Vortex Formation and Evolution in Planet Harboring Disks Under Thermal Relaxation

Gomes, Aiara Lobo; Klahr, Hubert; Uribe, Ana; Pinilla, P.; Surville, Clément

doi:10.1088/0004-637x/810/2/94

Cited by 27 publications

(29 citation statements)

References 68 publications

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“…This only occurs for weak vortices, which can fade quickly before the growth phase ends and do not smooth out the nearby gap edge as much as stronger vortices formed by quickly accreting planets. Note that secondary vortices have also been observed by Lobo Gomes et al (2015) for discs with a nonisothermal equation of state, albeit at a different location further from the planet.…”

Section: Vortex Reformationmentioning

confidence: 58%

“…Les & Lin 2015;Lobo Gomes et al 2015;Bae et al 2016). None the less, computational planet-disc interaction studies are notoriously susceptible to resolution artefacts (e.g.…”

Section: Convergence Testsmentioning

confidence: 99%

“…If the asymmetric discs observed with ALMA are induced by vortices from giant planets, more detailed thermodynamics may need to be incorporated into future simulations to model them properly. Accounting for the disc cooling time-scale or planetary accretion luminosity may lead to stronger vortices even with slow growth rates (Les & Lin 2015;Lobo Gomes et al 2015;Owen & Kollmeier 2016).…”

Section: O N C L U S I O N Smentioning

confidence: 99%

“…Previous simulations of planet-induced vortices have neglected realistic growth time-scales for the planet, only allowing it to reach its full mass in less than 100 orbits (e.g. de Val-Borro et al 2007;Fu et al 2014a;Lobo Gomes et al 2015;Bae et al 2016). In this regime, the vortex does not form until after the planet has attained its final mass.…”

Section: Introductionmentioning

confidence: 99%

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Slowly-growing gap-opening planets trigger weaker vortices

Hammer

Kratter

Lin

2016

Mon. Not. R. Astron. Soc.

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The presence of a giant planet in a low-viscosity disc can create a gap edge in the disc's radial density profile sharp enough to excite the Rossby wave instability. This instability may evolve into dust-trapping vortices that might explain the 'banana-shaped' features in recently observed asymmetric transition discs with inner cavities. Previous hydrodynamical simulations of planet-induced vortices have neglected the time-scale of hundreds to thousands of orbits to grow a massive planet to Jupiter size. In this work, we study the effect of a giant planet's runaway growth time-scale on the lifetime and characteristics of the resulting vortex. For two different planet masses (1 and 5 Jupiter masses) and two different disc viscosities (α = 3 × 10 −4 and 3 × 10 −5 ), we compare the vortices induced by planets with several different growth time-scales between 10 and 4000 planet orbits. In general, we find that slowly-growing planets create significantly weaker vortices with lifetimes and surface densities reduced by more than 50 per cent. For the higher disc viscosity, the longest growth time-scales in our study inhibit vortex formation altogether. Additionally, slowly-growing planets produce vortices that are up to twice as elongated, with azimuthal extents well above 180 • in some cases. These unique, elongated vortices likely create a distinct signature in the dust observations that differentiates them from the more concentrated vortices that correspond to planets with faster growth time-scales. Lastly, we find that the low viscosities necessary for vortex formation likely prevent planets from growing quickly enough to trigger the instability in self-consistent models.

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Section: Vortex Reformationmentioning

confidence: 58%

“…Les & Lin 2015;Lobo Gomes et al 2015;Bae et al 2016). None the less, computational planet-disc interaction studies are notoriously susceptible to resolution artefacts (e.g.…”

Section: Convergence Testsmentioning

confidence: 99%

Section: O N C L U S I O N Smentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Slowly-growing gap-opening planets trigger weaker vortices

Hammer

Kratter

Lin

2016

Mon. Not. R. Astron. Soc.

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“…A simple explanation for the dark ring is the presence of a supplementary planet of moderate mass inside the ring. It has also been proposed by Lobo Gomes et al (2015) that a first vortex, formed at the edge of the central cavity, might accrete matter and cleans the orbit at a slightly larger radius. This process can then create a ring and be at the origin of a vortex of second generation.…”

Section: Possible Scenariosmentioning

confidence: 86%

The Complex Morphology of the Young Disk MWC 758: Spirals and Dust Clumps around a Large Cavity

Boehler

Ricci

Weaver

et al. 2018

ApJ

126

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We present Atacama Large Millimeter Array (ALMA) observations at an angular resolution of 0.1 -0.2 of the disk surrounding the young Herbig Ae star MWC 758. The data consist of images of the dust continuum emission recorded at 0.88 millimeter, as well as images of the 13 CO and C 18 O J = 3-2 emission lines. The dust continuum emission is characterized by a large cavity of roughly 40 au in radius which might contain a mildly inner warped disk. The outer disk features two bright emission clumps at radii of ∼ 47 and 82 au that present azimuthal extensions and form a double-ring structure. The comparison with radiative transfer models indicates that these two maxima of emission correspond to local increases in the dust surface density of about a factor 2.5 and 6.5 for the south and north clumps, respectively. The optically thick 13 CO peak emission, which traces the temperature, and the dust continuum emission, which probes the disk midplane, additionally reveal two spirals previously detected in near-IR at the disk surface. The spirals seen in the dust continuum emission present, however, a slight shift of a few au towards larger radii and one of the spirals crosses the south dust clump. Finally, we present different scenarios in order to explain the complex structure of the disk.

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Dust Evolution in Protoplanetary Disks

Andrews¹,

Birnstiel²

2018

Handbook of Exoplanets

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Over the past decade, advancement of observational capabilities, specifically the Atacama Large Millimeter/submillimeter Array (ALMA) and SPHERE instrument, alongside theoretical innovations like pebble accretion, have reshaped our understanding of planet formation and the physics of protoplanetary disks. Despite this progress, mysteries persist along the winded path of micrometer-sized dust, from the interstellar medium, through transport and growth in the protoplanetary disk, to becoming gravitationally bound bodies. This review outlines our current knowledge of dust evolution in circumstellar disks, yielding the following insights:• Theoretical and laboratory studies have accurately predicted the growth of dust particles to sizes that are susceptible to accumulation through transport processes like radial drift and settling. • Critical uncertainties in that process remain the level of turbulence, the threshold collision velocities at which dust growth stalls, and the evolution of dust porosity. • Symmetric and asymmetric substructure are widespread. Dust traps appear to be solving several long-standing issues in planet formation models, and they are observationally consistent with being sites of active planetesimal formation. • In some instances, planets have been identified as the causes behind substructures. This underlines the need to study earlier stages of disks to understand how planets can form so rapidly.In the future, better probes of the physical conditions in optically thick regions, including densities, turbulence strength, kinematics, and particle properties will be essential for unraveling the physical processes at play.

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Vortex Formation and Evolution in Planet Harboring Disks Under Thermal Relaxation

Cited by 27 publications

References 68 publications

Slowly-growing gap-opening planets trigger weaker vortices

Slowly-growing gap-opening planets trigger weaker vortices

The Complex Morphology of the Young Disk MWC 758: Spirals and Dust Clumps around a Large Cavity

Dust Evolution in Protoplanetary Disks

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