The solid content of circumstellar disks is inherited from the interstellar medium: dust
particles of at most a micrometer in size. Protoplanetary disks are the environment where …

The latest observation of HL Tau by ALMA revealed spectacular concentric dust rings in its
circumstellar disk. We attempt to explain the multiple ring structure as a consequence of …

Many processes during the evolution of protoplanetary disks and during planet formation are
highly sensitive to the sizes of dust particles that are present in the disk: the efficiency of dust …

Accumulation of dust and ice particles into planetesimals is an important step in the planet
formation process. Planetesimals are the seeds of both terrestrial planets and the solid cores …

Rapid orbital drift of macroscopic dust particles is one of the major obstacles to planetesimal
formation in protoplanetary disks. We re-examine this problem by considering the porosity …

Context. The formation of planetesimals is often accredited to the collisional sticking of dust
grains. The exact process is unknown, as collisions between larger aggregates tend to lead …

Standard accretion disk models suggest that the snow line in the solar nebula migrated
interior to the Earth's orbit in a late stage of nebula evolution. In this late stage, a significant …

We perform smoothed particle hydrodynamics (SPH) simulations of an isolated galaxy with a
new treatment for dust formation and destruction. To this aim, we treat dust and metal …

Pebble accretion is the mechanism in which small particles (“pebbles”) accrete onto big
bodies (planetesimals or planetary embryos) in gas-rich environments. In pebble accretion …

Context. Collisional growth of dust aggregates is an essential process in forming
planetesimals in protoplanetary disks, but disruption through high-velocity collisions …