Photometric and polarimetric activity of RZ Psc

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

doi:10.1134/1.1592837

Cited by 19 publications

(35 citation statements)

References 7 publications

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“…The brightness variability of RZ Psc has been presented in previous publications that reported a quasi-periodic variation of the stellar flux level during bright periods, albeit with different periods (Shakhovskoi et al 2003;Rostopchina et al 1999). Here we present a rigorous analytical period search with the aim to settle the question of any periodicity in RZ Psc's photometric data of the past forty years.…”

Section: Optical Variabilitymentioning

confidence: 76%

Active asteroid belt causes the UXOR phenomenon in RZ Piscium

Wit

Гринин

Potravnov

et al. 2013

A&A

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We report the discovery of mid-infrared excess emission in the young object RZ Psc. The excess constitutes ∼8% of its L bol and is well fit by a single 500 K blackbody, implying a dust-free region within ∼0.7 AU for optically thick dust. The object displays dust obscuration events (UXOR behaviour) on a time scale that suggests dusty material on orbits of ∼0.5 AU. We also report a 12.4-year cyclical photometric variability that can be interpreted as caused by perturbations in the dust distribution. The system is characterized by a high inclination, marginal extinction (during bright photometric states), a single temperature for the warm dust, and an age estimate that puts the star beyond the formation stage. We propose that the dust occultation events present a dynamical view of an active asteroid belt whose collisional products sporadically obscure the central star.

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Section: Optical Variabilitymentioning

confidence: 76%

Active asteroid belt causes the UXOR phenomenon in RZ Piscium

Wit

Гринин

Potravnov

et al. 2013

A&A

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“…In this regard it is interesting to take note of a photometric period of about 1000 days for CQ Tau [18], which is responsible for a low amplitude variability of the star. Given the above remarks, the existence of a regularity in the motion of the dust clouds may affect the observed shape of the Na I D sodium line profiles.…”

Section: The Resonance Sodium Doublet Na I D Linesmentioning

confidence: 99%

Structure of the inner region of the accretion disk of the Herbig Ae star CQ Tau based on long-term monitoring data

et al. 2007

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Results from simultaneous spectral and photometric monitoring of the Herbig Ae star CQ Tau in the neighborhood of the Hα and resonance sodium doublet Na I D lines are presented. It is shown that the inner structure of the accretion disk of CQ Tau is nonuniform and consists of two regions with quite different kinematic characteristics. Region I is characterized by relative stability and a smooth long-term variation in the velocity of the gas along the line of sight. Region II is distinguished by the highest velocities and a variability in their maximum values over time scales from a few days to 700 days. The dust clouds which produse the star's brightness minima may also be the source of cold gas and contribute to the observed spectral variability. We assume that region I of the disk coincides with the accretion disk of the star. The kinematic differences in region II may be caused by dissipation of circumstellar dust clouds which, moving in elongated orbits, are able to approach the star quite closely.

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“…These observations show that the inner structure of this star's accretion disk varies over a time scale close to 1000 days. Furthermore, CQ Tau has been found to have a 1020 day photometric period [29]. These results may indicate a similarity in the physical mechanisms responsible for the observed changes.…”

Section: Resultsmentioning

confidence: 85%

Structure of the inner regions of the circumstellar gas envelopes around young hot stars. II. The new cycle of spectral activity of the Herbig Ae star HD 31648

2007

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The results of the high-resolution long-term spectral monitoring of the Herbig Ae star HD 31648 in the regions of emission Hα line, Na I D resonance lines and OI 7774 lines are presented. We confirmed the conclusion, made in previous papers, that the spectral variability of the star in the region of Hα line have a cyclic character. It is manifested itself as the changing of the equivalent width and intensity of Hα line of the time scale of about 1200d. It is shown, that the stellar wind is non-homogeneous and consists of several components, which are differed each other by their velocities. They are observed as in the H line as in Na I D resonance lines. The component's parameters are changed during the cycle of stellar activity (in the maximum of activity the velocity and density of the wind are taken the largest values and then they are gradually decreased). The investigation of rapid variability of the He I 5876 line on the time scale of a few hours allows find the correlation between the variability of the blue and the red wings of the line. It points at the connection between the accretion and the outflows. Such connection, in particularly, is predicted by the modeling of the wind from young stars made in the frame of the magneto-centrifugal model, the accordance of which for the HD 31648 was shown in the previous papers. In the present work we confirmed this conclusion on the basis of the new data.We found the weak variability of the stellar brightness (about 0.2m), which is agree with the spectral variability (the brightness of the star becomes lower in the maximum of the activity). These changes are well explained by the process of the dust transfer from CS disk by the stellar wind. This process is likely to be more effective in the maximum of activity.An analysis of the variability of other spectral lines shows the agreement between the changing of the Hα line, the Na I D resonance doublet lines and KI 7698 line. The weak connection between the He I 5876 and the Na I D lines is also found. Since the formation regions of He I 5876 and Na I D lines are essentially different, we can conclude that the phenomena, responsible for the observed cyclic variability, take place in a spacious region of the CS envelope. We believe that the most plausible reason of found cyclic variability is the reconstruction of the inner structure of the CS gas envelope, caused by the presence around the star a low mass companion or planet.

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Photometric and polarimetric activity of RZ Psc

Cited by 19 publications

References 7 publications

Active asteroid belt causes the UXOR phenomenon in RZ Piscium

Active asteroid belt causes the UXOR phenomenon in RZ Piscium

Structure of the inner region of the accretion disk of the Herbig Ae star CQ Tau based on long-term monitoring data

Structure of the inner regions of the circumstellar gas envelopes around young hot stars. II. The new cycle of spectral activity of the Herbig Ae star HD 31648

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