Disk Surface Density Transitions as Protoplanet Traps

By F. Masset, A. Morbidelli, A. Crida, J. Ferreira. 2006

282 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/805e799d40982540dcbf7b0f57eff0f56891071c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Morbidelli
2. Anders Johansen
3. S. Raymond
4. Michiel Lambrechts
5. W. Kley
6. R. Nelson
7. B. Bitsch
8. A. Izidoro

In Spectroscopy

1. D. Lin
2. W. Kley
3. Shigeru Ida
4. R. Nelson
5. C. Baruteau
6. S. Paardekooper
7. Brad M. S. Hansen
8. G. D’Angelo

Citations in the corpus

• Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, background): “In such regions where the viscosity or the opacity sharply changes, the migration of the giant planet cores can come to a complete halt (Masset et al. 2006; Lyra et al. 2010; Kretke & Lin 2012; Bitsch et al. 2013; Pierens et al. 2013).”
• TESTING IN SITU ASSEMBLY WITH THE KEPLER PLANET CANDIDATE SAMPLE (2013, background): “One possibility, suggested by several authors (e.g., Masset et al. 2006), is that the torque may reverse sign at particular locations in the disk, leading to “planet traps”—preferred locations where planets assemble.”
• Breaking the chains: hot super-Earth systems from migration and disruption of compact resonant chains (2017, background): “When the first embryo reaches the inner edge of the disc, its migration is stopped by the planet disc–edge interaction (Masset et al. 2006) and other embryos migrate into a resonant chain with up to 10 or more closein planets (Figs 4–6).”
• Planet-Disk Interaction and Orbital Evolution (2012, background): “…migration include: strong corotation torques operating in regions where there are steep positive surface density gradients (socalled ‘planet traps’) (Masset et al., 2006); reductions in the differential Lindblad torque in regions of sharp opacity transition (Menou & Goodman, 2004); magnetic…”
• Fossilized condensation lines in the Solar System protoplanetary disk (2015, background): “obably due to the existence of an inner edge of the protoplanetary disk where the Keplerian period is equal to the star’s rotation period (Koenigl, 1991; Lin et al., 1996), acting like a planet-trap (Masset et al., 2006). The presence of planet-trap would change completely the picture presented in I”
• Migration and the Formation of Systems of Hot Super-Earths and Neptunes (2006, background): “Recently, Masset et al. (2006) have proposed that inward protoplanet migration can be halted near sharp disk inner edges which act as traps.”
• A torque formula for non-isothermal Type I planetary migration – II. Effects of diffusion (2010, background): “The entropy-related horseshoe drag seems to play an important role in three-dimensional discs as well (Kley et al. 2009), and it has been shown that, in an isothermal set-up, the effect of the horseshoe drag is stronger in three dimensions (Masset et al. 2006).”
• Toward a Deterministic Model of Planetary Formation. IV. Effects of Type I Migration (2008, background): “…variation in the surface density and temperature gradient (Masset et al. 2006b), intrinsic turbulence in the disk (Laughlin et al. 2004; Nelson & Papaloizou 2004), self-induced unstable flow (Koller & Li 2004; Li et al. 2005), and nonlinear radiative and hydrodynamic feedback (Masset et al. 2006a).”
• Halting type I planet migration in non-isothermal disks (2006, background): “For deeply embedded objects, material could be bound in the smaller Bondi sphere (Masset et al. 2006b), so that we may exclude a region that is too large.”
• Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc (2008, background): “…type I migration, such as a disc edge caused by a magnetospheric cavity (Terquem & Papaloizou 2007) or a “planet trap” produced by a region of positive density gradient in the disc (Masset et al. 2006; Morbidelli et al. 2008), on a resonant group that has already formed and migrated some distance.”
• On the Migration of Protogiant Solid Cores (2006, background): “This yields: νm = 0.035 ( q h )3/2 a2Ωp, (16) where νm is the minimal viscosity to avoid the coorbital torque saturation (Masset et al. 2006).”
• The dynamics of Jupiter and Saturn in the gaseous protoplanetary disk (2007, background): “Moreover, Saturn’s core, independently of its formation location, might have suffered Type I migration until it was halted at the edge of Jupiter’s gap, which acts as a planet trap (Masset et al., 2006), or in a mean motion resonance with Jupiter (Thommes, 2005).”
• FORMATION OF THE TERRESTRIAL PLANETS FROM A NARROW ANNULUS (2009, background): “It has been suggested (e.g., Masset et al. 2006) that local changes in the density profile, either due to changes in the disk structure or true evacuation of inner gaseous holes, can reduce or reverse the effects of this migration, which would also lead to a pile-up of solid material.”