Unified Simulations of Planetary Formation and Atmospheric Evolution: Effects of Pebble Accretion, Giant Impacts, and Stellar Irradiation on Super-Earth Formation
@article{Ogihara2020UnifiedSO, title={Unified Simulations of Planetary Formation and Atmospheric Evolution: Effects of Pebble Accretion, Giant Impacts, and Stellar Irradiation on Super-Earth Formation}, author={Masahiro Ogihara and Yasunori Hori}, journal={The Astrophysical Journal}, year={2020}, volume={892} }
A substantial number of super-Earths have been discovered, and atmospheres of transiting super-Earths have also been observed by transmission spectroscopy. Several lines of observational evidence indicate that most super-Earths do not possess massive H2/He atmospheres. However, accretion and retention of less massive atmospheres on super-Earths challenge planet formation theory. We consider the following three mechanisms: (i) envelope heating by pebble accretion, (ii) mass loss during giant…
12 Citations
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References
SHOWING 1-10 OF 99 REFERENCES
IN SITU ACCRETION OF HYDROGEN-RICH ATMOSPHERES ON SHORT-PERIOD SUPER-EARTHS: IMPLICATIONS FOR THE KEPLER-11 PLANETS
- Physics, Geology
- 2012
Motivated by recent discoveries of low-density super-Earths with short orbital periods, we have investigated in situ accretion of H-He atmospheres on rocky bodies embedded in dissipating warm disks,…
Hydrodynamics of embedded planets’ first atmospheres – III. The role of radiation transport for super-Earth planets
- Physics, Geology
- 2017
The population of close-in super-Earths, with gas mass fractions of up to 10 per cent represents a challenge for planet formation theory: how did they avoid runaway gas accretion and collapsing to…
Formation of planetary systems by pebble accretion and migration
- Geology, PhysicsAstronomy & Astrophysics
- 2021
At least 30% of main sequence stars host planets with sizes of between 1 and 4 Earth radii and orbital periods of less than 100 days. We use N-body simulations including a model for gas-assisted…
N-body simulations of planet formation via pebble accretion I: First Results
- Geology, Physics
- 2017
Context. Planet formation with pebbles has been proposed to solve a couple of long-standing issues in the classical formation model. Some sophisticated simulations have been done to confirm the…
The Deposition of Heavy Elements in Giant Protoplanetary Atmospheres: The Importance of Planetesimal–Envelope Interactions
- Physics, GeologyThe Astrophysical Journal
- 2019
In the standard model for giant planet formation, the planetary growth begins with accretion of solids, followed by a buildup of a gaseous atmosphere as more solids are accreted and, finally, by…
Enhanced atmospheric loss on protoplanets at the giant impact phase in the presence of oceans
- Geology, PhysicsNature
- 2005
It is suggested that remnants of the noble-gas rich proto-atmosphere survived on Venus, but not on Earth, because most of the neon must have escaped from both planets’ atmospheres later to yield the observed ratio of neon to argon.
A reassessment of the in situ formation of close-in super-Earths
- Geology, Physics
- 2015
Context. A large fraction of stars host one or multiple close-in super-Earth planets. There is an active debate about whether these planets formed in situ or at greater distances from the central…
How planets grow by pebble accretion
- Physics, GeologyAstronomy & Astrophysics
- 2019
During their formation, planets form large, hot atmospheres due to the ongoing accretion of solids. It has been customary to assume that all solids end up at the center, constituting a “core” of…
Formation of close-in super-Earths in evolving protoplanetary disks due to disk winds
- Geology, PhysicsAstronomy & Astrophysics
- 2018
Context. Planets with masses larger than about 0.1 M⊕ undergo rapid inward migration (type I migration) in a standard protoplanetary disk. Recent magnetohydrodynamical simulations revealed the…
Formation of Giant Planets
- Geology, Physics
- 1982
This is a descriptive and non-mathematical summary of giant planet formation theories. There are two end-member models, core accretion and disk instability. In the core accretion model, several to…