Formation of planetary systems by pebble accretion and migration

@article{Izidoro2018FormationOP,
  title={Formation of planetary systems by pebble accretion and migration},
  author={Andr{\'e} Izidoro and Bertram Bitsch and Sean N. Raymond and Anders Johansen and Alessandro Morbidelli and Michiel Lambrechts and Seth Andrew Jacobson},
  journal={arXiv: Earth and Planetary Astrophysics},
  year={2018}
}
At least 30% of main sequence stars host planets with sizes 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 ($\lesssim15M_{\oplus}$) and super-massive planetary cores potentially able to become gas giant… 
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References

SHOWING 1-10 OF 237 REFERENCES
Formation of planetary systems by pebble accretion and migration: growth of gas giants
Giant planets migrate though the protoplanetary disc as they grow their solid core and attract their gaseous envelope. Previously, we have studied the growth and migration of an isolated planet in an
Formation of planetary systems by pebble accretion and migration
Super-Earths – planets with sizes between the Earth and Neptune – are found in tighter orbits than that of the Earth around more than one third of main sequence stars. It has been proposed that
Promoted mass growth of multiple, distant giant planets through pebble accretion and planet–planet collision
We propose a pebble-driven planet formation scenario to form giant planets with high multiplicity and large orbital distances in the early gas disc phase. We perform N-body simulations to
Formation of close in Super-Earths \& Mini-Neptunes: Required Disk Masses \& Their Implications
Recent observations by the {\it Kepler} space telescope have led to the discovery of more than 4000 exoplanet candidates consisting of many systems with Earth- to Neptune-sized objects that reside
Challenges in Forming the Solar System's Giant Planet Cores via Pebble Accretion
Though ~10 Earth mass rocky/icy cores are commonly held as a prerequisite for the formation of gas giants, theoretical models still struggle to explain how these embryos can form within the lifetimes
Forming Planets via Pebble Accretion
The detection and characterization of large populations of pebbles in protoplanetary disks have motivated the study of pebble accretion as a driver of planetary growth. This review covers all aspects
Pebble Accretion and the Diversity of Planetary Systems
I examine the standard model of planet formation, including pebble accretion, using numerical simulations. Planetary embryos large enough to become giant planets do not form beyond the ice line
Migration and the Formation of Systems of Hot Super-Earths and Neptunes
The existence of extrasolar planets with short orbital periods suggests that planetary migration induced by tidal interaction with the protoplanetary disk is important. Cores and terrestrial planets
Global models of planetary system formation in radiatively-inefficient protoplanetary discs
We present the results of N-body simulations of planetary system formation in radiatively-inefficient disc models, where positive corotation torques may counter the rapid inward migration of low-mass
Formation of short-period planets by disc migration
Protoplanetary discs are thought to be truncated at orbital periods of around 10 d. Therefore, the origin of rocky short-period planets with P < 10 d is a puzzle. We propose that many of these
...
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