Variable stars observer DPV

Pavol A. Dubovský

dpv

Observing statistics in 2022

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Observing time dedicated to CCD time series observations in Kolonica and total number of light curves

Number of visual estimates in 2020: 1108

Total number of visual estimates: 74355

Visual observations

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Light curves of several semiregular and symbiotic variables from my program. Visual estimates together with data from ASAS-SN survey and CCD observations from AAVSO database. Some time visual data are useful (WY And), sometime the advantage of one visual observer is visible (CH Cyg), sometime visual data fill the gap in the survey data (TZ Cep), sometime visual observation are completely wrong (CK Vir).

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V723 Cas

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Nova Cas 1995 probably finished its long supersoft X-ray source phase. This SSS phase was accompanied with periodic (0.6932672d) brightness variation interpreted as orbital wave. The amplitude of these variations increased until 2005. It reached 2.0 mag in the B band. Then it was decreasing slowly. The abrupt change came in 2015. Goranskij et al. reported amplitude only 0.3 mag (2015ATel.7985….1G). I observed V723 Cas regularly since 2010 with 1 meter VNT telescope. Unfortunately in 2015 Goranskij was the first to observe the target.

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Eclipsing polar V808 Aur

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Previously known as CRTS J071126.0+440405 discovered in January 2009 by Catalina Sky Survey as relatively bright polar with deep eclipses. In the active state there is a pre-eclipse dip at phase -0.13 interpreted as eclipse caused by accretion stream falling toward white dwarf. The deep eclipse is the occultation of the hot spot by the secondary. The hot spot is also occulted by the white dwarf itself for half the spin period, opposite to the phase of the deep eclipse. I’m observing the object with 1 meter VNT telescope several times each season. High and low states with 3 magnitude difference are also observed.

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