Formation of planetary systems by pebble accretion and migration

@article{Bitsch2021FormationOP,
  title={Formation of planetary systems by pebble accretion and migration},
  author={Bertram Bitsch and Andr{\'e} Izidoro and Anders Johansen and Sean N. Raymond and Alessandro Morbidelli and Michiel Lambrechts and Seth Andrew Jacobson},
  journal={Astronomy \& Astrophysics},
  year={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 pebble accretion and disk–planet tidal interaction to study the formation of super-Earth systems. We show that the integrated pebble mass reservoir creates a bifurcation between hot super-Earths or hot-Neptunes (≲15 M⊕) and super-massive planetary cores potentially able to become gas giant planets (≳15… 
The eccentricity distribution of giant planets and their relation to super-Earths in the pebble accretion scenario
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The observed correlation between outer giant planets and inner super-Earths is emerging as an important constraint on planet formation theories. In this study, we focus on Kepler-167, which is
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We herein develop a new simple model for giant planet formation, which predicts the final mass of a giant planet born in a given disk, by adding the disk mass loss due to photoevaporation and a new
Inner rocky super-Earth formation: distinguishing the formation pathways in viscously heated and passive discs
  • B. Bitsch
  • Physics, Geology
    Astronomy & Astrophysics
  • 2019
Observations have revealed that super-Earths (planets up to 10 Earth masses) are the most abundant type of planets in the inner systems. Their formation is strongly linked to the structure of the
Unified Simulations of Planetary Formation and Atmospheric Evolution. II. Rapid Disk Clearing by Photoevaporation Yields Low-mass Super-Earth Atmospheres
Super-Earths possess low-mass H$_2$/He atmospheres (typically less than 10% by mass). However, the origins of super-Earth atmospheres have not yet been ascertained. We investigate the role of rapid
Planet formation by pebble accretion in ringed disks
Context. Pebble accretion is expected to be the dominant process for the formation of massive solid planets, such as the cores of giant planets and super-Earths. So far, this process has been studied
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The physics of planet formation is investigated using a population synthesis approach. We develop a simple model for planetary growth including pebble and gas accretion, and orbital migration in an
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