Gas accretion onto Jupiter mass planets in discs with laminar accretion flows

Abstract

(Abridged) Studies have shown that a Jovian mass planet embedded in a viscous protoplanetary disc (PPD) can accrete gas efficiently through the gap and doubles its mass in $\sim 0.1$ Myr. The planet also migrates inwards on a timescale of $\sim 0.1$ Myr. These timescales are short compared to PPD lifetimes, and raise questions about the origins of cold giant exoplanets. However, PPDs are unlikely to be globally turbulent, and instead they may launch magnetised winds such that accretion towards the star occurs in laminar accretion flows located in narrow layers near the surfaces of the disc. The aim of this study is to examine the rate at which gas accretes onto Jovian mass planets that are embedded in layered PPDs. We use 3D hydrodynamical simulations of planets embedded in PPDs, in which a constant radial mass flux towards the star of $\dot{m}=10^{-8}$ M${}_{\odot }$ yr${}^{-1}$ is sustained. We consider a classical viscous alpha model, and also models in which an external torque is applied in narrow surface layers to mimic the effects of a magnetised wind. The accreting layers are parameterised by their column densities ${\Sigma }_{\mathrm{A}}$, and we consider values in the range 0.1 to 10 g cm${}^{-2}$. The viscous model gives results in agreement with previous studies. We find the accretion rate onto the planet in the layered models crucially depends on the planet's ability to block the wind-induced mass flow. For ${\Sigma }_{\mathrm{A}}=10$ g cm${}^{-2}$, the planet torque can block the mass flow through the disc, accretion onto the planet is slow, and a mass doubling time of 10 Myr is obtained. For ${\Sigma }_{\mathrm{A}}=0.1$ g cm${}^{-2}$, accretion is fast and the mass doubling time is 0.2 Myr. Although the radial mass flow through the layered disc models is always $10^{-8}$ M${}_{\odot }$ yr${}^{-1}$, adopting different values of ${\Sigma }_{\mathrm{A}}$ leads to very different gas accretion rates onto gas giant planets.

14 pages, 11 figures, accepted for publication in Astronomy & Astrophysics

References in corpus (13)

• A comparative study of disc-planet interaction
• Global simulations of protoplanetary disks with ohmic resistivity and ambipolar diffusion
• Planetesimal formation starts at the snow line
• On the formation of planetary systems via oligarchic growth in thermally evolving viscous discs
• Migration of massive planets in accreting disks
• Global MHD simulations of stratified and turbulent protoplanetary discs. I. Model properties
• Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line
• Radiation Hydrodynamical Turbulence In Protoplanetary Disks: Numerical Models and Observational Constraints
• Steady State by Recycling prevents Premature Collapse of Protoplanetary Atmospheres
• Migration of Jupiter mass planets in low viscosity discs
• Recycling of the first atmospheres of embedded planets: Dependence on core mass and optical depth
• Migration of Jupiter mass planets in discs with laminar accretion flows
• Protoplanetary disk formation from the collapse of a prestellar core

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