Sebastian Lorek
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View article: Super-Earth formation in systems with cold giants
Super-Earth formation in systems with cold giants Open
Around our Sun, terrestrial planets did not reach masses higher than that of Earth, while super-Earths are found to orbit approximately every other solar-like star. It remains unclear what divides these super-Earth systems from those that …
View article: Super-Earth formation in systems with cold giants
Super-Earth formation in systems with cold giants Open
Around our Sun, terrestrial planets did not grow beyond Earth in mass, while super-Earths are found to orbit approximately every other solar-like star. It remains unclear what divides these super-Earth systems from those that form terrestr…
View article: UV processing of icy pebbles in the outer parts of VSI-turbulent disks
UV processing of icy pebbles in the outer parts of VSI-turbulent disks Open
Icy dust particles emerge in star-forming clouds and are subsequently incorporated in protoplanetary disks, where they coagulate into larger pebbles up to millimeter in size. In the disk midplane, ices are shielded from UV radiation, but m…
View article: UV-processing of icy pebbles in the outer parts of VSI-turbulent disks
UV-processing of icy pebbles in the outer parts of VSI-turbulent disks Open
Icy dust particles emerge in star-forming clouds and are subsequently incorporated in protoplanetary disks, where they coagulate into larger pebbles up to mm in size. In the disk midplane, ices are shielded from UV radiation, but moderate …
View article: Formation of flattened planetesimals by gravitational collapse of rotating pebble clouds
Formation of flattened planetesimals by gravitational collapse of rotating pebble clouds Open
Planetesimals are believed to form by the gravitational collapse of aerodynamically concentrated clumps of pebbles. Many properties of the objects in the cold classical Kuiper belt -- such as binarity, rotation, and size distribution -- ar…
View article: Formation of flattened planetesimals by gravitational collapse of rotating pebble clouds
Formation of flattened planetesimals by gravitational collapse of rotating pebble clouds Open
Planetesimals are believed to form by the gravitational collapse of aerodynamically concentrated clumps of pebbles. Many properties of the objects in the cold classical Kuiper belt – such as binarity, rotation, and size distribution – are …
View article: Growing the seeds of pebble accretion through planetesimal accretion
Growing the seeds of pebble accretion through planetesimal accretion Open
We explore the growth of planetary embryos by planetesimal accretion up to and beyond the point at which pebble accretion becomes efficient at the so-called Hill-transition mass. Both the transition mass and the characteristic mass of plan…
View article: Growing the seeds of pebble accretion through planetesimal accretion
Growing the seeds of pebble accretion through planetesimal accretion Open
We explore the growth of planetary embryos by planetesimal accretion up to and beyond the point where pebble accretion becomes efficient at the so-called Hill-transition mass. Both the transition mass and the characteristic mass of planete…
View article: A close-encounter method for simulating the dynamics of planetesimals
A close-encounter method for simulating the dynamics of planetesimals Open
The dynamics of planetesimals plays an important role in planet formation because their velocity distribution sets the growth rate to larger bodies. When planetesimals form in the gaseous environment of protoplanetary discs, their orbits a…
View article: Comet Formation in the Framework of Streaming Instability
Comet Formation in the Framework of Streaming Instability Open
The bodies of the solar system formed 4.6 Gyr ago in the protoplanetary disk around the young protosun. Starting with submicrometre-sized dust and ice grains, collisions and coalescence led to the formation of aggregates, planetesimals, an…
View article: Local growth of dust- and ice-mixed aggregates as cometary building blocks in the solar nebula
Local growth of dust- and ice-mixed aggregates as cometary building blocks in the solar nebula Open
Context. Comet formation by gravitational instability requires aggregates that trigger the streaming instability and cluster in pebble-clouds. These aggregates form as mixtures of dust and ice from (sub-)micrometre-sized dust and ice grain…
View article: Comet formation in collapsing pebble clouds
Comet formation in collapsing pebble clouds Open
\n Context. Comets are remnants of the icy planetesimals that formed beyond the ice line in the solar nebula. Growing from μm-sized dust and ice particles to km-sized objects is, however, difficult because of growth barriers and time scale…
View article: Comet formation in collapsing pebble clouds. What cometary bulk density implies for the cloud mass and dust-to-ice ratio
Comet formation in collapsing pebble clouds. What cometary bulk density implies for the cloud mass and dust-to-ice ratio Open
Comets are remnants of the icy planetesimals that formed beyond the ice line in the Solar Nebula. Growing from micrometre-sized dust and ice particles to km-sized objects is, however, difficult because of growth barriers and time scale con…