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

Skliarevskii, Aleksandr M.; Pavlyuchenkov, Ya. N.; Vorobyov, Eduard I.

doi:10.1134/s1063772921030045

Cited by 5 publications

(2 citation statements)

References 32 publications

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“…where I ν is the radiation intensity at a given position (r, φ) in the disk, B ν (erg s −1 cm −2 Hz −1 sr −1 ) is the Planck function, T d is the dust temperature, and τ ν = κ ν,sm Σ d,sm + κ ν,gr Σ d,gr is the total optical depth of the small and grown dust populations. The frequency dependent absorption opacities κ ν,sm and κ ν,gr (per gramm of dust mass) for the small and grown dust populations with maximum sizes a * and a max , respectively, were taken from our earlier work (Skliarevskii et al 2021). We assumed that each dust component has a constant slope of p = 3.5 for the dust size distribution that extends from 5 × 10 −3 µm to a * = 1.0 µm for small dust and from a * to a max for grown dust.…”

Section: Evolution Of the Spectral Index In The Postburst Phasementioning

confidence: 99%

“…× 10 −3 µm and 1.0 µm, and grown dust with an adaptive dust size distribution between 1.0 µm and a max . To calculate the spectral indices in the dust millimeter emission, we use the frequency dependent dust absorption opacities from(Skliarevskii et al 2021). For the reader convenience, FigureB.1 presents these opacities as a function of the maximum dust size a max .…”

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Evolution of dust in protoplanetary disks of eruptive stars

Vorobyov

Skliarevskii

Molyarova

et al. 2022

A&A

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Aims. Luminosity bursts in young FU Orionis-type stars warm up the surrounding disks of gas and dust, thus inflicting changes on their morphological and chemical composition. In this work, we aim at studying the effects that such bursts may have on the spatial distribution of dust grain sizes and the corresponding spectral index in protoplanetary disks. Methods. We use the numerical hydrodynamics code FEOSAD, which simulates the co-evolution of gas, dust, and volatiles in a protoplanetary disk, taking dust growth and back reaction on gas into account. The dependence of the maximum dust size on the water ice mantles is explicitly considered. The burst is initialized by increasing the luminosity of the central star to 100–300 L⊙ for a time period of 100 yr. Results. The water snowline shifts during the burst to a larger distance, resulting in the drop of the maximum dust size interior to the snowline position because of more efficient fragmentation of bare grains. After the burst, the water snowline shifts quickly back to its preburst location followed by renewed dust growth. The timescale of dust regrowth after the burst depends on the radial distance so that the dust grains at smaller distances reach the preburst values faster than the dust grains at larger distances. As a result, a broad peak in the radial distribution of the spectral index in the millimeter dust emission develops at ≈10 au, which shifts further out as the disk evolves and dust grains regrow to preburst values at progressively larger distances. This feature is most pronounced in evolved axisymmetric disks rather than in young gravitationally unstable counterparts, although young disks may still be good candidates if gravitational instability is suppressed. We confirmed our earlier conclusion that spiral arms do not act as strong dust accumulators because of the Stokes number dropping below 0.01 within the arms, but this trend may change in low-turbulence disks. Conclusions. We argue that, depending on the burst strength and disk conditions, a broad peak in the radial distribution of the spectral index can last for up to several thousand years after the burst has ended and can be used to infer past bursts in otherwise quiescent protostars. The detection of a similar peak in the disk around V883 Ori, an FU Orionis-type star with an unknown eruption date, suggests that such features may be common in the post-outburst objects.

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Section: Evolution Of the Spectral Index In The Postburst Phasementioning

confidence: 99%

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confidence: 99%

Evolution of dust in protoplanetary disks of eruptive stars

Vorobyov

Skliarevskii

Molyarova

et al. 2022

A&A

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The burst mode of accretion in massive star formation with stellar inertia

Meyer

Vorobyov

Elbakyan

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The burst mode of accretion in massive star formation is a scenario linking the initial gravitational collapse of parent pre-stellar cores to the properties of their gravitationally unstable discs and of their accretion-driven bursts. In this study, we present a series of high-resolution 3D radiation-hydrodynamics numerical simulations for young massive stars formed out of collapsing $100\, \rm M_{\odot }$ molecular cores spinning with several values of the ratio of rotational-to-gravitational energies $\beta =5\%$–$9\%$. The models include the indirect gravitational potential caused by disc asymmetries. We find that this modifies the barycenter of the disc, causing significant excursions of the central star position, which we term stellar wobbling. The stellar wobbling slows down and protracts the development of gravitational instability in the disc, reducing the number and magnitude of the accretion-driven bursts undergone by the young massive stars, whose properties are in good agreement with that of the burst monitored from the massive protostar M17 MIR. Including stellar wobbling is therefore important for accurate modeling disc structures. Synthetic alma interferometric images in the millimeter waveband show that the outcomes of efficient gravitational instability such as spiral arms and gaseous clumps can be detected for as long as the disc is old enough and has already entered the burst mode of accretion.

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Luminosity Outbursts in Interacting Protoplanetary Systems

Skliarevskii,

Vorobyov

2023

Astron. Rep.

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

Cited by 5 publications

References 32 publications

Evolution of dust in protoplanetary disks of eruptive stars

Evolution of dust in protoplanetary disks of eruptive stars

The burst mode of accretion in massive star formation with stellar inertia

Luminosity Outbursts in Interacting Protoplanetary Systems

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