105 citations · 379 across the 11 of their papers we have counts for
11 papers
The influence of a static planetary atmosphere on spin transfer during pebble accretion
M. J. Yzer, R. G. Visser, C. Dominik
We study the effect an atmosphere has on pebble orbits and spin build-up on a planet's surface during pebble accretion in the extreme case of a static atmosphere. We numerically in…
SHAMPOO: A stochastic model for tracking dust particles under the influence of non-local disk processes
M. Oosterloo, I. Kamp, W. van Westrenen +1
The abundances of CHNOS are crucial for the composition of planets. At the onset of planet formation, large amounts of these elements are stored in ices on dust grains in planet-fo…
Forming equal mass planetary binaries via pebble accretion
T. J. Konijn, R. G. Visser, C. Dominik +1
Binary solar system objects are common and range from satellite systems with very large mass ratios to mass ratios very close to unity. A well-known example of a binary i…
The radial structure of planetary bodies formed by the streaming instability
Rico G. Visser, Joanna Drążkowska, Carsten Dominik
Comets and small planetesimals are believed to contain primordial building blocks in the form of millimeter to centimeter sized pebbles. One of the viable growing mechanisms to for…
Spinning up planetary bodies by pebble accretion
R. G. Visser, C. W. Ormel, C. Dominik +1
Most major planetary bodies in the solar system rotate in the same direction as their orbital motion: their spin is prograde. Theoretical studies to explain the direction as well a…
Contribution of the core to the thermal evolution of sub-Neptunes
A. Vazan, C. W. Ormel, L. Noack +1
Sub-Neptune planets are a very common type of planets. They are inferred to harbour a primordial (H/He) envelope, on top of a (rocky) core, which dominates the mass. Here, we inves…
Radial and vertical dust transport inhibit refractory carbon depletion in protoplanetary disks
L. Klarmann, C. W. Ormel, C. Dominik
The Earth is strongly depleted in carbon compared to the dust in the ISM, implying efficient removal of refractory carbon before parent body formation. It has been argued that grai…
Effect of Core Cooling on the Radius of Sub-Neptune Planets
A. Vazan, C. W. Ormel, C. Dominik
Sub-Neptune planets are very common in our galaxy and show a large diversity in their mass-radius relation. In sub-Neptunes most of the planet mass is in the rocky part (hereafter…
A panoptic model for planetesimal formation and pebble delivery
Sebastiaan Krijt, Chris W. Ormel, Carsten Dominik +1
The journey from dust particle to planetesimal involves physical processes acting on scales ranging from micrometers (the sticking and restructuring of aggregates) to hundreds of a…
Erosion and the limits to planetesimal growth
Sebastiaan Krijt, Chris W. Ormel, Carsten Dominik +1
The coagulation of microscopic dust into planetesimals is the first step towards planet formation. The size and shape of the growing aggregates determine the efficiency of this ear…
Stirring up the dust: A dynamical model for halo-like dust clouds in transitional disks
Sebastiaan Krijt, Carsten Dominik
A small number of young stellar objects show signs of a halo-like structure of optically thin dust. This halo or torus is located within a few AU of the star, but its origin has no…