Water ice is one of the most abundant materials in dense molecular clouds and in the outer
reaches of protoplanetary disks. In contrast to other materials (eg, silicates), water ice is …

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 …

Context. Several barriers have been proposed in planetesimal formation theory: bouncing,
fragmentation, and radial drift problems. Understanding the structure evolution of dust …

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

Context. Dust grains coagulate to form dust aggregates in protoplanetary disks. Their
porosity can be extremely high in the disks. Although disk emission may come from fluffy …

The processes that govern the evolution of dust and water (in the form of vapor or ice) in
protoplanetary disks are intimately connected. We have developed a model that simulates …

In protoplanetary disks, micron-sized dust grains coagulate to form highly porous dust
aggregates. Because the optical properties of these aggregates are not completely …

Context. The journey from dust particle to planetesimal involves physical processes acting
on scales ranging from micrometers (the sticking and restructuring of aggregates) to …

Context. The coagulation of microscopic dust into planetesimals is the first step towards the
formation of planets. The composition, size, and shape of the growing aggregates determine …

Abstract 1I/'Oumuamua is the first interstellar interloper to be detected, and it shows a non-
gravitational acceleration that cannot be accounted for by outgassing, given the strict upper …