Gravitoviscous protoplanetary disks with a dust component

Vorobyov, Eduard I.; Skliarevskii, Aleksandr M.; Elbakyan, Vardan G.; Pavlyuchenkov, Ya. N.; Akimkin, V. V.; Guêdel, M.

doi:10.1051/0004-6361/201935438

Cited by 32 publications

(26 citation statements)

References 44 publications

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“…Although this is the first study of the MRI-triggered burst phenomenon where dust dynamics and growth is explicitly taken into account, our model of dust growth is still simplistic and needs improvement, with the ultimate goal to employ the Smoluchowski-type integro-differential equation (Drażkowska et al 2019). We have not considered the effects of magnetocentrifugal disk winds that can be efficient in removing mass and angular momentum in the disk regions from several to several tens of astronomical units (e.g., Suzuki et al 2016;Bai 2016;Guedel et al 2019), thus potentially affecting the burst activity by reducing the rate of mass accumulation in the innermost disk regions. It is, however, not easy to take disk winds in the thin-disk hydrodynamic models into account (which may require to relax the zero external current condition in our case) and we will consider several options in the future on how to proceed in this direction.…”

Section: Comparison With Previous Studies and Model Caveatsmentioning

confidence: 99%

Accretion bursts in magnetized gas-dust protoplanetary disks

Vorobyov

Khaibrakhmanov

Basu

et al. 2020

A&A

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Aims. Accretion bursts triggered by the magnetorotational instability (MRI) in the innermost disk regions were studied for protoplanetary gas-dust disks that formed from prestellar cores of a various mass Mcore and mass-to-magnetic flux ratio λ. Methods. Numerical magnetohydrodynamics simulations in the thin-disk limit were employed to study the long-term (~1.0 Myr) evolution of protoplanetary disks with an adaptive turbulent α-parameter, which explicitly depends on the strength of the magnetic field and ionization fraction in the disk. The numerical models also feature the co-evolution of gas and dust, including the back-reaction of dust on gas and dust growth. Results. A dead zone with a low ionization fraction of x≲10−13 and temperature on the order of several hundred Kelvin forms in the inner disk soon after its formation, extending from several to several tens of astronomical units depending on the model. The dead zone features pronounced dust rings that are formed due to the concentration of grown dust particles in the local pressure maxima. Thermal ionization of alkaline metals in the dead zone trigger the MRI and associated accretion burst, which is characterized by a sharp rise, small-scale variability in the active phase, and fast decline once the inner MRI-active region is depleted of matter. The burst occurrence frequency is highest in the initial stages of disk formation and is driven by gravitational instability (GI), but it declines with diminishing disk mass-loading from the infalling envelope. There is a causal link between the initial burst activity and the strength of GI in the disk fueled by mass infall from the envelope. We find that the MRI-driven burst phenomenon occurs for λ = 2–10, but diminishes in models with Mcore ≲ M⊙, suggesting a lower limit on the stellar mass for which the MRI-triggered burst can occur. Conclusions. The MRI-triggered bursts occur for a wide range of mass-to-magnetic flux ratios and initial cloud core masses. The burst occurrence frequency is highest in the initial disk formation stage and reduces as the disk evolves from a gravitationally unstable to a viscous-dominated state. The MRI-triggered bursts are intrinsically connected with the dust rings in the inner disk regions, and both can be a manifestation of the same phenomenon, that is to say the formation of a dead zone.

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Section: Comparison With Previous Studies and Model Caveatsmentioning

confidence: 99%

Accretion bursts in magnetized gas-dust protoplanetary disks

Vorobyov

Khaibrakhmanov

Basu

et al. 2020

A&A

Self Cite

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“…To study the origin of tail-like structures we employed the Formation and Evolution Of a Star And its circumstellar Disk (FEOSAD) code described in detail in . The FEOSAD code was further modified in Vorobyov et al (2019) to include the effect of back reaction of dust on gas. We also introduced the central smart cell (CSC) -a simple model for the innermost disk region which is difficult to resolve in numer-ical hydrodynamics simulations.…”

