Survival of planet-induced vortices in 2D disks

Rometsch, Thomas; Ziampras, Alexandros; Kley, W.; Béthune, William

doi:10.1051/0004-6361/202142105

Cited by 20 publications

(19 citation statements)

References 62 publications

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“…As time progresses, the number of vortices changes and becomes more compact. This general behavior is unlike previous results with a single planet where vortices tend to get more elongated and finally decay away (Hammer et al 2021;Rometsch et al 2021).…”

Section: Morphology Of Vorticescontrasting

confidence: 99%

“…Radiative damping can play an important role in the wave dissipation (Miranda & Rafikov 2020), and for cooling time in the range t cool Ω K ä [0.1, 1], the planetary spiral waves become weaker and the AMF dissipates faster compared to the spirals in an isothermal disk (Zhang & Zhu 2020). Accordingly, the vortices' lifetime may be affected by considering a finite cooling time as shown by Rometsch et al (2021), where the shortest lifetimes occur for t cool Ω K ∼ 1 (Fung & Ono 2021). A similar effect may be expected in our simulations, but it is possibly less important, as the vortices' lifetimes in simulations with multiple planets depend on more factors than just the wave damping by shocks.…”

Section: Viscosity and Thermodynamic Effectsmentioning

confidence: 99%

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Substructures in Protoplanetary Disks Imprinted by Compact Planetary Systems

Garrido-Deutelmoser

Petrovich

Krapp

et al. 2022

ApJ

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The substructures observed in protoplanetary disks may be the signposts of embedded planets carving gaps or creating vortices. The inferred masses of these planets often fall in the Jovian regime despite their low abundance compared to lower-mass planets, partly because previous works often assume that a single substructure (a gap or vortex) is caused by a single planet. In this work, we study the possible imprints of compact systems composed of Neptune-like planets (∼10–30 M ⊕) and show that long-standing vortices are a prevalent outcome when their interplanetary separation (Δa) falls below ∼8 times H p—the average disk’s scale height at the planet’s locations. In simulations where a single planet is unable to produce long-lived vortices, two-planet systems can preserve them for at least 5000 orbits in two regimes: (i) fully shared density gaps with elongated vortices around the stable Lagrange points L 4 and L 5 for the most compact planet pairs (Δa ≲ 4.6 H p), and (ii) partially shared gaps for more widely spaced planets (Δa ∼ 4.6–8 H p) forming vortices in a density ring between the planets through the Rossby wave instability. The latter case can produce vortices with a wide range of aspect ratios down to ∼3 and can occur for planets captured into the 3:2 (2:1) mean-motion resonances for disks’ aspects ratios of h ≳ 0.033 (h ≳ 0.057). We suggest that their long lifetimes are sustained by the interaction of spiral density waves launched by the neighboring planets. Overall, our results show that the distinguishing imprint of compact systems with Neptune-mass planets are long-lived vortices inside the density gaps, which in turn are shallower than single-planet gaps for a fixed gap width.

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Section: Morphology Of Vorticescontrasting

confidence: 99%

Section: Viscosity and Thermodynamic Effectsmentioning

confidence: 99%

Substructures in Protoplanetary Disks Imprinted by Compact Planetary Systems

Garrido-Deutelmoser

Petrovich

Krapp

et al. 2022

ApJ

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show abstract

Section: Morphology Of Vorticescontrasting

confidence: 99%

“…Radiative damping can play an important role in the wave dissipation (Miranda & Rafikov 2020) and for cooling time in the range t cool Ω K ∈ [0.1, 1], the planetary spiral waves become weaker and the AMF dissipates faster compared to the the spirals in an isothermal disk (Zhang & Zhu 2020). Accordingly, the vortices' lifetime may be affected by considering a finite cooling time as shown by Rometsch et al (2021), where the shortest lifetimes occur for t cool Ω K ∼ 1 (Fung & Ono 2021). A similar effect may be expected in our simulations, but possibly less important as the vortices' lifetimes in simulations with multiple planets depend on more factors than just the wave damping by shocks.…”

Section: Viscosity and Thermodynamic Effectsmentioning

confidence: 99%

Substructures in protoplanetary disks imprinted by compact planetary systems

Garrido-Deutelmoser,

Petrovich,

Krapp

et al. 2022

Preprint

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The substructures observed in protoplanetary disks may be the signposts of embedded planets carving gaps or creating vortices. The inferred masses of these planets often fall in the Jovian regime despite their low abundance compared to lower-mass planets, partly because previous works often assume that a single substructure (a gap or vortex) is caused by a single planet. In this work, we study the possible imprints of compact systems composed of Neptune-like planets (∼ 10 − 30 M ⊕ ) and show that longstanding vortices are a prevalent outcome when their inter-planetary separation (∆a) falls below ∼ 8 times H p -the average disk's scale height at the planets locations. In simulations where a single planet is unable to produce long-lived vortices, two-planet systems can preserve them for at least 5, 000 orbits in two regimes: i) fully-shared density gaps with elongated vortices around the stable Lagrange points L 4 and L 5 for the most compact planet pairs (∆a 4.6 H p ); ii) partially-shared gaps for more widely spaced planets (∆a ∼ 4.6 − 8 H p ) forming vortices in a density ring between the planets through the Rossby wave instability. The latter case can produce vortices with a wide range of aspect ratios down to ∼ 3 and can occur for planets captured into the 3:2 (2:1) mean-motion resonances for disk's aspects ratios of h 0.033 (h 0.057). We suggest that their long lifetimes are sustained by the interaction of spiral density waves launched by the neighboring planets. Overall, our results show that distinguishing imprint of compact systems with Neptune-mass planets are long-lived vortices inside the density gaps, which in turn are shallower than single-planet gaps for a fixed gap width.

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“…We use a β-cooling prescription similar to Gammie (2001), and follow the implementation detailed in Rometsch et al (2021).…”

Section: Parametrised β-Coolingmentioning

confidence: 99%

How cooling influences circumbinary discs

Sudarshan

Penzlin

Ziampras

et al. 2022

A&A

Self Cite

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Circumbinary disc observations and simulations show large, eccentric inner cavities. Recent work has shown that the shape and size of these cavities depend on the aspect ratio and viscosity of the disc, as well as the binary eccentricity and mass ratio. It has been further shown that, for gaps created by planets, the cooling timescale significantly affects the shape and size of the gap. In this study, we consider the effect of different cooling models on the cavity shape in a circumbinary disc. We compare locally isothermal and radiatively cooled disc models to ones with a parametrised cooling timescale (β-cooling), implemented in 2D numerical simulations for varying binary eccentricities. While the shape of the cavity for radiative and locally isothermal models remains comparable, the inner disc structure changes slightly, leading to a change in the precession rate of the disc. With β-cooled models, the shape and size of the cavity changes dramatically towards values of β = 1. Based on our findings, we introduce a parametrised β model that accounts for the shorter cooling timescale inside the cavity while adequately reproducing the results of the radiative model, and we highlight that accurate treatment of the thermodynamics inside the cavity has a significant impact in modelling circumbinary systems.

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Survival of planet-induced vortices in 2D disks

Cited by 20 publications

References 62 publications

Substructures in Protoplanetary Disks Imprinted by Compact Planetary Systems

Substructures in Protoplanetary Disks Imprinted by Compact Planetary Systems

Substructures in protoplanetary disks imprinted by compact planetary systems

How cooling influences circumbinary discs

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