How Flow Isolation May Set the Mass Scale for Super-Earth Planets

@article{Rosenthal2020HowFI,
  title={How Flow Isolation May Set the Mass Scale for Super-Earth Planets},
  author={M. Rosenthal and R. Murray-Clay},
  journal={The Astrophysical Journal},
  year={2020},
  volume={898},
  pages={108}
}
Much recent work on planet formation has focused on the growth of planets by accretion of grains whose aerodynamic properties make them marginally coupled to the nebular gas, a theory commonly referred to as "pebble accretion". While pebble accretion can ameliorate some of the issues presented by growth by purely gravitational processes, it has other issues when compared with observations of exoplanetary systems. A particular concern is the preponderance of planets that end their growth as… Expand

Figures from this paper

Exploring the conditions for forming cold gas giants via planetesimal accretion
The formation of cold gas giants akin to Jupiter and Saturn in orbit and mass is a major challenge for planetesimal-driven core accretion models, due to the low core growth rates far from the star.Expand
Formation of Giant Planet Satellites
Recent analyses have shown that the concluding stages of giant planet formation are accompanied by the development of large-scale meridional flow of gas inside the planetary Hill sphere. ThisExpand
Erosion-driven Size Redistribution of Protoplanetary Disk Solids and the Onset of Streaming Instability and Pebble Accretion
The formation of the first planetesimals and the final growth of planetary cores relies on the abundance of small pebbles. The efficiencies of both the streaming instability (SI) process, suggestedExpand
How planets grow by pebble accretion
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" ofExpand
Requirements for gravitational collapse in planetesimal formation --- the impact of scales set by Kelvin-Helmholtz and nonlinear streaming instability.
The formation of planetesimals is an unsolved problem in planet formation theory. A prominent scenario for overcoming dust growth barriers in dead zones is the gravitational collapse of locallyExpand
Sub-Neptune formation: the view from resonant planets
The orbital period ratios of neighbouring sub-Neptunes are distributed asymmetrically near first-order resonances. There are deficits of systems---"troughs" in the period ratio histogram---just shortExpand

References

SHOWING 1-10 OF 72 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 anExpand
The radial dependence of pebble accretion rates: A source of diversity in planetary systems I. Analytical formulation
Context. The classical "planetesimal" accretion scenario for the formation of planets has recently evolved with the idea that "pebbles", centimeter- to meter-sized icy grains migrating inExpand
Formation of planetary systems by pebble accretion and migration. How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
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 thatExpand
A Balanced Budget View on Forming Giant Planets by Pebble Accretion
Pebble accretion refers to the assembly of rocky planet cores from particles whose velocity dispersions are damped by drag from circumstellar disc gas. Accretion cross-sections can approach maximalExpand
The growth of planets by pebble accretion in evolving protoplanetary discs
The formation of planets depends on the underlying protoplanetary disc structure, which in turn influences both the accretion and migration rates of embedded planets. The disc itself evolves on timeExpand
Rapid growth of gas-giant cores by pebble accretion
The observed lifetimes of gaseous protoplanetary discs place strong constraints on gas and ice giant formation in the core accretion scenario. The approximately 10-Earth-mass solid core responsibleExpand
Growing the terrestrial planets from the gradual accumulation of submeter-sized objects
TLDR
It is shown that a new mode of planet formation known as “Viscous Stirred Pebble Accretion,” which has recently been shown to produce the giant planets, also naturally explains the small size of Mars and the low mass of the asteroid belt, and there is a unified model that can be used to explain all of the basic properties of the authors' solar system. Expand
Formation of planetary systems by pebble accretion and migration
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 pebbleExpand
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 lineExpand
Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
The formation of planetary cores must proceed rapidly in order for the giant planets to accrete their gaseous envelopes before the dissipation of the protoplanetary gas disc (less than or similar toExpand
...
1
2
3
4
5
...