Planets form and obtain their compositions in disks of gas and dust around young stars. The
chemical compositions of these planet-forming disks regulate all aspects of planetary …

Planets form in disks of gas and dust around young stars. The disk molecular reservoirs and
their chemical evolution affect all aspects of planet formation, from the coagulation of dust …

Carbon is an essential element for life but how much can be delivered to young planets is
still an open question. The chemical characterization of planet-forming disks is a crucial step …

The disk mass is among the most important input parameter for every planet formation
model to determine the number and masses of the planets that can form. We present an …

Before the origin of simple cellular life, the building blocks of RNA (nucleotides) had to form
and polymerize in favorable environments on early Earth. At this time, meteorites and …

Flattened, rotating disks of cool dust and gas extending for tens to hundreds of astronomical
units are found around almost all low-mass stars shortly after their birth. These disks …

Ultracool dwarfs (UCD; T eff<∼ 3000 K) cool to settle on the main sequence after∼ 1 Gyr.
For brown dwarfs, this cooling never stops. Their habitable zones (HZ) thus sweeps inward …

Proxima b is a planet with a minimum mass of 1.3M⊕ orbiting within the habitable zone (HZ)
of Proxima Centauri, a very low-mass, active star and the Sun's closest neighbor. Here we …

Aims. The composition of planetary solids and gases is largely rooted in the processing of
volatile elements in protoplanetary disks. To shed light on the key processes, we carry out a …

The Kepler spacecraft has discovered a large number of planets with up to one-year periods
and down to terrestrial sizes. While the majority of the target stars are main-sequence dwarfs …