Simulations of Gaseous Disc-Embedded Planet Interaction

Abstract

We present three-dimensional self-gravitating smoothed-particle hydrodynamics (SPH) simulations of an isothermal gaseous disc interacting with an embedded planet. Discs of varying stability are simulated with planets ranging from 10 Earth-masses to 2 Jupiter-masses. The SPH technique provides the large dynamic range needed to accurately capture the large scale behavior of the disc as well as the small scale interaction of the planet with surrounding material. Most runs used 10^5 gas particles, giving us the spatial resolution required to observe the formation of planets. We find four regions in parameter space: low-mass planets undergo Type I migration; higher-mass planets can form a gap; the gravitational instability mode of planet formation in marginally stable discs can be triggered by embedded planets; discs that are completely unstable can fragment to form many planets. The disc stability is the most important factor in determing which interaction a system will exhibit. For the stable disc cases, our migration and accretion time-scales are shorter and scale differently than previously suggested.

10 pages, 8 figures, see http://hpcc.astro.washington.edu/grads/gwl/disc_planet_interaction for high-resolution color figures and movies

References in corpus (12)

• Gasoline: An adaptable implementation of TreeSPH
• Disk Accretion Onto High-Mass Planets
• Mass Flow and Accretion through gaps in Accretion Discs
• The Migration and Growth of Protoplanets in Protostellar Discs
• Formation of giant planets by fragmentation of protoplanetary disks
• Three-dimensional Calculations of High and Low-mass Planets Embedded in Protoplanetary Discs
• Orbital Migration and Mass Accretion of Protoplanets in 3D Global Computations with Nested Grids
• Nested-grid calculations of disk-planet interaction
• Planet migration and gap formation by tidally-induced shocks
• Dynamics of Circumstellar Disks
• Early planet formation as a trigger for further planet formation
• On the Early Evolution of Forming Jovian Planets I: Initial Conditions, Systematics and Qualitative Comparisons to Theory

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