Halting type I planet migration in non-isothermal disks

By S. Paardekooper, G. Mellema. 2006

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Aims. We investigate the effect of including a proper energy balance on the interaction of a low-mass planet with a protoplanetary disk. Methods. We use a three-dimensional version of the RODEO method to perform hydrodynamical simulations including the energy equation. Radiation is included in the flux-limited diffusion approach. Results. The sign of the torque is sensitive to the ability of the disk to radiate away the energy generated in the immediate surroundings of the planet. In the case of high opacity, corresponding to the dense inner regions of protoplanetary disks, migration is directed outward , instead of the usual inward migration that was found in locally isothermal disks. For low values of the opacity we recover inward migration and show that torques originating in the coorbital region are responsible for the change in migration direction.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/20ac82d0228315b701a441448dcbca8f022228e9

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Citations in the corpus

Planet-Disk Interaction and Orbital Evolution (2012, background): “…from disk shadowing and illumination variations in the presence of a planet (Jang-Condell & Sasselov, 2005); stochastic migration induced by disk turbulence (Nelson & Papaloizou, 2004; Laughlin, Steinacker & Adams, 2004); and corotation torques in radiative disks (Paardekooper & Mellema, 2006b).”
Assisted inspirals of stellar mass black holes embedded in AGN discs: solving the ‘final au problem’ (2016, background): “However, these rates are very sensitive to the thermodynamics of the gas near the binary, and are sufficiently uncertain (e.g., Paardekooper & Mellema 2006) that it is difficult to come to a definitive conclusion.”
Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, background): “Paardekooper & Mellema (2006) and Baruteau & Masset (2008) have also shown that depending on specific local thermodynamic disk properties, the net torque can also be positive, i.e. causing outward migration.”
Pebble-isolation mass: Scaling law and implications for the formation of super-Earths and gas giants (2018, background): “Paardekooper & Mellema (2006) included diffusion into the motion of dust particles in gas discs in the presence of 30 ME planets and estimated this effect to be of the order of 1%, indicating that diffusion of dust particles does not play a role in opening a gap in dust distribution of…”
Breaking the chains: hot super-Earth systems from migration and disruption of compact resonant chains (2017, background): “Planets may either migrate inward or outward depending on the combination of different torques from the disc (Paardekooper & Mellema 2006, 2008; Baruteau & Masset 2008; Paardekooper & Papaloizou 2008; Kley, Bitsch & Klahr 2009).”
Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, result): “Based on the results of Paardekooper & Mellema (2006), Baruteau & Masset (2008), Kley & Crida (2008), Kley et al. (2009) and Paardekooper et al. (2010), we now distinguish several sub-types of type I migration which lead to different migration directions and rates.”
A torque formula for non-isothermal Type I planetary migration – II. Effects of diffusion (2010, methodology): “We take χ to be a constant throughout the disc. rodeo (ROe solver for Disc Embedded Objects, Paardekooper & Mellema (2006b)) is a finite volume method, using an approximate Riemann solver (Roe 1981) to calculate fluxes between computational cells.”
Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc (2008, background): “…remedies include: stochastic migration in a turbulent disc (Nelson & Papaloizou 2004; Nelson 2005); corotation torques operating in a region of positive gradient in disc surface density (Masset et al. 2006); corotation torques in radiatively inefficient discs (Paardekooper & Mellema 2006).”
The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores (2015, background): “his \accretional torque" should lose relative importance. But at this stage, the thermal structure of the disk becomes relevant, as it can excite an entropy-driven corotation torque on the core (Paardekooper and Mellema, 2006; Paardekooper et al., 2010, 2011; Masset and Casoli, 2009, 2010). Bit”
The structure of protoplanetary discs around evolving young stars (2014, background): “However, the migration of cores cores depends on the thermodynamics in the disc, and even outward migration of planetary cores is possible (Paardekooper & Mellema 2006; Kley & Crida 2008; Baruteau & Masset 2008; Kley et al. 2009).”
MIGRATION THEN ASSEMBLY: FORMATION OF NEPTUNE-MASS PLANETS INSIDE 1 AU (2011, background): “Furthermore, it is no longer clear that migration implies a monotonic inward motion (e.g., Paardekooper & Mellema 2006; Oishi et al. 2007; Adams & Bloch 2009).”
A torque formula for non-isothermal type I planetary migration – I. Unsaturated horseshoe drag (2009, background): “In Paardekooper & Mellema (2006a), it was shown through three-dimensional (3D), radiation-hydrodynamic simulations that for deeply embedded lowmass planets, type I migration could be qualitatively different from the isothermal case.”
On the Corotation Torque in a Radiatively Inefficient Disk (2007, background): “More recently, Paardekooper & Mellema (2006) (hereafter PM06) have performed global, high resolution 3D calculations with nested grids that include radiative transfer.”