Kabardino Balkaria, Russia
Kabardino Balkaria, Russia

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Weselak T.,Kazimierz Wielki University in Bydgoszcz | Galazutdinov G.A.,Católica del Norte University | Galazutdinov G.A.,Pulkovo Observatory | Sergeev O.,International Center for Astronomical | And 3 more authors.
Acta Astronomica | Year: 2014

The analysis of radial velocities of interstellar spectral features: CH, CH+ as well as 4964 and 6196 diffuse interstellar bands, seen in spectra of HD 151932 and HD 152233, suggests that carrier of the former is spatially correlated with CH while that of the latter - with CH+. A further analysis, done in this paper and based on the sample of 106 reddened OB stars, partly confirms this suggestion, showing that the CH column density correlates indeed much better with the equivalent width of the 4964 DIB than with that of the 6196 DIB. However, the strengths of the 6196 DIB correlate only marginally better with CH+ than with CH.


Krisandova Z.,Slovak Academy of Sciences | Ivanova O.,Main Astronomical Observatory of the NAS of Ukraine | Svoren J.,Slovak Academy of Sciences | Borisenko S.,Main Astronomical Observatory of the NAS of Ukraine | And 3 more authors.
Contributions of the Astronomical Observatory Skalnate Pleso | Year: 2014

We present photometric data of Comet C/2012 S1 (ISON) observed at heliocentric distance of 6.2-4.6 AU. The observations were made with the 60-cm telescope Zeiss-600 (ICAMER, p. Terskol, Russia). We analyze B, V and R bands images to describe the dusty cometary coma and to investigate its brightness.


Zhilyaev B.E.,Ukrainian Academy of Sciences | Andreev M.V.,International Center for Astronomical | Sergeev A.V.,International Center for Astronomical | Reshetnik V.N.,Taras Shevchenko National University | Parakhin N.A.,International Center for Astronomical
Astronomy Letters | Year: 2012

We present the results of fast spectrophotometry for two flares on EV Lac with a time resolution of 8 s and a spectroscopic resolution R ~100. The observations were performed in May and August 2010 with a slitless spectrograph on the Zeiss-600 telescope at Peak Terskol. We have estimated the UBVR magnitudes from spectrograms through a mathematical convolution of the spectra with the filter transmission curves. The UBV R amplitudes of the August 10, 2010 flare are 2m .83, 1m .94, 0m .82 and 0m .28, respectively. The UBV R amplitudes of the May 30, 2010 flare are 0m .25, 0m .15, 0m .10, 0m .28 respectively. A detailed colorimetric analysis has allowed important parameters of the flares on EV Lac to be estimated: the temperatures at maximum light and their sizes. The color-color (U - B)-(B - V) diagrams confirm that both flares at maximum light radiate as a blackbody. The temperatures at maximum light was 13 400 ± 500 K for the August flare and 5700 ± 100 K for the May flare. During the May flare, an additional hydrogen emission appeared in the Balmer Hα, Hβ, Hγ, Hδ, He{open}, Hζ lines and the Balmer continuum (3647 Å) in the spectrum of EV Lac. The excess of emission in the Balmer lines was approximately from two to thirty percent. Based on our colorimetric analysis, we have estimated the linear sizes of the flares at maximum light. The size of the May 30, 2010 flare is approximately 7% of the stellar radius. The size of the August 10, 2010 flare is 3. 9% of the stellar radius. © 2012 Pleiades Publishing, Ltd.


Zhilyaev B.E.,Ukrainian Academy of Sciences | Verlyuk I.A.,Ukrainian Academy of Sciences | Andreev M.V.,International Center for Astronomical | Sergeev A.V.,International Center for Astronomical | And 10 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2013

V390 Aurigae is a rapidly rotating, chromospherically active late-type giant. The X-ray emission from the corona of V390 Aur, observed by the XMM-Newton space observatory, indicates intense flaring activity on this star. Multisite, coordinated high-speed UBVRI photometry of V390 Aur and a reference starwas carried out in years 2002-2009 at the Peak Terskol, Crimean and Belogradchik observatories, aimed at finding persistent variability on millisecond-tosubsecond time-scales. We find that variability is peaked at f ~ 1Hz, gradually subsiding in the range 0.1-10 Hz, with the peak rms amplitude of 0.005 mag in the UBV bands. We conclude that the light curves of V390 Aur contain microflares that may be responsible for the observed activity on subsecond time-scales, with a relative power of fluctuations reaching (2.1-3.0) × 10-5 in the UBV bands. © 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.


Sharova O.I.,Radiophysical Research Institute | Agafonov M.I.,Radiophysical Research Institute | Karitskaya E.A.,Russian Academy of Sciences | Bochkarev N.G.,13 Universitetskij pr | And 3 more authors.
Proceedings of the International Astronomical Union | Year: 2011

The 2D and 3D Doppler tomograms of X-ray binary system Cyg X-1 (V1357 Cyg) were reconstructed from spectral data for the line HeII 4686Å obtained with 2-m telescope of the Peak Terskol Observatory (Russia) and 2.1-m telescope of the Mexican National Observatory in June, 2007. Information about gas motions outside the orbital plane, using all of the three velocity components Vx, Vy, Vz, was obtained for the first time. The tomographic reconstruction was carried out for the system inclination angle of 45°. The equal resolution (50 × 50 × 50 km/s) is realized in this case, in the orbital plane (Vx, Vy) and also in the perpendicular direction Vz. The checkout tomograms were realized also for the inclination angle of 40° because of the angle uncertainty. Two versions of the result showed no qualitative discrepancy. Details of the structures revealed by the 3D Doppler tomogram were analyzed. © International Astronomical Union 2012.

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