Planet-Disk Interaction and Orbital Evolution

By W. Kley, R. Nelson. 2012

533 citations recorded by the source corpus.

As planets form and grow within gaseous protoplanetary disks, the mutual gravitational interaction between the disk and planet leads to the exchange of angular momentum and migration of the planet. We review current understanding of disk-planet interactions, focusing in particular on physical processes that determine the speed and direction of migration. We describe the evolution of low-mass planets embedded in protoplanetary disks and examine the influence of Lindblad and corotation torques as a function of the disk properties. The role of the disk in causing the evolution of eccentricities and inclinations is also discussed. We describe the rapid migration of intermediate-mass planets that may occur as a runaway process and examine the transition to gap formation and slower migration driven by the viscous evolution of the disk for massive planets. The roles and influence of disk self-gravity and magnetohydrodynamic turbulence are discussed in detail, as a function of the planet mass, as is the evolution...

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/512af261a056b0e63fe01dc98522d458808fa79a

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Citations in the corpus

OBSERVATIONAL SIGNATURES OF PLANETS IN PROTOPLANETARY DISKS: SPIRAL ARMS OBSERVED IN SCATTERED LIGHT IMAGING CAN BE INDUCED BY PLANETS (2015, background): “In protoplanetary disks, planets can excite spiral density waves through gravitational disk–planet interactions (Kley & Nelson 2012).”
Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations (2015, background): “…form at http://www.aanda.org The evolution of protoplanetary disks and planets are closely connected as the disk properties define the initial conditions of planet formation, and the planet evolution subsequently affects the disk properties (e.g. Kley & Nelson 2012; Baruteau et al. 2014).”
Gas density drops inside dust cavities of transitional disks around young stars observed with ALMA (2015, background): “Other effects that play a role in dynamic clearing are for example migration and planet accretion luminosity (e.g. Kley & Nelson 2012).”
HOW EMPTY ARE DISK GAPS OPENED BY GIANT PLANETS (2013, background): “…50 St. George Street, Toronto, Ontario, Canada M5S 3H4 2 Department of Astronomy, UC Berkeley, Hearst Field Annex B-20, Berkeley, CA 94720-3411 3 Department of Earth and Planetary Science, UC Berkeley, 307McCone Hall, Berkeley, CA 94720-4767 jor axes (for a review, see Kley and Nelson 2012).”
MIGRATION THEN ASSEMBLY: FORMATION OF NEPTUNE-MASS PLANETS INSIDE 1 AU (2011, background): “Although the notion of gaseous disk migration has a long, physically motivated provenience (e.g., Goldreich & Tremaine 1980; Ward 1997), the nature of the migration and when it occurs is still a subject of significant uncertainty (see Kley & Nelson 2012 for a recent review).”
CHARACTERIZING THE COOL KOIs. IV. KEPLER-32 AS A PROTOTYPE FOR THE FORMATION OF COMPACT PLANETARY SYSTEMS THROUGHOUT THE GALAXY (2012, methodology): “Interactions with either a gaseous disk or a disk of planetesimals can cause radial migration of planetary orbits (see Kley & Nelson 2012, for a review).”
A LIKELY CLOSE-IN LOW-MASS STELLAR COMPANION TO THE TRANSITIONAL DISK STAR HD 142527 (2012, background): “A binary + planet system can open a much larger gap than can be formed by the binary by itself (Nelson 2003; Kley et al. 2008; Kley & Nelson 2008, 2012).”
The GAPS Programme with HARPS-N at TNG - XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets (2017, unknown): “The former would yield mainly circular orbits and spin-orbit alignments because of damping by the disc (e.g. Goldreich & Tremaine 1980; Papaloizou & Larwood 2000; Kley & Nelson 2012).”
IN SITU FORMATION AND DYNAMICAL EVOLUTION OF HOT JUPITER SYSTEMS (2015, background): “Over the past two decades, this sequence of events has become an established theoretical paradigm, and considerable effort has been dedicated to determining the precise nature of the dominant mode of orbital transport (Wu and Murray 2003; Kley and Nelson 2012; Beaugé and Nesvorný 2012).”
Magellan Adaptive Optics Imaging of PDS 70: Measuring the Mass Accretion Rate of a Young Giant Planet within a Gapped Disk (2018, background): “While gapped (“transition” and “pre-transition”) disks around young stars are fundamental to inform planet formation and disk evolution models (e.g., D’Angelo et al. 2003, Kley & Nelson 2012, Uribe et al. 2013), so far the link to planet formation has lacked significant direct evidence.”
WEAK TURBULENCE IN THE HD 163296 PROTOPLANETARY DISK REVEALED BY ALMA CO OBSERVATIONS (2015, background): “The threshold for a massive planet to open a gap within the disk depends on the ability of the accretion flow to refill the gap; weaker turbulence, and hence a weaker accretion flow, would allow smaller planets to open large disk gaps (Crida et al. 2006; Kley & Nelson 2012; Fung et al. 2014).”
The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths (2012, background): “Theoretical uncertainties include the effects of co-rotation resonances, disk thermodynamics (which can even cause planets to migrate outward; see, e.g., section 2.2 in Kley & Nelson 2012, and references therein), and the perennial mystery of the source of viscosity in protoplanetary disks.”
RINGED SUBSTRUCTURE AND A GAP AT 1 au IN THE NEAREST PROTOPLANETARY DISK (2016, background): “The dynamical alternative instead postulates that the dark annuli are true gaps that have had their densities depleted by interactions with (as yet unseen) planetarymass companions (Lin & Papaloizou 1986; Kley & Nelson 2012).”
Water delivery and giant impacts in the 'Grand Tack' scenario (2014, unknown): “Giant planets of roughly a Jupiter mass or larger can clear a gap in the disk and migrate by a process referred to as ‘‘type-II’’ migration, in which the planet moves inwards, following the viscous evolution of the disk (Lin and Papaloizou, 1986; Kley and Nelson, 2012).”
MAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND (2014, background): “Our scenario also neglects gas disk turbulence and its associated density fluctuations, which can cause oligarchs’ semi-major axes and eccentricities to random walk (Kley & Nelson 2012, their section 3.1; Okuzumi & Ormel 2013).”
STELLAR ROTATION PERIODS OF THE KEPLER OBJECTS OF INTEREST: A DEARTH OF CLOSE-IN PLANETS AROUND FAST ROTATORS (2013, background): “The former might determine the point where the planetary migration stops (Kley & Nelson 2012), while the latter determines the stellar rotation evolution.”