Gas accretion on to planetary cores: three-dimensional self-gravitating radiation hydrodynamical calculations

@article{Ayliffe2009GasAO,
  title={Gas accretion on to planetary cores: three-dimensional self-gravitating radiation hydrodynamical calculations},
  author={Ben A. Ayliffe and Matthew R. Bate},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2009},
  volume={393},
  pages={49-64}
}
  • B. Ayliffe, M. Bate
  • Published 8 November 2008
  • Physics
  • Monthly Notices of the Royal Astronomical Society
We present results from three-dimensional, self-gravitating radiation hydrodynamical models of gas accretion by planetary cores. In some cases, the accretion flow is resolved down to the surface of the solid core – the first time such simulations have been performed. We investigate the dependence of the gas accretion rate upon the planetary core mass, and the surface density and opacity of the encompassing protoplanetary disc. Accretion of planetesimals is neglected. We find that high-mass… Expand
Global 3D radiation-hydrodynamic simulations of gas accretion: Opacity-dependent growth of Saturn-mass planets
The full spatial structure and temporal evolution of the accretion flow into the envelopes of growing gas giants in their nascent discs is only accessible in simulations. Such simulations areExpand
Quasi-static contraction during runaway gas accretion onto giant planets
Gas-giant planets, like Jupiter and Saturn, acquire massive gaseous envelopes during the approximately 3 Myr-long lifetimes of protoplanetary discs. In the core accretion scenario, the formation of aExpand
Gas accretion onto a protoplanet and formation of a gas giant planet
We investigate gas accretion on to a protoplanet, by considering the thermal effect of gas in three-dimensional hydrodynamical simulations, in which the wide region from a protoplanetary gas disc toExpand
Accretion in giant planet circumplanetary discs
During the final growth phase of giant planets, accretion is thought to be controlled by a surrounding circumplanetary disk. Current astrophysical accretion disk models rely on hydromagneticExpand
ACCRETION OF JUPITER-MASS PLANETS IN THE LIMIT OF VANISHING VISCOSITY
In the core-accretion model, the nominal runaway gas-accretion phase brings most planets to multiple Jupiter masses. However, known giant planets are predominantly Jupiter mass bodies. ObtainingExpand
Circum-planetary discs as bottlenecks for gas accretion onto giant planets
With hundreds of exoplanets detected, it is necessary to revisit giant planets accretion models to explain their mass distribution. In particular, formation of sub-jovian planets remains unclear,Expand
ACCRETION OF GAS ONTO GAP-OPENING PLANETS AND CIRCUMPLANETARY FLOW STRUCTURE IN MAGNETIZED TURBULENT DISKS
We have performed three-dimensional magnetohydrodynamical simulations of stellar accretion disks, using the PLUTO code, and studied the accretion of gas onto a Jupiter-mass planet and the structureExpand
Feedback-limited accretion: variable luminosity from growing planets
Planets form in discs of gas and dust around stars, and continue to grow by accretion of disc material while available. Massive planets clear a gap in their protoplanetary disc, but can still accreteExpand
Three-dimensional radiation-hydrodynamics calculations of the envelopes of young planets embedded in protoplanetary disks
We perform global three-dimensional (3D) radiation-hydrodynamics calculations of the envelopes surrounding young planetary cores of 5, 10, and 15 Earth masses, located in a protoplanetary disk at 5Expand
Exploring the conditions required to form giant planets via gravitational instability in massive protoplanetary discs
We carry out global three-dimensional radiation hydrodynamical simulations of self-gravitating accretion discs to determine if, and under what conditions, a disc may fragment to form giant planets.Expand
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 55 REFERENCES
Mass flow and accretion through gaps in accretion discs
We study the structure and dynamics of the gap created by a protoplanet in an accretion disc. The hydrodynamic equations for a flat, two-dimensional, non-self-gravitating protostellar accretion discExpand
Timescales for planetary accretion and the structure of the protoplanetary disk
Abstract This paper outlines a unified scenario for Solar System formation consistent with astrophysical constraints. Jupiter's core could have grown by runaway accretion of planetesimals to a massExpand
Gas Flow across Gaps in Protoplanetary Disks
We analyze the gas accretion flow through a planet-produced gap in a protoplanetary disk. We adopt the α-disk model and ignore effects of planetary migration. We develop a semianalytic,Expand
The interaction of giant planets with a disc with MHD turbulence – IV. Migration rates of embedded protoplanets
We present the results of global cylindrical disc simulations and local shearing box simulations of protoplanets interacting with a disc undergoing magnetohydrodynamic (MHD) turbulence. The specificExpand
ORBITAL MIGRATION AND MASS ACCRETION OF PROTOPLANETS IN THREE-DIMENSIONAL GLOBAL COMPUTATIONS WITH NESTED GRIDS
We investigate the evolution of protoplanets with different masses embedded in an accretion disk, via global fully three-dimensional hydrodynamical simulations. We consider a range of planetaryExpand
Evolution of Migrating Planets Undergoing Gas Accretion
We analyze the orbital and mass evolution of planets that undergo runaway gas accretion by means of two- and three-dimensional hydrodynamic simulations. The disk torque distribution per unit diskExpand
Three-dimensional calculations of high- and low-mass planets embedded in protoplanetary discs
We analyse the non-linear, three-dimensional response of a gaseous, viscous protoplanetary disc to the presence of a planet of mass ranging from 1 Earth mass (1 M⊕) to 1 Jupiter mass (1 MJ) by usingExpand
Models of accreting gas giant protoplanets in protostellar disks
We present evolutionary models of gas giant planets forming in protoplanetary disks. We first consider protoplanet models that consist of solid cores surrounded by hydrostatically supported gaseousExpand
Formation of Giant Planets
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 toExpand
Calculations of the accretion and evolution of giant planets: The effects of solid cores
The evolution of the giant planets is calculated under the general hypothesis that the solid cores formed first, by accretion of small particles, and that these cores later gravitationally attractedExpand
...
1
2
3
4
5
...