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Planet-Disk Interactions
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Planet-Disk Interactions
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Planet-disk interactions, where an embedded massive body interacts gravitationally with the protoplanetary disk it was formed in, can play an important role in reshaping both the disk and the orbit of the planet. Spiral density waves are launched into the disk by the planet, which, if they are strong enough, can lead to the formation of a gap. Both effects are observable with current instruments. The back-reaction of perturbations induced in the disk, both wave-like and non-wavelike, is a change in orbital elements of the planet. The efficiency of orbital migration is a long-standing problem in planet formation theory. We discuss recent progress in planet-disk interactions for different planet masses and disk parameters, in particular the level of turbulence, and progress in modeling observational signatures of embedded planets.
Forward citations
Cited by 12 Pith papers
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The Distinctive Evolution and Spectral Energy Distribution of Binary Massive Black Hole Accretion
Combining three accretion disk states for binary massive black holes, the paper predicts a spectrum 'notch' and a mass-ratio evolution attractor at q~1e-3 for extreme-mass-ratio binaries.
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Dynamically Selected Mass-Radius Relationship for Low Mass Exoplanets
Planets inferred to have suffered giant collisions are more massive than pristine ones but retain comparable hydrogen envelope fractions, implying collisions occurred before disk gas dispersal.
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A Framework to Model Stellar Irradiated Disks with Frequency-dependent Absorption and Scattering Opacities in Athena++
A new implementation of radial rays and multigroup radiation transport in Athena++ for frequency-dependent stellar irradiation achieves 2-5% average temperature agreement with Monte Carlo benchmarks in hydrostatic dis...
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Orbital evolution of highly eccentric bodies embedded in a ringed accretion disc
Prograde highly eccentric perturbers in a ringed isothermal disc circularize and accumulate at the ring, forming a migration trap, while retrograde perturbers migrate inward without re-intersecting.
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Dust Growth in Binary Systems: Inhibition of dust settling and growth in circumbinary discs
Dust grains in circumbinary discs end up five times smaller than in single-star discs, and the conditions for streaming-instability clumping are not met, arguing against in-situ planet formation there.
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Resonant Super-Earths Dancing With EKL Oscillations: TTV Phase Excitation and Resonance Disruption by EKL Interactions between a Cold Jupiter and Stellar Companion
Simulations indicate EKL interactions excite TTV phases and disrupt resonances in a significant fraction of near-resonant super-Earth systems over 16 Myr.
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Planet formation at the inner edge of the dead zone II. Outbursts, rings, vortices, and suppression of planetesimal formation
2D radiation-hydrodynamical simulations find accretion outbursts unstable to Rossby-wave instability, forming vortices that suppress planetesimal formation until post-burst quiescence.
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$\alpha\beta q_\mathrm{th}$-mapping of planet-induced density wave damping in protoplanetary discs
Nonlinear shock formation dominates angular momentum deposition from planet-induced density waves, cooling matches it for sub-thermal planets, and viscosity only matters at unrealistically high values.
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A low viscosity relatively thick twisted disk in a supermassive binary black hole as a potential model of OJ 287
A relatively thick low-viscosity twisted disk can explain the two orbit crossings per period observed in OJ 287 if secondary-disk collisions provide extra heating.
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A JWST, ALMA and VLA survey of the Ophiuchus-A star-forming region: Unveiling hidden dust mass and connecting infrared outflows to their radio origins
A multi-wavelength survey of 20 Ophiuchus protostars finds dust masses tens to hundreds of times larger than millimetre-only estimates, if the adopted dust-opacity model is correct.
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On the Dust Substructures Triggered by Two Super-Earths Migrating in Low-viscosity Disks
Two migrating super-Earths in low-viscosity disks trigger narrow and broad dust substructures with high dust-to-gas ratios favorable for planetesimal formation.
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The Intrinsic Multiplicity Distribution of Exoplanets Revealed from the Radial Velocity Method. II. Constraints on Giant Planet Multiplicity from Different Surveys
Giant planet multiplicity is low, with 10.6% and 15.8% of Sun-like stars hosting at least one giant planet within 10 au across the two surveys, mostly as singles, inconsistent with scattering models.
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