Unusual recurrent eclipses of the UX Ori star WW Vul

Rostopchina-Shakhovskaja, A. N.; Гринин, В. П.; Shakhovskoi, D. N.

doi:10.1007/s10511-012-9223-z

Cited by 10 publications

(3 citation statements)

References 24 publications

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“…Such asymmetries are often attributed to dust trapped in A&A 605, A122 (2017) large-scale vortices that are able to collect large amounts of dust grains with sizes of the order of ∼1 mm. Another indirect way to detect vortices in disks is the fortuitous observation of eclipses of a young star by the trapped dust in a highly inclined disk (Barge & Viton 2003;Rostopchina-Shakhovskaja et al 2012).…”

Section: Introductionmentioning

confidence: 99%

“…Such asymmetries are often attributed to dust trapped in large-scale vortices which are able to collect large amounts of dust grains with sizes of the order of ∼ 1 mm. Another indirect way to detect vortices in disks is the fortuitous eclipses of a young star by the trapped dust in a highly inclined disk (Barge & Viton 2003;Rostopchina-Shakhovskaja et al 2012). In this paper, numerical simulations are performed to follow the evolution of dust particles embedded in a gas disk that contains a vortex.…”

Section: Introductionmentioning

confidence: 99%

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Gaps and rings carved by vortices in protoplanetary dust

Barge

Ricci

Carilli

et al. 2017

A&A

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Context. Large-scale vortices in protoplanetary disks are thought to form and survive for long periods of time. Hence, they can significantly change the global disk evolution and particularly the distribution of the solid particles embedded in the gas, possibly explaining asymmetries and dust concentrations recently observed at submillimeter and millimeter wavelengths. Aims. We investigate the spatial distribution of dust grains using a simple model of protoplanetary disk hosted by a giant gaseous vortex. We explore the dependence of the results on grain size and deduce possible consequences and predictions for observations of the dust thermal emission at submillimeter and millimeter wavelengths. Methods. Global 2D simulations with a bi-fluid code are used to follow the evolution of a single population of solid particles aerodynamically coupled to the gas. Possible observational signatures of the dust thermal emission are obtained using simulators of ALMA and Nest Generation Very Large Array (ngVLA) observations. Results. We find that a giant vortex not only captures dust grains with Stokes number S t < 1 but can also affect the distribution of larger grains (with S t ∼ 1) carving a gap associated with a ring composed of incompletely trapped particles. The results are presented for different particle sizes and associated with their possible signatures in disk observations. Conclusions. Gap clearing in the dust spatial distribution could be due to the interaction with a giant gaseous vortex and their associated spiral waves without the gravitational assistance of a planet. Hence, strong dust concentrations at short sub-mm wavelengths associated with a gap and an irregular ring at longer mm and cm wavelengths could indicate the presence of an unseen gaseous vortex.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Gaps and rings carved by vortices in protoplanetary dust

Barge

Ricci

Carilli

et al. 2017

A&A

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“…(ii) With a certain combination of the disc wind parameters and the radiation wavelength the polarization degree may not change or change in a narrow range during an eclipse. Rostopchina-Shakhovskaja et al (2012) observed such eclipses of the UX Ori star WW Vul.…”

Section: Introductionmentioning

confidence: 96%

UX Ori Stars Eclipses by Large-Scale Disc Perturbations

Shulman,

Grinin

2021

Preprint

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The eclipses of UX Ori type stars by large-scale disc humps are studied in detail. The influence of the hump extension on the eclipse depth and parameters of the linear polarization is modelled and compared with a compact cloud eclipse model. Eclipses were investigated both for the flared disc and for the disc with a puffing-up in the dust sublimation zone. It is shown that the large-scale hump eclipse may be significantly deeper than a compact cloud eclipse and show a greater linear polarization degree compared to it. It is also demonstrated that the hump extension together with the disc puffing-up can strongly affect the degree of polarization and colour index of the star during the eclipse. The position angle of the linear polarization may also change markedly during and after an eclipse by a large scale hump for the model with a puffed-up inner rim. Also, in this model, the maximum degree of the linear polarization can be achieved not at the brightness minimum, but closer to the end of the eclipse.

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T Tauri and Herbig Ae/Be stars

Bastien¹,

Kolokolova²,

Hough³

et al. 2015

Polarimetry of Stars and Planetary Systems

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Observations of magnetic fields of stars at the pre-main sequence phase can provide important new insights into the complex physics of the late stages of star formation. This is especially true at intermediate stellar masses, where magnetic fields are strong and globally organised, and therefore most amenable to direct study. Recent circularly-polarised spectroscopic observations of pre-main sequence Herbig Ae/Be stars have revealed the presence of organised magnetic fields in the photospheres of a small fraction of these objects. To date, 9 magnetic HAeBe stars have been detected, and those detections confirmed by repeated observations. The morphology and variability of their Stokes V signatures indicates that their magnetic fields have important dipole components of ∼kG strength, and that the dipole is stable on timescales ofat least years. These magnetic stars exhibit a large range of stellar mass, from ∼ 2 − 13 M ⊙ , and diverse rotational properties, with v sin i from a few km/s to ∼ 200 km/s. Most magnetic HAeBe stars show approximately solar abundances; they clearly do not generally exhibit the strong and systematic peculiarities of the magnetic main sequence A and B type stars (the Ap/Bp stars). The observed fractional bulk incidence of magnetic HAeBe stars is about 7%, a value compatible with the incidence of magnetic intermediate-mass stars on the main sequence. This low incidence is at odds with formation scenarios generally involving magneticallymediated accretion. The similarily between the magnetic properties of the premain sequence and main sequence intermediate-mass stars appears compatible with the hypothesis of a fossil origin of magnetism in these objects.

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Unusual recurrent eclipses of the UX Ori star WW Vul

Cited by 10 publications

References 24 publications

Gaps and rings carved by vortices in protoplanetary dust

Gaps and rings carved by vortices in protoplanetary dust

UX Ori Stars Eclipses by Large-Scale Disc Perturbations

T Tauri and Herbig Ae/Be stars

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