The classification of variable stars is essential for understanding stellar evolution and dynamics. With the growing volume of light curve data from extensive surveys, there is a need for automated and accurate classification methods. Traditional methods often rely on manual feature extraction and selection, which can be time-consuming and less adaptable to large datasets. In this work, we present an approach using a convolutional neural network (CNN) to classify variable stars using only raw light curve data and their known periods, without the need for manual feature extraction or hand-selected data preprocessing. Our method utilizes phase-folding to organize the light curves and directly learns the variability patterns crucial for classification. Trained and tested on the Optical Gravitational Lensing Experiment (OGLE) dataset, our model demonstrates an average accuracy of 88% and an F1 score of 0.89 across five well-known classes of variable stars. We also compared our classification model with the Random Forest (RF) classifier and showed that our model gives better results across all of the classification metrics. By leveraging CNN, our approach does not need manual feature extraction and can handle diverse light curve shapes and sampling cadences. This automated, data-driven method offers a powerful tool for classifying variable stars, enabling efficient processing of large datasets from current and future sky surveys.

We present a new study of the Z Cam-type eclipsing cataclysmic variable AY Piscium with the aim of determining the fundamental parameters of the system and the structure of the accretion flow therein. We use time-resolved photometric observations supplemented by spectroscopy in the standstill, to which we applied our light-curve modeling techniques and the Doppler tomography method, to update system parameters. We found that the system has a massive white dwarf M _WD = 0.90(4) M _☉, a mass ratio q = 0.50(3), and the effective temperature of a secondary T ₂ = 4100(50) K. The system inclination is i = 74.°8(7). The orbital period of the system P _orb = 0.217320523(8) day is continuously increasing at a rate of P ̇ orb = + 7.6 ( 5 ) × 10 − 9 day yr⁻¹. The mass-transfer rate varies between 2.4 × 10⁻¹⁰ M _⊙ yr⁻¹ in quiescence up to 1.36 × 10⁻⁸ M _⊙ yr⁻¹ in outburst. The accretion disk transitions from the cooler, flared, steady-state disk to a warmer state with a practically constant and relatively high disk height. The mass-transfer rate is about 1.6 × 10⁻⁹ M _⊙ yr⁻¹ in the standstill. The Balmer emission lines show a multicomponent structure similar to that observed in long-orbital-period nova-like systems. Out of standstill, the system exhibits outburst bimodality, with long outbursts being more prominent. We conclude that the Balmer emission lines in AY Psc are formed by the combination of radiation from the irradiated surface of the secondary, from the outflow zone, and from winds originating in the bright spot and the disk’s inner part.

Eclipsing cataclysmic variables (CVs) are key targets for determining binary system parameters through photometric modeling, yet many of them remain poorly characterized. In this work, we present a list (catalog) of 37 confirmed eclipsing CVs selected based on high-quality and publicly available TESS photometric data. The sample includes both long-period systems (with orbital periods exceeding 4 h), such as Z Cam, U Gem, and nova-like variables, as well as a significant number of SW Sextantis stars. Selection criteria required the presence of clearly defined eclipses and sufficient signal-to-noise ratios for reliable analysis. The catalog provides a foundation for phase-folded light curve studies and future modeling efforts aimed at deriving key physical parameters such as component masses, radii, inclinations, and accretion geometries. Notably, several systems, such as V482 Cam, OZ Dra, ASASSN-14ix, and others, have no previously published physical parameters. Our list is accessible via a dedicated website, where each system will have a separate page, including data from TESS, AAVSO, and ZTF. This resource is intended to support detailed follow-up studies. It may encourage other research groups with observational and modeling expertise to contribute to the investigation of these promising but understudied systems.

Мақалада жалпы білім беретін мектептердегі физика сабақтарына STEMәдістерін кіріктірудің теориялық және практикалық аспектілері қарастырылады. STEM (Science, Technology, Engineering, Mathematics) тәсілі оқушылардың ғылыми-техникалық ойлауын, зерттеушілік қабілеттерін және инженерлік дағдыларын дамытуға бағытталған заманауи білім беру технологиясы ретінде сипатталады. Зерттеу барысында 7-9 сыныптарға арналған физика оқулықтарының мазмұнына талдау жасалып, зертханалық жұмыстар саны мен олардың STEM талаптарына сәйкестігі анықталды. Нәтижесінде 7-8 сыныптарда тәжірибелік жұмыстар жеткілікті деңгейде қамтылғаны, ал 9-сыныпта олардың саны шектеулі екендігі айқындалды. Осыған байланысты 9-сынып физика курсына STEM-жобаларды енгізудің қажеттілігі негізделді. Мақалада оқушылардың теориялық білімдерін тәжірибемен ұштастыруға бағытталған бірқатар STEM жобалар ұсынылған: центрге тартқыш үдеуді анықтау, айналмалы қозғалысты зерттеу, қарапайым лифт моделін құрастыру, реактив арба жасау, акустикалық кабина жобалау және перископ құрастыру. Бұл жобалар оқушылардың физикалық құбылыстарды терең түсінуіне, эксперимент жүргізу дағдыларын қалыптастыруға және пәнаралық байланыстарды жүзеге асыруға мүмкіндік береді. Сонымен қатар, мақалада STEMәдістерін енгізудің артықшылықтары мен шектеулері талданып, Қазақстандағы білім беру жүйесінде оны тиімді жүзеге асырудың негізгі бағыттары айқындалған. STEM тәсілі физика пәнін оқытудың сапасын арттырып, оқушылардың пәнге қызығушылығын күшейтетін тиімді құрал ретінде қарастырылады.

We present a new study of the Z~Cam-type eclipsing cataclysmic variable AY~Piscium with the aim of determining the fundamental parameters of the system and the structure of the accretion flow therein. We use time-resolved photometric observations supplemented by spectroscopy in the standstill, to which we applied our light-curve modeling techniques and the Doppler tomography method, to update system parameters. We found that the system has a massive white dwarf $M_{\rm WD}=0.90(4)$ \ms, a mass ratio $q=0.50(3)$, and the effective temperature of a secondary $T_2 = 4100(50)$~K. The system inclination is $i=74.^{\circ}8(7)$. The orbital period of the system $P_{\mathrm{orb}}=0.217320523(8)\;\mathrm{d}$ is continuously increasing with the rate of $\dot{P}_{\mathrm{orb}} = +7.6(5)\times10^{-9}$ d year$^{-1}$. The mass transfer rate varies between 2.4$\times$10$^{-10}$ M$_\odot$ year$^{-1}$ in quiescence up to 1.36$\times$10$^{-8}$ M$_\odot$ year$^{-1}$ in outburst. The accretion disk transitions from the cooler, flared, steady-state disk to a warmer state with a practically constant and relatively high disk height. The mass transfer rate is about 1.6$\times$10$^{-9}$ M$_\odot$ year$^{-1}$ in the standstill. The Balmer emission lines show a multi-component structure similar to that observed in long-orbital-period nova-like systems. Out of standstill, the system exhibits outburst bimodality, with long outbursts being more prominent. We conclude that the Balmer emission lines in AY~Psc are formed by the combination of radiation from the irradiated surface of the secondary, from the outflow zone, and from winds originating in the bright spot and the disk's inner part.