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

Demidova, T. V.; Гринин, В. П.

doi:10.3847/1538-4357/ac53a6

Cited by 6 publications

(1 citation statement)

References 40 publications

(43 reference statements)

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“…In the rest of this section, we aim to provide a rough quantification about the possible presence of giant planets in relation with the SED groups and the stellar metallicities, based on observed disk structures from high-resolution techniques. It must be noted that such a quantification is difficult to assess, given that most (if not all) structures observed in protoplanetary disks can be potentially explained either invoking the presence of planets or different phenomena (for a recent example, see, e.g., Demidova & Grinin 2022).…”

Section: Planet Candidates Metallicities and Sed Groupsmentioning

confidence: 99%

Relation between metallicities and spectral energy distributions of Herbig Ae/Be stars

Díaz

Montesinos

Mendigutía

et al. 2023

A&A

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Context. Most studies devoted to Herbig Ae/Be stars (HAeBes) assume solar metallicity. However, the stellar metallicity, [M/H], is a fundamental parameter that can strongly differ depending on the source and may have important implications for planet formation. It has been proposed that the deficit of refractory elements observed in the surfaces of some HAeBes may be linked to the presence of cavities in their disks and is likely caused by Jovian planets that trap the metal-rich content. Aims. This work aims to provide a robust test on the previous proposal by analyzing the largest sample of HAeBes characterized by homogeneously derived [M/H] values and stellar and circumstellar properties. Methods. The spectra of 67 HAeBes, along with their well-known properties drawn from our previous work, have been collected from the ESO Science Archive Facility. Their [M/H] values were derived based on the comparison with Kurucz synthetic models. Statistical analyses were carried out with the aim to test the potential relation between [M/H] and the Meeus group I sources, with spectral energy distributions (SEDs) associated with the presence of cavities potentially carved by giant planets. We critically analyzed the eventual link between [M/H], the SED groups, and the presence of such planets. Results. Our statistical study robustly confirms that group I sources tend to have a lower [M/H] (typically ~ −0.10) than that of group II HAeBes (~ +0.14). A similar analysis involving SED-based transitional disks, with infrared excess only at wavelengths of ≥2.2 µm, does not reveal such a relation with [M/H]. This result indicates that not all processes capable of creating holes in the inner dust disks end up having an effect on the stellar abundances. The spatial distributions of group I and II sources are similar, at least within the available range of distances to the galactic centre and the galactic plane, for which the observed [M/H] differences are not driven by environmental effects. In addition, group I sources tend to have stronger (sub-) mm continuum emission presumably related to the presence of giant planets. Indeed, literature results indicate that disk substructures probably associated with the presence of giant planets are up to ten times more frequent in group I HAeBes than in group II. Finally, along with the metallicities derived for the whole sample, surface gravities and projected rotational velocities are additional outcomes reported in this work. Conclusions. We provide indirect evidence to suggest that giant planets are more frequent around group I/low [M/H] stars than around the rest of the HAeBes. However, a direct test of the previous hypothesis requires multiple detections of forming planets in their disks. Such detections have so far been limited to the candidate around the metal depleted ([M/H] = −0.35 ± −0.25) group I HAeBe star AB Aur, which is consistent with our findings.

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Section: Planet Candidates Metallicities and Sed Groupsmentioning

confidence: 99%

Relation between metallicities and spectral energy distributions of Herbig Ae/Be stars

Díaz

Montesinos

Mendigutía

et al. 2023

A&A

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Comparison of Two Methods for Modeling the Dynamics of Gas Flows in a Protoplanetary Disk

Grigoryev¹,

Demidova²

2023

Communications in Computer and Information Science

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Cloudlet capture model for the accretion streamer onto the disc of DG Tau

Hanawa,

Garufi,

Podio

et al. 2024

Monthly Notices of the Royal Astronomical Society

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DG Tau is a nearby T Tauri star associated with a collimated jet, a circumstellar disk and a streamer a few hundred au long. The streamer connects to the disk at ∼50 au from DG Tau. At this location SO emission is observed, likely due to the release of sulphur from dust grains caused by the shock of the impact of the accretion streamer onto the disk. We investigate the possibility that the DG Tau streamer was produced via cloudlet capture on the basis of hydrodynamic simulations, considering a cloudlet initiating infall at 600 au from DG Tau with low angular momentum so that the centrifugal force is smaller than the gravitational force, even at 50 au. The elongation of the cloudlet into a streamer is caused by the tidal force when its initial velocity is much less than the free-fall velocity. The elongated cloudlet reaches the disk and forms a high density gas clump. Our hydrodynamic model reproduces the morphology and line-of-sight velocity of CS (5 − 4) emission from the Northern streamer observed with ALMA. We discuss the conditions for forming a streamer based on the simulations. We also show that the streamer should perturb the disk after impact for several thousands of years.

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

Cited by 6 publications

References 40 publications

Relation between metallicities and spectral energy distributions of Herbig Ae/Be stars

Relation between metallicities and spectral energy distributions of Herbig Ae/Be stars

Comparison of Two Methods for Modeling the Dynamics of Gas Flows in a Protoplanetary Disk

Cloudlet capture model for the accretion streamer onto the disc of DG Tau

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