3D simulations of planet trapping at disc–cavity boundaries

Romanova, M. M.; Lii, Patrick; Koldoba, A. V.; Ustyugova, G. V.; Blinova, A. A.; Lovelace, R. V. E.; Kaltenegger, Lisa

doi:10.1093/mnras/stz535

Cited by 34 publications

(31 citation statements)

References 84 publications

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“…The radius at which this occurs is often called a planet trap, since the torque balance will cause a planet to halt migration and become trapped at a fixed orbital radius. This behavior has been found in several other numerical studies (e.g., Morbidelli et al 2008;Baillié et al 2016;Romanova et al 2019). Since the planets we consider in this work reside at (or near) the inner disk edge, slightly external to the interior cavity, Type I torques are expected to act outward, and under standard assumptions, C I ≈ −0.6 (Ward 1997;Tanaka et al 2002).…”

Section: Type I Torquessupporting

confidence: 78%

Migrating Planets into Ultra-short-period Orbits during Episodic Accretion Events

Becker

Batygin

Adams

2021

ApJ

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Ultra-short-period (USP) planets reside inside the expected truncation radius for typical T Tauri disks. As a result, their current orbital locations require an explanation beyond standard disk migration or in situ formation. Modern theories of planet-disk interactions indicate that once a planet migrates close to the disk's inner truncation radius, Type I torques vanish or switch direction, depending on the stellar and disk conditions, so that the planet is expected to stop its orbital decay and become trapped. In this work, we show that that magnetically driven sub-Keplerian gas flow in the inner disk can naturally counteract these effects and produce systems with USP planets at their observed orbital radii. The sub-Keplerian gas flow provides a headwind to small planets, and the resulting torque can overcome the effects of outward Type I migration near the corotation radius. For suitable disk and planet parameters, the torques due to the sub-Keplerian gas flow lead to inward migration on a rapid timescale. Over the time span of an FU Ori outburst, which moves the disk truncation radius inward, the rapid headwind migration can place planets in USP orbits. The combination of headwind migration and FU Ori outbursts thus provides a plausible mechanism to move small planets from a = 0.05-0.1 au down to a = 0.01-0.02 au. This effect is amplified for low-mass planets, consistent with existing observations.

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Section: Type I Torquessupporting

confidence: 78%

Migrating Planets into Ultra-short-period Orbits during Episodic Accretion Events

Becker

Batygin

Adams

2021

ApJ

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“…Migrating cores tend to form configurations in which each pair of neighboring planets is in mean motion resonance (e.g., Cresswell & Nelson, 2008;Terquem & Papaloizou, 2007). In these "resonant chains," the innermost planet is anchored at the inner edge of the gaseous disk, which provides a positive torque to balance the negative ones felt by the other planets (Masset et al, 2006;Romanova et al, 2019). Resonant chains often become dynamically unstable after the gaseous disk dissipates, leading to phase of late giant impacts (Cossou et al, 2014;Ogihara & Ida, 2009;Terquem & Papaloizou, 2007).…”

Section: Silicate Water Ironmentioning

confidence: 99%

The Nature and Origins of Sub‐Neptune Size Planets

2021

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Planets intermediate in size between the Earth and Neptune, and orbiting closer to their host stars than Mercury does the Sun, are the most common type of planet revealed by exoplanet surveys over the last quarter century. Results from NASA's Kepler mission have revealed a bimodality in the radius distribution of these objects, with a relative underabundance of planets between 1.5 and 2.0 R⊕. This bimodality suggests that sub‐Neptunes are mostly rocky planets that were born with primary atmospheres a few percent by mass accreted from the protoplanetary nebula. Planets above the radius gap were able to retain their atmospheres (“gas‐rich super‐Earths”), while planets below the radius gap lost their atmospheres and are stripped cores (“true super‐Earths”). The mechanism that drives atmospheric loss for these planets remains an outstanding question, with photoevaporation and core‐powered mass loss being the prime candidates. As with the mass‐loss mechanism, there are two contenders for the origins of the solids in sub‐Neptune planets: the migration model involves the growth and migration of embryos from beyond the ice line, while the drift model involves inward‐drifting pebbles that coagulate to form planets close‐in. Atmospheric studies have the potential to break degeneracies in interior structure models and place additional constraints on the origins of these planets. However, most atmospheric characterization efforts have been confounded by aerosols. Observations with upcoming facilities are expected to finally reveal the atmospheric compositions of these worlds, which are arguably the first fundamentally new type of planetary object identified from the study of exoplanets.

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“…where f " exp r´pr p´rin q{x hs s is a smooth fitting function, r p is the planet disk location, and f "1 (f "0) refers to the planet at the disk edge (far away from the disk edge). Although the above equations are derived analytically, we note that the termination of planet migration at the inner disk edge due to one-sided torque induced from a steep density transition is also obtained from hydrodynamic simulations 25,26 .…”

Section: Methodsmentioning

confidence: 99%

“…In contrast, planets at the disk's inner edge only interact with gas on the outside of their orbits. As a result of larger-amplitude Lindblad and corotation torques, a planet below the mass threshold for opening a gap stops migrating inward at the disk inner edge 25,26 . If the disk inner edge is itself moving radially outward due to disk dispersal, then the planet may subsequently migrate outward along with the expanding inner edge (see Supplementary Information).…”

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confidence: 99%

An early dynamical instability among the Solar System’s giant planets triggered by the gas disk’s dispersal

Liu

Raymond

Jacobson

2020

Preprint

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The Solar System’s orbital structure is thought to have been sculpted by a dynamical instability among the giant planets[1–4]. Yet the instability trigger and exact timing have proved hard to pin down[5–9]. The giant planets formed within a gas-dominated disk around the young Sun. Motivated by giant exoplanet systems found in mean motion resonance[10], hydrodynamical modeling has shown that while the disk was present the giant planets migrated into a compact orbital configuration, in a chain of resonances[2,11]. Here we use a suite of dynamical simulations to show that the giant planets’ instability was likely triggered by the dispersal of the Sun’s gaseous disk. As the disk evaporated from the inside-out, its inner edge swept successively across and dynamically perturbed each planet’s orbit in turn. Saturn and each ice giants’ orbits were torqued strongly enough to migrate outward. As a given planet migrated outward with the disk’s inner edge the orbital configuration of the exterior system was compressed, triggering dynamical instability. The final orbits of our simulated systems match those of the Solar System for a viable range of astrophysical parameters. Our results demonstrate that the giant planet instability happened as the gaseous disk dissipated, constrained by astronomical observations to be a few to ten million years after the birth of the Solar System [12]. Late-stage terrestrial planet formation would occur mostly after such an early giant planet instability [13,14], thereby avoiding the possibility of de-stabilizing the terrestrial planets [15] and naturally accounting for the small mass of Mars relative to Earth and the mass depletion of the main asteroid belt [16].

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3D simulations of planet trapping at disc–cavity boundaries

Cited by 34 publications

References 84 publications

Migrating Planets into Ultra-short-period Orbits during Episodic Accretion Events

Migrating Planets into Ultra-short-period Orbits during Episodic Accretion Events

The Nature and Origins of Sub‐Neptune Size Planets

An early dynamical instability among the Solar System’s giant planets triggered by the gas disk’s dispersal

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