Mechanisms for eclipsing in exotic eclipsing systems

Гринин, В. П.; Тамбовцева, Л. В.

doi:10.1007/s10511-006-0046-7

Cited by 5 publications

(5 citation statements)

References 33 publications

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“…These authors hypothesized that an optically thick dust cloud obscured most of the star during the minimum while at the same time covering up much of the lineemitting region, causing the change in profile shapes. Grinin & Tambovtseva (1995) calculated H profiles in rough agreement with the observations using a model of the circumstellar obscuration and assuming gas in the inner disk with a velocity distribution similar to our magnetospheric accretion models.…”

Section: Line Profilessupporting

confidence: 77%

Magnetospheres and Disk Accretion in Herbig Ae/Be Stars

Muzerolle

D’Alessio²,

Calvet

et al. 2004

ApJ

230

379

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We present evidence of magnetically mediated disk accretion in Herbig Ae/Be stars. Magnetospheric accretion models of Balmer and sodium profiles calculated with appropriate stellar and rotational parameters are in qualitative agreement with the observed profiles of the Herbig Ae star UX Ori and yield a mass accretion rate of $10 À8 M yr À1 . If more recent indications of an extremely large rotation rate for this object are correct, the magnetic field geometry must deviate from that of a standard dipole in order to produce line emission consistent with observed flux levels. Models of the associated accretion shock qualitatively explain the observed distribution of excess fluxes in the Balmer discontinuity for a large ensemble of Herbig Ae/Be stars and imply typically small mass accretion rates, P10 À7 M yr À1 . In order for accretion to proceed onto the star, significant amounts of gas must exist inside the dust destruction radius, which is potentially problematic for recently advocated scenarios of ''puffed'' inner dust wall geometries. However, our models of the inner gas disk show that for the typical accretion rates we have derived, the gas should generally be optically thin, thus allowing direct stellar irradiation of the inner dust edge of the disk.

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Section: Line Profilessupporting

confidence: 77%

Magnetospheres and Disk Accretion in Herbig Ae/Be Stars

Muzerolle

D’Alessio²,

Calvet

et al. 2004

ApJ

230

379

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“…The blueshifted absorption in the Hα and Na D line profiles is supposed to be an indicator of the wind flows. It should be mentioned, that an alternative interpretation of the Hα line profiles was proposed by Grinin and Tambovtseva (1995) when studying the variability of emission line profiles in Herbig Ae/Be stars: if a dust cloud obscuring successively different parts of the emission region from the observer moves around the star, then characteristic changes must be observed in the Hα line profile. However, the views of the causes of spectroscopic and photometric variability of T Tauri stars have changed noticeably over the elapsed 20 years.…”

Section: Discussionmentioning

confidence: 99%

Wind dynamics and circumstellar extinction variations in the T Tauri star RY Tau

2016

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The wind interaction with the dusty environment of the classical T Tauri star RY Tau has been investigated. During two seasons of 2013-2015 we carried out a spectroscopic and photometric (BV R) monitoring of the star. A correlation between the stellar brightness and the radial velocity of the wind determined from the Hα and Na D line profiles has been found for the first time. The irregular stellar brightness variations are shown to be caused by extinction in a dusty disk wind at a distance of about 0.2 AU from the star. We suppose, that variations of the circumstellar extinction results from cyclic rearrangements of the stellar magnetosphere and coronal mass ejections, which affect the dusty disk wind near the inner boundary of the circumstellar disk.

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“…Then, Δθ≪θ. With the help of from the paper by Grinin & Tambovtseva (2006), one can obtain the optical depth of the cone ‘wall’ along the radius r ′ 1 r ′ 2 , which at the small γ can be replaced by the radius r 1 r 2 and is parallel to the disc plane and intersects the disc axis at the distance h from the point O′ (Fig. 3).…”

Section: Precession Scenariomentioning

confidence: 99%

Disc wind in the HH 30 binary models

Тамбовцева

Гринин

2008

Monthly Notices of the Royal Astronomical Society

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Recent interferometric observations of the young stellar object(YSO) HH 30 have revealed a low velocity outflow in the $^{12}$CO J=1-2 molecule line (Pety et al. 2006). We present here two models of the low velocity disc winds with the aim of investigating an origin of this molecular outflow. Following Andlada et al. (2006) we treated HH 30 as a binary system. Two cases have been considered: i) the orbital period $P$ = 53 yrs and ii) $P \le$ 1 yr. Calculations showed that in the first case the outflow cone had a spiral-like structure due to summing the velocities of the orbital motion and the disc wind. Such a structure contradicts the observations. In the second case, the outflow cone demonstrates a symmetry relatively to the system axis and agrees well with the observations.Comment: 5 pages, 4 figures. accepted by Mon. Not. R. Astron. So

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Mechanisms for eclipsing in exotic eclipsing systems

Cited by 5 publications

References 33 publications

Magnetospheres and Disk Accretion in Herbig Ae/Be Stars

Magnetospheres and Disk Accretion in Herbig Ae/Be Stars

Wind dynamics and circumstellar extinction variations in the T Tauri star RY Tau

Disc wind in the HH 30 binary models

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