The EMCCD-based speckle interferometer of the BTA 6-m telescope: Description and first results

Максимов, А. Ф.; Balega, Yu. Yu.; Dyachenko, V. V.; Малоголовец, Е. В.; Растегаев, Д. А.; Semernikov, E. A.

doi:10.1134/s1990341309030092

Cited by 50 publications

(37 citation statements)

References 6 publications

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“…A system of speckle image detection based on a CCD with internal signal amplification was used (Maksimov et al, 2009). Speckle interferograms were obtained with filters having central wavelengths/half-widths of 700/40, 800/100, 900/60 nm in the case of XZ Tau and 800/100 nm in the case of VY Tau.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Orbital motions and light curves of young binaries XZ Tau and VY Tau

et al. 2016

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The results of our speckle interferometric observations of young binaries VY Tau and XZ Tau are presented. For the first time, we found a relative displacement of VY Tau components as well as a preliminary orbit for XZ Tau. It appeared that the orbit is appreciably non-circular and is inclined by i 47 o from the plane of the sky. It means that the rotation axis of XZ Tau A and the axis of its jet are significantly non-perpendicular to the orbital plane. We found that the average brightness of XZ Tau had been increasing from the beginning of the last century up to the mid-thirties and then it decreased by ∆B > 2 mag. The maximal brightness has been reached significantly later on the time of periastron passage. The total brightness of XZ Tau's components varied in a non-regular way from 1970 to 1985 when eruptions of hot gas from XZ Tau A presumably had occurred. In the early nineties the variations became regular following which a chaotic variability had renewed. We also report that a flare activity of VY Tau has resumed after 40 yr pause, parameters of the previous and new flares are similar, and the flares are related with the A component.

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Section: Observations and Data Reductionmentioning

confidence: 99%

Orbital motions and light curves of young binaries XZ Tau and VY Tau

et al. 2016

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“…A system of speckle image detection based on a CCD with internal signal amplification was used [30]. Speckle interferograms were obtained in the visible with filters having central wavelengths of 550 and 800 nm and pass-band halfwidths of 20 and 100 nm, respectively.…”

Section: Observationsmentioning

confidence: 99%

Reverse rotation of the accretion disk in RW Aur A: Observations and a physical model

et al. 2012

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Speckle interferometry of the young binary system RW Aur was performed with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences using filters with central wavelengths of 550 nm and 800 nm and passband halfwidths of 20 nm and 100 nm, respectively. The angular separation of the binary components was 1.448 ′′ ± 0.005 and the position angle of the system was 255.9 o ± 0.3. at the observation epoch (JD 2 454 255.9). We find using published data that these values have been changing with mean rates of +0.002 ′′ /yr and +0.02 o /yr, respectively, over the past 70 years. This implies that the direction of the orbital motion of the binary system is opposite to the direction of the disk rotation in RW Aur A. We propose a physical model to explain the formation of circumstellar accretion disks rotating in the reverse direction relative to young binary stars surrounded by protoplanetary disks. Our model can explain the characteristic features of the matter flow in RW Aur A: the high accretion rate, small size of the disk around the massive component, and reverse direction of rotation.

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“…Speckle interferometric observations of ι UMa were carried out on the SAO 6-m telescope in the near IR in 2009-2010, using an EMCCD-based speckle interferometer [23]. The seeing due to atmospheric effects was 1 in November 2009 and February 2010.…”

Section: Outer Ab Subsystemmentioning

confidence: 99%

“…These data were used to measure the position parameters and brightness differences between the components. The reduction technique applied to the speckleinterferometric 6-m data is described in [23][24][25]. The system was resolved into its components for the first time since 1983.…”

Section: Outer Ab Subsystemmentioning

confidence: 99%

Physical parameters and dynamical properties of the multiple system ι UMa (ADS 7114)

et al. 2012

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We analyze the physical parameters, orbital elements, and dynamic stability of the multiple system ι UMa (HD 76644 = ADS 7114). We have used the positions from the WDS catalog and our own observations on the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences and the 1.5-m Russian-Turkish Telescope (Antalya, Turkey). We have obtained more precise orbital parameters of the subsystems, and spectral types, absolute magnitudes, and masses of the components. The primary has Sp = F0 V-IV, M = 1.7 ± 0.1M , T eff = 7260 ± 70 K, and log g = 4.30 ± 0.07. The companion in the close Aa subsystem is most likely a white dwarf with a mass of approximately 1.0 ± 0.3M . The spectral types and masses of the components in the BC subsystem are M3V, M4V and 0.35 ± 0.05M , 0.30 ± 0.05M , respectively. The total mass is 3.4 ± 0.4M . The Aa subsystem probably has an orbital period of 4470 d = 12.2 y and an eccentricity of approximately 0.6. The outer subsystem seems to have a period of approximately 2084 yrs and an eccentricity of approximately 0.9. We have carried out simulations using the stability criteria and shown that for all possible variations in the component parameters, the multiple system is unstable on a time scale of less than 10 6 years with a probability exceeding 0.98. Possible reasons for this instability are discussed.

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The EMCCD-based speckle interferometer of the BTA 6-m telescope: Description and first results

Cited by 50 publications

References 6 publications

Orbital motions and light curves of young binaries XZ Tau and VY Tau

Orbital motions and light curves of young binaries XZ Tau and VY Tau

Reverse rotation of the accretion disk in RW Aur A: Observations and a physical model

Physical parameters and dynamical properties of the multiple system ι UMa (ADS 7114)

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