scattered light from molecular cloud cores in the wavelength
range 3–5 μm (called “coreshine”) seems to indicate the presence of grains with sizes above …