Publications
Section: PZ: main journal
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I present a detection of 44 new double-mode high-amplitude delta Scuti variable stars, HADS(B) type, pulsating in the fundamental and first overtone modes. We analyzed all observations available for these stars in the ASAS-SN online public archive using the period-search software developed by Dr. V.P. Goranskij for Windows environment. Additionally, in individual cases, I used data of the SuperWASP, CSS, and ASAS-3 surveys. Light elements and parameters of the light curves of both oscillations were obtained.
We obtained several light curves of V957 Cep in 2009, 2011, 2013, 2016, and 2019 at the Crimean Astronomical Station of M.V. Lomonosov Moscow State University and at the Tien Shan Observatory of the V.G. Fesenkov Astrophysical Institute. Using the TESS satellite observations, we found brightness variations of V957 Cep with the period P_p=0.664 d and amplitude A_p=0.0076 mag. For our light curves (2009-2019) and TESS light curves (2019-2020), orbital elements were computed and a new value of the apsidal motion rate d(omega)/dt=1.47 deg +/- 0.15 deg per year was derived. We found a possible light-time effect that can indicate gravitational influence of one or several additional bodies in the system on the central binary. Based on the currently available data, the amplitude and period of the light-time effect still cannot be reliably estimated.
We present calculations of radial velocity corrections along the phase curve due to influence of the spotted surface of the active giant, PZ Mon. The maximum deviation from a relatively uniformly-bright stellar disk is about 0.20 - 0.25 km/s.
We describe our attempt to find new candidate classical Cepheids and other pulsating variable stars in the LAMOST spectroscopic survey using GAIA EDR3 data and existing photometric archives. Several stars deserve dedicated photometric observations.
New observations of V961 Cep, an eclipsing star with elliptical orbit (P=7.04 d, V=10.14 m, e=0.03, F0 V+F5 V) revealed that its primary component was a delta Sct variable with the period P=0.0482603 d and a pulsation amplitude of 0.009 m in the V band.
I present a detection of 118 new double-mode high-amplitude Delta Scuti variable stars, HADS(B) type, pulsating in the fundamental and first overtone modes. We analyzed all observations available for these stars in the ASAS-SN online public archive using the period-search software developed by Dr. V.P. Goranskij for Windows environment. Additionally, in individual cases, I used data of the SuperWASP, CSS, ASAS-3, and NSVS surveys. Light elements and parameters of the light curves of both oscillations were obtained.
We present a new Name-List of variable stars containing information on 779 variable stars in globular star clusters (constellations Lynx - Ophiuchus; 27 clusters in 4 constellations) that now get their names in the system of the General Catalogue of Variable Stars (GCVS). Also, GCVS names are assigned to eleven recent Novae in our Galaxy. A correction to the 83rd Name-list of variable stars is announced.
In September, 2021, we obtained about 1100 UBVRcIc CCD observations of the dwarf nova with coordinates RA=23h11m10.9s; Dec=+01deg30'03" (J2000) during its outburst. Our analysis of this photometric series showed that the studied variable star had superhumps at stage "B"; two rebrightenings were detected after the end of the outburst. The mass component ratio q = 0.06 was estimated; color temperature variations during the outburst were studied. The variable is a typical WZ Sge star with a short superhump period, 0.0516days. The detected period is close to the lower limit for the WZ Sge variables.
We present the results of long-term photometry (2009-2021) of the new W UMa-type star GSC 3599-2569 discovered in 2013 at the Kourovka Observatory. We have found a change in the period of this eclipsing system. Based on more extensive observational data, the previously detected cyclical change in the brightness of the system, not associated with eclipses and caused by spot activity on the surface of the components, was confirmed. The length of this period has been specified. 11 new times of minima of GSC~3599-2569 are presented.
An analysis of the new UBVR_cI_c observations of V1674 Her obtained by the authors shows that the star is a very fast Nova, with parameters T_2 = 1.1d, T_3 = 2.2d. The orbital period at the brightness decline, 39 - 56 days after the outburst, was 0.15290d, the shape of the light curve featured two unequal minima separated by half a period, the amplitude of the observed wave being 0.12 mag. |