Section: Numerical Model Of a Gaseous And Dusty Diskmentioning

confidence: 99%

“…In that work, we considered the effect that the mass transport rate through the central smart cell (CSC) can have on the global evolution of the entire disk. Following the notation adopted in Vorobyov et al (2019), we assume that the mass accretion from the CSC on the star is a fraction ξ of mass accretion from the disk to the CSĊ M * ,csc = ξṀ disk forṀ disk > 0, 0 forṀ disk 0.…”

Section: Tail-like Structures Produced By Close Encounters With a (Sumentioning

confidence: 99%

The origin of tail-like structures around protoplanetary disks

Vorobyov

Skliarevskii

Elbakyan

et al. 2020

A&A

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Aims. We study the origin of tail-like structures recently detected around the disk of SU Aurigae and several FU Orionis type stars. Methods. Dynamic protostellar disks featuring ejections of gaseous clumps and quiescent protoplanetary disks experiencing a close encounter with an intruder star were modelled using the numerical hydrodynamics code FEOSAD. Both the gas and dust dynamics were taken into account, including dust growth and mutual friction between the gas and dust components. Only plane-of-the-disk encounters were considered. Results. Ejected clumps produce a unique type of tails that are characterized by a bow-shock shape. These tails owe its origin to the supersonic motion of the ejected clumps through the dense envelope, which often surrounds young gravitationally unstable protostellar disks. The ejected clumps either sit at the head of the tail-like structure or disperse if their mass is insufficient to withstand the head wind of the envelope. On the other hand, close encounters with quiescent protoplanetary disks produce three types of the tail-like structures, which we defined as pre-collisional, post-collisional, and spiral tails. These tails can in principle be distinguished by peculiar features of the gas and dust flow in and around them. We found that the brown-dwarf-mass intruders do not capture circumintruder disks during the encounter, while the sub-solar-mass intruders can acquire appreciable circumintruder disks with elevated dust-to-gas ratios, which can ease their observational detection. However, this is true only for prograde collisions; the retrograde intruders fail to collect an appreciable gas and dust from the disk of the target. The masses of gas in the tails vary in the 0.85-11.8 M Jup limits, while the total mass of dust lies in the 1.75-30.1 M ⊕ range, with the spiral tails featuring the highest masses. The predicted mass of dust in the model tail-like structures is therefore higher than what was inferred for similar structures in SU Aur, FU Ori, and Z CMa, making their observational detection feasible. Conclusions. Tail-like structures around protostellar and protoplanetary disks can act as a smoking gun to infer interesting phenomena, such as clump ejection or close encounters. particular, the bow-shock morphology of the tails could point to clump ejections as a possible formation mechanism. Further numerical and observational studies are needed to better understand the detectability and properties of the tails.

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“…The growth of the dust particles is limited in the model by the so-called fragmentation limit, at which collisions of the dust grains lead not to their coagulation, but to destruction. Using the dynamic FEOSAD model, the details of the dust evolution in a protoplanetary disk were obtained [22], as well as the influence of the inner region of the disk on its evolution [23], and the dynamics of pebbles were investigated [24].…”

Section: Results Of the Modeling Of The Dynamic Evolution Of The Diskmentioning

confidence: 99%

Restoration of the Parameters of a Gas-Dust Disk Based on Its Synthetic Images

2021

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The topic of the present study is combining a dynamic model of a protoplanetary disk with the computations of radiation transfer for obtaining synthetic spectra and disk images suitable for immediate comparison of the model with observations. Evolution of the disk was computed using the FEOSAD hydrodynamic model, which includes a self-consistent calculation of the dynamics of dust and gas in the 2D thin disk approximation. Radiation transfer was simulated by the open code RADMC-3D. Three phases of disk evolution were considered: a young gravitationally unstable disk, a disk during an accretion luminosity burst, and an evolved disk. For these *

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Gravitoviscous protoplanetary disks with a dust component

Cited by 32 publications

References 44 publications

Accretion bursts in magnetized gas-dust protoplanetary disks

Accretion bursts in magnetized gas-dust protoplanetary disks

The origin of tail-like structures around protoplanetary disks

Restoration of the Parameters of a Gas-Dust Disk Based on Its Synthetic Images

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