Disk eccentricity and embedded planets

By W. Kley, G. Dirksen. 2005

174 citations recorded by the source corpus.

Aims. We investigate the response of an accretion disk to the presence of a perturbing protoplanet embedded in the disk through time dependent hydrodynamical simulations. Methods. The disk is treated as a two-dimensional viscous fluid and the planet is kept on a fixed orbit. We run a set of simulations varying the planet mass, and the viscosity and temperature of the disk. All runs are followed until they reach a quasi-equilibrium state. Results. We find that for planetary masses above a certain minimum mass, already 3 M Jup for a viscosity of v = 10 -5 , the disk makes a transition from a nearly circular state into an eccentric state. Increasing the planetary mass leads to a saturation of disk eccentricity with a maximum value of around 0.25. The transition to the eccentric state is driven by the excitation of an m = 2 spiral wave at the outer 1:3 Lindblad resonance. The effect occurs only if the planetary mass is large enough to clear a sufficiently wide and deep gap to reduce the damping effect of the outer 1:2 Lindblad resonance. An increase in viscosity or temperature in the disk, which both tend to close the gap, have an adverse influence on the disk eccentricity. Conclusions. In the eccentric state the mass accretion rate onto the planet is greatly enhanced, an effect that may ease the formation of massive planets beyond about 5 M Jup that are otherwise difficult to reach.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/92f09a62d866d37220de5821db098407ac38d3f4

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. Anders Johansen
2. A. Morbidelli
3. C. Mordasini
4. T. Birnstiel
5. Y. Alibert
6. D. Wilner
7. S. Andrews
8. Th. Henning

Citations in the corpus

• Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, background): “Such a situation arises if the eccentric instability (Papaloizou et al. 2001; Kley & Dirksen 2006) allows the planets to efficiently access disk material even after a gap has formed.”
• Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, background): “But the significant number of planets lying above the solid line indicates that mechanisms like the eccentric instability (Kley & Dirksen 2006) that allow growth beyond the gap barrier seem to play an important role in nature.”
• The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation (2018, result): “Such an eccentric gap edge for the Mp 3MJ planet is consistent with previous studies (Lubow 1991a, 1991b; Kley & Dirksen 2006; Teyssandier & Ogilvie 2017).”
• Toward a Deterministic Model of Planetary Formation. IV. Effects of Type I Migration (2008, background): “Some numerical simulations indicate that a residual amount of gas may continue to flow into the gap after both the viscous and thermal conditions are satisfied (D’Angelo et al. 2003; Kley & Dirksen 2006; Tanigawa & Ikoma 2007).”
• Gas Flow across Gaps in Protoplanetary Disks (2005, background): “But accretion may still occur at higher planet masses, if the disk becomes eccentric as a consequence of a tidal instability (Papaloizou et al. 2001; Kley & Dirksen 2006; D’Angelo et al. 2005).”
• An Eccentric Circumbinary Accretion Disk and the Detection of Binary Massive Black Holes (2006, background): “The simulations of disks with planets also indicate that an initially circular disk becomes eccentric over time, even if the orbit of the planet is circular (Papaloizou, Nelson, & Masset 2001; Kley & Dirksen 2006).”
• Planet-Disk Interaction and Orbital Evolution (2012, background): “For massive planets of a few MJup a new but related effect occurs in that the outer disk can become eccentric even if the planet is on a circular orbit (Papaloizou, Nelson & Masset, 2001; Kley & Dirksen, 2006).”
• The primordial excitation and clearing of the asteroid belt—Revisited (2006, background): “…1996; Lubow et al., 1999) tend to form planets on circular orbits, and it is not clear that planet–disk interactions are capable of exciting the eccentricities and inclinations of Jupiter-and Saturn-mass planets (e.g., Papaloizou et al., 2001; D'Angelo et al., 2006; Kley and Dirksen, 2006).”
• Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution (2009, result): “However, it has also been shown (see Kley & Dirksen 2006) that when the mass of the planet becomes of the order of 3 − 5 MX (MX is the mass of Jupiter ≈ 318 M⊕), the disk-planet system can undergo a dynamic instability, leading to a substantial increase of the accretion rate of gas.”
• THREE-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS OF CIRCUMBINARY ACCRETION DISKS: DISK STRUCTURES AND ANGULAR MOMENTUM TRANSPORT (2011, background): “Simulations of protoplanetary disks have shown that these disks are subject to a resonant mode coupling instability (Kley & Dirksen 2006; D’Angelo et al. 2006).”
• Ring shaped dust accumulation in transition disks (2012, background): “Kley & Dirksen (2006) showed that the disk becomes eccentric with the presence of a planet with a mass Mp > 3MJup (for a constant viscosity given by ν = 10−5), which may cause a change in the equilibrium state.”
• HOW EMPTY ARE DISK GAPS OPENED BY GIANT PLANETS (2013, background): “For a planet held on a fixed circular orbit embedded in a non-gravitating disk for which/r = 0.05 andα ≈ 0.005, Kley and Dirksen (2006) found thatq & 0.003 led to eccentric disks; forα ≈ 0.01, the requiredq & 0.005.”
• Building the terrestrial planets: Constrained accretion in the inner Solar System (2009, background): “However, other studies have shown that eccentricity growth via planet-disk interactions can only occur for very massive, > 10MJup planets (Papaloizou et al., 2001; Kley and Dirksen, 2006).”
• DIRECT IMAGING OF FINE STRUCTURES IN GIANT PLANET-FORMING REGIONS OF THE PROTOPLANETARY DISK AROUND AB AURIGAE (2011, background): “It is also noted that there is a possibility that the inner ring is intrinsically elliptical due to the influence of an unseen gravitating object, which could be another indication of the presence of a planet (Kley & Dirksen 2006).”
• Observational Signatures of Planets in Protoplanetary Disks I: Gaps Opened by Single and Multiple Young Planets in Disks (2014, background): “Also, in Model 4×2MJ, the gap is slightly eccentric, as a result of the disk-planet interaction in the high planet mass regime (Kley & Dirksen 2006; D’Angelo et al. 2006; Ataiee et al. 2013; Pinilla et al. 2014).”
• The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, background): “Hydrodynamical simulations of planet-disk interactions indicate that the eccentricity of annular substructures increases for more massive planets and for lower disk viscosities (e.g. Lubow 1991; Kley & Dirksen 2006; Zhang et al. 2018).”