A highly settled disk around oph163131
M Villenave, KR Stapelfeldt, G Duchêne… - The Astrophysical …, 2022 - iopscience.iop.org
High dust density in the midplane of protoplanetary disks is favorable for efficient grain
growth and can allow fast formation of planetesimals and planets, before disks dissipate …
growth and can allow fast formation of planetesimals and planets, before disks dissipate …
Separating gas-giant and ice-giant planets by halting pebble accretion
M Lambrechts, A Johansen, A Morbidelli - Astronomy & Astrophysics, 2014 - aanda.org
In the solar system giant planets come in two flavours: gas giants (Jupiter and Saturn) with
massive gas envelopes, and ice giants (Uranus and Neptune) with much thinner envelopes …
massive gas envelopes, and ice giants (Uranus and Neptune) with much thinner envelopes …
The effect of gas drag on the growth of protoplanets-analytical expressions for the accretion of small bodies in laminar disks
CW Ormel, HH Klahr - Astronomy & Astrophysics, 2010 - aanda.org
Planetary bodies form by accretion of smaller bodies. It has been suggested that a very
efficient way to grow protoplanets is by accreting particles of size≪ km (eg, chondrules …
efficient way to grow protoplanets is by accreting particles of size≪ km (eg, chondrules …
Planetesimal formation starts at the snow line
J Drążkowska, Y Alibert - Astronomy & Astrophysics, 2017 - aanda.org
Context. The formation stage of planetesimals represents a major gap in our understanding
of the planet formation process. Late-stage planet accretion models typically make arbitrary …
of the planet formation process. Late-stage planet accretion models typically make arbitrary …
Rapid coagulation of porous dust aggregates outside the snow line: a pathway to successful icy planetesimal formation
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 …
formation in protoplanetary disks. We re-examine this problem by considering the porosity …
The New Generation Planetary Population Synthesis (NGPPS)-II. Planetary population of solar-like stars and overview of statistical results
Context. Planetary formation and evolution is a combination of multiple interlinked
processes. Constraining the mechanisms observationally requires statistical comparison to …
processes. Constraining the mechanisms observationally requires statistical comparison to …
Hf–W–Th evidence for rapid growth of Mars and its status as a planetary embryo
N Dauphas, A Pourmand - Nature, 2011 - nature.com
Terrestrial planets are thought to have formed through collisions between large planetary
embryos of diameter∼ 1,000–5,000 km. For Earth, the last of these collisions involved an …
embryos of diameter∼ 1,000–5,000 km. For Earth, the last of these collisions involved an …
The formation of Jupiter by hybrid pebble–planetesimal accretion
The standard model for giant planet formation is based on the accretion of solids by a
growing planetary embryo, followed by rapid gas accretion once the planet exceeds a so …
growing planetary embryo, followed by rapid gas accretion once the planet exceeds a so …
On the water delivery to terrestrial embryos by ice pebble accretion
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 …
interior to the Earth's orbit in a late stage of nebula evolution. In this late stage, a significant …
Giant planet formation, evolution, and internal structure
The large number of detected giant exoplanets offers the opportunity to improve our
understanding of the formation mechanism, evolution, and interior structure of gas giant …
understanding of the formation mechanism, evolution, and interior structure of gas giant …