Modelling the Gas Dynamics of Protoplanetary Disks by the SPH Method

Demidova, T. V.

doi:10.1007/s10511-016-9448-3

Cited by 9 publications

(7 citation statements)

References 61 publications

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“…The evolution of the remnant in the gas disk was simulated by the smoothed particle hydrodynamics (SPH) method. The calculations were performed using the code Gadget-2 (Springel et al 2001;Springel 2005) modified by us (Demidova 2016). In total, from 5 × 10 5 to 2.5 × 10 6 particles of the gas disk and from 5 × 10 3 to 2 × 10 5 particles of the perturbation were involved in the simulations.…”

Section: Methodsmentioning

confidence: 99%

Clumpy Accretion in Pre-main-sequence Stars as a Source of Perturbations in Circumstellar Disks

Demidova

Гринин

2022

ApJ

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The development of perturbations in the circumstellar disks of pre-main-sequence stars caused by clumpy accretion was investigated. Here we perform 3D smoothed particle hydrodynamics simulations of disks perturbed by a recent clump accretion event. These simulations are further explored by radiative transfer calculations to quantify the observational appearance of such disks. It was shown that the density waves in the disks were formed at the fall of the clump. After several revolutions they can transform into spirals and ring structures. Their images in millimeter wavelengths are very similar to those observed with Atacama Large Millimeter/submillimeter Array in some protoplanetary disks. We assume that clumpy accretion may be the source of such structures.

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Section: Methodsmentioning

confidence: 99%

Clumpy Accretion in Pre-main-sequence Stars as a Source of Perturbations in Circumstellar Disks

Demidova

Гринин

2022

ApJ

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“…The evolution of the remnant in gas disk was simulated by the SPH method (smooth particle hydrodynamics). The calculations were performed using the code Gadget-2 (Springel et al 2001;Springel 2005) modified by us (Demidova 2016). In total, from 5 • 10 5 to 2.5 • 10 6 particles of the gas disk and from 5 • 10 3 to 2 • 10 5 particles of the perturbation were involved in the simulations.…”

Section: Methodsmentioning

confidence: 99%

Clumpy accretion in pre-main-sequence stars as a source of perturbations in circumstellar disks

Demidova,

Grinin

2022

Preprint

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The development of perturbations in the circumstellar disks of pre-main-sequence stars caused by clumpy accretion was investigated. Here we perform 3D hydrodynamical SPH simulations of disks perturbed by a recent clump accretion event. These simulations are further explored by radiative transfer calculations to quantify observational appearance of such disks. It was shown that the density waves in the disks were formed at the fall of the clump. After several revolutions they can transform into spirals and ring structures. Their images in mm-wavelengths are very similar to those observed with ALMA in some protoplanetary disks. We assume that the clumpy accretion may be the source of such structures.

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“…We modified this code and applied it to the computations of hydrodynamic flows in the models described above. A detailed description of the modified code is presented in Demidova (2016).…”

Section: The Model and Methodsmentioning

confidence: 99%

SPH simulations of structures in protoplanetary disks

Demidova

Гринин

2017

Astron. Lett.

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The hydrodynamic models of the protoplanetary disk, which perturbed by the embeded low-mass companion, were calculated by our modification of GADGET-2 code. The cases of circular and eccentric orbits which can be coplanar or slightly inclined to the disk midplane were considered. The column density of test particles on the line of sight between the central star and observer was computed during the simulations. Then the column density of the circumstellar dust was calculated under the assumption that the dust and gas are well mixed with a mass ratio 1 : 100. To research the influence of the disk orientation relative to the observer on the circumstellar extinction the calculations were made for four angles of inclination of the line of sight to the disk midplane and eight directions along the azimuth. The column density in the circumstellar and circumbinary disk were computed separately. The calculations have shown the periodic variations of column density can arise both in the circumstellar and circumbinary disks. The amplitude and shape of the variation strongly depend on the parameters of the simulated system (eccentricity and inclination of the orbit, the mass ratio of the companion and star) and its orientation in space. The results of our simulations can be used to explain the cyclic variation of the brightness of young UX Ori type stars.

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Modelling the Gas Dynamics of Protoplanetary Disks by the SPH Method

Cited by 9 publications

References 61 publications

Clumpy Accretion in Pre-main-sequence Stars as a Source of Perturbations in Circumstellar Disks

Clumpy Accretion in Pre-main-sequence Stars as a Source of Perturbations in Circumstellar Disks

Clumpy accretion in pre-main-sequence stars as a source of perturbations in circumstellar disks

SPH simulations of structures in protoplanetary disks

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