Non-linear development of secular gravitational instability in protoplanetary disks

Tominaga, Ryosuke T.; Inutsuka, Shu‐ichiro; Takahashi, Sanemichi Z.

doi:10.1093/pasj/psx143

Cited by 43 publications

(30 citation statements)

References 20 publications

(22 reference statements)

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“…To name but a few, one set of proposed mechanisms is related to the condensation fronts of various volatile species, which mark a transition in dust properties (e.g., Zhang et al 2015;Okuzumi et al 2016;Hu et al 2019;Owen 2020). Another set of scenarios is associated with gas-dust coupling, including secular gravitational instability (Shariff & Cuzzi 2011;Youdin 2011;Takahashi & Inutsuka 2014;Tominaga et al 2018Tominaga et al , 2019, dust-driven viscous ring-instability (Wünsch et al 2005;Dullemond & Penzlin 2018), and self-induced dust traps (Drazkowska et al 2016;Gonzalez et al 2017).…”

Section: Annular Substructuresmentioning

confidence: 99%

Global three-dimensional simulations of outer protoplanetary discs with ambipolar diffusion

Cui

Bai

2021

Monthly Notices of the Royal Astronomical Society

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The structure and evolution of protoplanetary disks (PPDs) are largely governed by disk angular momentum transport, mediated by magnetic fields. In the most observable outer disk, ambipolar diffusion is the primary non-ideal magnetohydrodynamic(MHD) effect. In this work, we study the gas dynamics in outer PPDs by conducting a series of global 3D non-ideal MHD simulations with ambipolar diffusion and net poloidal magnetic flux, using the Athena++ MHD code, with resolution comparable to local simulations. Our simulations demonstrate the co-existence of magnetized disk winds and turbulence driven by the magneto-rotational instability (MRI). While MHD winds dominate disk angular momentum transport, the MRI turbulence also contributes significantly. We observe that magnetic flux spontaneously concentrate into axisymmetric flux sheets, leading to radial variations in turbulence levels, stresses, and accretion rates. Annular substructures arise as a natural consequence of magnetic flux concentration. The flux concentration phenomena show diverse properties with different levels of disk magnetization and ambipolar diffusion. The disk generally loses magnetic flux over time, though flux sheets could prevent the leak of magnetic flux in some cases. Our results demonstrate the ubiquity of disk annular substructures in weakly MRI turbulent outer PPDs, and imply a stochastic nature of disk evolution.

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Section: Annular Substructuresmentioning

confidence: 99%

Global three-dimensional simulations of outer protoplanetary discs with ambipolar diffusion

Cui

Bai

2021

Monthly Notices of the Royal Astronomical Society

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“…Various instabilities are proposed as a possible mechanism to form planetesimals. The streaming instability is one example (e.g., Youdin & Goodman 2005; disks and debris disks (Takahashi & Inutsuka 2014;Tominaga et al 2018). Moreover, the secular GI is one of the possible mechanisms to create multiple rings that recent observations with Atacama Large Millimeter/submillimeter Array (ALMA) have found in some protoplanetary disks (e.g., ALMA Partnership et al 2015;Andrews et al 2016;Tsukagoshi et al 2016;Isella et al 2016;Fedele et al 2017Fedele et al , 2018.…”

Section: Introductionmentioning

confidence: 99%

Revised Description of Dust Diffusion and a New Instability Creating Multiple Rings in Protoplanetary Disks

Tominaga

Takahashi

Inutsuka

2019

ApJ

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Various instabilities have been proposed as a promising mechanism to accumulate dust. Moreover, some of them are expected to lead to the multiple-ring structure formation and the planetesimal formation in protoplanetary disks. In a turbulent gaseous disk, the growth of the instabilities and the dust accumulation are quenched by turbulent diffusion of dust grains. The diffusion process has been often modeled by a diffusion term in the continuity equation for the dust density. The dust diffusion model, however, does not guarantee the angular momentum conservation in a disk. In this study, we first formulate equations that describe the dust diffusion and also conserve the total angular momentum of a disk. Second, we perform the linear perturbation analysis on the secular gravitational instability (GI) using the equations. The results show that the secular GI is a monotonically growing mode, contrary to the result of previous analyses that found it overstable. We find that the overstability is caused by the non-conservation of the angular momentum. Third, we find a new axisymmetric instability due to the combination of the dust-gas friction and the turbulent gas viscosity, which we refer to as two-component viscous gravitational instability (TVGI). The most unstable wavelength of TVGI is comparable to or smaller than the gas scale height. TVGI accumulates dust grains efficiently, which indicates that TVGI is a promising mechanism for the formation of multiple-ring-like structures and planetesimals. Finally, we examine the validity of the ring formation via the secular GI and TVGI in the HL Tau disk and find both instabilities can create multiple rings whose width is about 10 au at orbital radii larger than 50 au.

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“…Pinte et al (2016) show that apparent gaps of HL Tau require α ∼ 10 −4 . Note that such a small α is favorable for creating the observed multiple ring-like structure in HL Tau through secular gravitational instability (Takahashi & Inutsuka 2014Tominaga et al 2018). Impact velocities of v imp ≤ 40 cm/s are found in protoplanetary disks with α ∼ 10 −4 (see Fig.…”

Section: Turbulencementioning

confidence: 91%

Collisional elongation: Possible origin of extremely elongated shape of 1I/‘Oumuamua

Sugiura

Kobayashi

Inutsuka

2019

Icarus

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Light curve observations of a recently discovered interstellar object 1I/'Oumuamua suggest that this object has an extremely elongated shape with the axis ratio 0.3 or smaller. Planetesimal collisions can produce irregular shapes including elongated shapes. In this paper, we suggest that the extremely elongated shape of 1I/'Oumuamua may be the result of such an impact. To find detailed impact conditions to form the extremely elongated objects, we conduct numerical simulations of planetesimal collisions using Smoothed Particle Hydrodynamics method for elastic dynamics with self-gravity and interparticle friction. Impacts into strengthless target planetesimals with radius 50 m are conducted with various ratios of impactor mass to target mass q, friction angles φ d , impact velocities v imp , and impact angles θ imp . We find that impacts with q ≥ 0.5, φ d ≥ 40 • , v imp ≤ 40 cm/s, and θ imp ≤ 30 • produce remnants with the ratio of intermediate to major axis length less than 0.3. This impact condition suggests that the parent protoplanetary disk in the planetesimal collision stage was weakly turbulent (α < 10 −4 for the inner disk) and composed of planetesimals smaller than ∼ 7 km to ensure small impact velocity.

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Non-linear development of secular gravitational instability in protoplanetary disks

Cited by 43 publications

References 20 publications

Global three-dimensional simulations of outer protoplanetary discs with ambipolar diffusion

Global three-dimensional simulations of outer protoplanetary discs with ambipolar diffusion

Revised Description of Dust Diffusion and a New Instability Creating Multiple Rings in Protoplanetary Disks

Collisional elongation: Possible origin of extremely elongated shape of 1I/‘Oumuamua

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