On the width and shape of gaps in protoplanetary disks

Crida, A.; Morbidelli, Alessandro; Masset, F.

doi:10.1016/j.icarus.2005.10.007

Cited by 583 publications

(771 citation statements)

References 21 publications

(58 reference statements)

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“…With increased planet growth time-scales, we find that the RWI is in fact triggered soon after the planet mass reaches the gap-opening criterion from Crida et al (2006), which is well below the final planet masses studied here. Although the vortex evolution at the trigger point is not sensitive to T growth , the planet growth time-scale strongly affects the saturated state of the vortex.…”

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

confidence: 54%

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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: O N C L U S I O N Smentioning

confidence: 54%

“…We can interpret these results by first considering the gap-opening process, which begins before the RWI is triggered. According to Crida, Morbidelli & Masset (2006), planets open gaps when 3 4…”

Section: R E S U Lt Smentioning

confidence: 99%

Slowly-growing gap-opening planets trigger weaker vortices

Hammer

Kratter

Lin

2016

Mon. Not. R. Astron. Soc.

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“…For higher mass planets, migration is again subdivided into two modes: disc-dominated type II migration, when the local disc mass is larger than the planetary mass (the migration rate is then simply given by the viscous evolution of the protoplanetary disc), and planet-dominated type II migration in the opposite case (see M09). The transition between type I and type II migration occurs when 3 4 (Crida et al 2006), where H disc is the disc scale-height at the location of the planet, and Re = a 2 M Ω ν is the macroscopic Reynolds number at the location of the planet (ν is the same as the one used for the disc evolution).…”

Section: Orbital Evolution: Disc-planet Interactionmentioning

confidence: 99%

Planet formation models: the interplay with the planetesimal disc

Fortier

Alibert

Carron

et al. 2012

A&A

123

195

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Context. According to the sequential accretion model (or core-nucleated accretion model), giant planet formation is based first on the formation of a solid core which, when massive enough, can gravitationally bind gas from the nebula to form the envelope. The most critical part of the model is the formation time of the core: to trigger the accretion of gas, the core has to grow up to several Earth masses before the gas component of the protoplanetary disc dissipates. Aims. We calculate planetary formation models including a detailed description of the dynamics of the planetesimal disc, taking into account both gas drag and excitation of forming planets. Methods. We computed the formation of planets, considering the oligarchic regime for the growth of the solid core. Embryos growing in the disc stir their neighbour planetesimals, exciting their relative velocities, which makes accretion more difficult. Here we introduce a more realistic treatment for the evolution of planetesimals' relative velocities, which directly impact on the formation timescale. For this, we computed the excitation state of planetesimals, as a result of stirring by forming planets, and gas-solid interactions. Results. We find that the formation of giant planets is favoured by the accretion of small planetesimals, as their random velocities are more easily damped by the gas drag of the nebula. Moreover, the capture radius of a protoplanet with a (tiny) envelope is also larger for small planetesimals. However, planets migrate as a result of disc-planet angular momentum exchange, with important consequences for their survival: due to the slow growth of a protoplanet in the oligarchic regime, rapid inward type I migration has important implications on intermediate-mass planets that have not yet started their runaway accretion phase of gas. Most of these planets are lost in the central star. Surviving planets have masses either below 10 M ⊕ or above several Jupiter masses. Conclusions. To form giant planets before the dissipation of the disc, small planetesimals (∼0.1 km) have to be the major contributors of the solid accretion process. However, the combination of oligarchic growth and fast inward migration leads to the absence of intermediate-mass planets. Other processes must therefore be at work to explain the population of extrasolar planets that are presently known.

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“…Our CO J=6-5 map shows that there is almost no CO J=6-5 emission located outside the outer ring; this is expected if there is a gap or a strong density decrease which implies sub-thermal excitation. Gap opening depends on several physical parameters such as the mass of the planet, the disc viscosity and aspect ratio 47 . For example, a Saturn-like body located at 250 au, in the circumbinary disc would open a gap of about 35 au assuming standard viscosity (α = 10 −2 ) and aspect ratio h(r)/r = 0.1.…”

mentioning

confidence: 99%

Possible planet formation in the young, low-mass, multiple stellar system GG Tau A

Dutrey

Folco

Guilloteau

et al. 2014

Nature

105

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Forming planets around binary stars may be more difficult than around single stars [1][2][3] . In a close binary star (< 100 au separation), theory predicts the presence of circumstellar discs around each star, and an outer circumbinary disc surrounding a gravitationally cleared inner cavity 4,5 . As the inner discs are depleted by accretion onto the stars on timescales of few 10 3 yr, replenishing material must be transferred from the outer reservoir in order to fuel 1 planet formation (which occurs on timescales of ∼1 Myr). Gas flowing through disc cavities has been detected in single star systems 6 . A circumbinary disc was discovered around the young low-mass binary system GGTau-A 7 , which has recently been proven to be a hierarchical triple system 8 . It has one large inner disc 9 around the southern single star and shows small amounts of shocked H 2 gas residing within the central cavity 10 , but other than a weak detection 11 , hitherto the distribution of cold gas in this cavity or in any other binary or multiple star system has never been determined. Here we report imaging of massive CO-emitting gas fragments within the GG Tau-A cavity. From the kinematics we conclude that the flow appears capable of sustaining the inner disc beyond the accretion lifetime, leaving time for planet formation to occur.The 1-5 Million year old 12, 13 triple stellar system GGTau-A is located at 140 pc in a hole of the Taurus molecular cloud. Its molecular emission is free of contamination 14 and there is no known outflow neither jet associated to the source. The main binary GGTau-A (Aa-Ab) and the close-binary GGTau-Ab (Ab1-Ab2) have an apparent separation of 35 au and 4.5 au, respectively 8 .The outer circumbinary Keplerian disc of gas and dust surrounding GGTau-A consists of a ring extending from radius r ∼ 190 to 280 au and an outer disc extending up to 800 au from the central stars with a total mass ∼ 0.15 M ⊙ 14 .Using the Atacama Large Millimetre Array (ALMA), we observed GGTau-A in the dust thermal emission at 0.45 mm and in CO J=6-5 line ( Fig.1: panels a,b,c) with an angular resolution θ ≃ 0.25 ′′ or ∼35 au. The continuum image shows cold dust emission from only one circumstellar 2 disc-like structure associated with GGTau-Aa 9, 15 . We estimate the minimum dust disc size to be ∼ 7 au while the minimum mass of gas and dust is roughly 10 −3 M ⊙ about Jupiter's mass. The complex CO J=6-5 spectral line shape at the location of GGTau-Aa also reveals the existence of a CO circumstellar disc of outer radius ∼ 20 au (Methods and Extended Data: Fig.2). We do not detect cold dust emission around GGTau-Ab even though the existence of inner dust disc(s) was reported from unresolved Infrared emission 16 . Our 0.45 mm upper limits (Methods) are compatible with tidal truncation which prevents any circumstellar disc to extend beyond about 2 au 8 .The ALMA CO J=6-5 image ( Fig.1 panels a,b,c and Extended Data: Fig.1 and Fig.2) also clearly resolves CO gas within the central cavity with a structure indicative of the streamer-like f...

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On the width and shape of gaps in protoplanetary disks

Cited by 583 publications

References 21 publications

Slowly-growing gap-opening planets trigger weaker vortices

Slowly-growing gap-opening planets trigger weaker vortices

Planet formation models: the interplay with the planetesimal disc

Possible planet formation in the young, low-mass, multiple stellar system GG Tau A

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