Publications
Section: PZ: main journal
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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.
8001 magnitude measurements in the B, V, and I_c filters were acquired for the high-amplitude delta Scuti variable V2455 Cyg. The observations and light curves are presented.
1665 magnitude measurements in the B, V, g', and r' filters were acquired for the double-mode Cepheid AS Cas. The light curves for both fundamental and first-overtone modes were constructed.
I present a detection of a new double-mode type~II Cepheid (BL Her type), USNO-B1.0 0992-0344981, pulsating in the fundamental and first-overtone modes. It is the fifth case in the Galaxy of stars of this type. For the analysis, I used all observations available for the star in the ASAS-SN, ASAS-3, NSVS, and ZTF online public archives. Light elements and parameters of the light curves were obtained. |
