More than 36 yr have passed since the discovery of the infrared excess from circumstellar dust orbiting the white dwarf G29-38, which at 17.5 pc it is the nearest and brightest of its class. The precise morphology of the orbiting dust remains only marginally constrained by existing data, subject to model-dependent inferences, and thus fundamental questions of its dynamical origin and evolution persist. This study presents a means to constrain the geometric distribution of the emitting dust using stellar pulsations measured at optical wavelengths as a variable illumination source of the dust, which reradiates primarily in the infrared. By combining optical photometry from the Whole Earth Telescope with 0.7–2.5 μm spectroscopy obtained with SpeX at NASA’s Infrared Telescope Facility, we detect luminosity variations at all observed wavelengths, with variations at most wavelengths corresponding to the behavior of the pulsating stellar photosphere, but toward the longest wavelengths the light curves probe the corresponding time variability of the circumstellar dust. In addition to developing methodology, we find the pulsation amplitudes decrease with increasing wavelength for principal pulsation modes, yet increase beyond ≈2 μm for nonlinear combination frequencies. We interpret these results as combination modes derived from the principal modes of identical ℓ values and discuss the implications for the morphology of the warm dust. We also draw attention to some discrepancies between our findings and theoretical expectations for the results of the nonlinearity imposed by the surface convection zone on mode–mode interactions and on the behavior of the first harmonic of the highest-amplitude pulsation mode.

We present the results of the analysis of spectral observations taken a few minutes before, at the time, and in the first minutes after the impact of the DART probe on the asteroid Dimorphos. Our analysis showed signs of Na i, Li i, and K i alkali metal emissions appearing at the time of the impact and for several minutes after it.

We present the conceptual framework of the Astronomical Hub (AstroHub), a unified platform combining various optical instruments at a single observatory. Its major approach lies in arranging conditions for research groups to install telescopes and equipment and participate in joint projects. AstroHub is planned to integrate Virtual Observatory (VO) tools, FAIR data principles, and a telescope network to create a powerful and attractive ecosystem for both robust near-Earth object (NEO) monitoring and diverse deep space research. We provide an overview of the AstroHub development directions in the case study of the Assy-Turgen Observatory.

The results of observations of the object Th4-4 in 1970–2024 showed that during this period the object went through several stages, when its characteristics corresponded to different classes of objects: Be star, symbiotic star and planetary nebula. Currently, the object appears to be a low-excitation planetary nebula.

Галактики с активными ядрами, и в частности сейфертовские галактики демонстрируют спектральную и фотометрическую переменность на временных интервалах от нескольких часов до нескольких лет. Источниками переменности могут быть газово-пылевые облака в окрестностях черной дыры, и отдельные звезды, периодически проходящие через аккреционный диск. Возможной причиной переменности может быть двойственная природа центральной черной дыры. В Астрофизическом институте им. Фесенкова спектральные наблюдения сейфертовских галактик проводятся на протяжении 50 лет. Для наблюдений используются телескоп АЗТ-8 и 1- метровые рефлекторы, расположенные на высокогорной Обсерватории ТШАО. В данной статье приводятся результаты спектральных и фотометрических исследований галактики NGC 5548. Анализ ее кривой блеска свидетельствует о том, что имеют место практически постоянные колебания значений B V R величин в пределах ~ 0m.3. Кроме того, прослеживается тенденция плавного изменения среднего уровня блеска, в частности, в сторону его повышения. Фрагменты спектрограмм, полученных в разные годы, содержат эмиссионные линии Hα и [NII] и дают возможность оценить изменения уровня континуума, формы профилей и потоков излучения в широкой компоненте водородной линии. Так, наблюдалось значительное увеличение ширины эмиссионных крыльев линии Hα. Кроме того, в 2004 г на коротковолновом крыле Hα появилась дополнительная эмиссионная деталь, которая просуществовала до 2018г. Лучевая скорость эмиссии менялась со временем, вызывая ее видимое смещение вдоль профиля основной линии. Подобные дополнительные эмиссии с переменными лучевыми скоростями могут создаваться эмиссионными объектами, движущимися в поле тяготения центрального тела.

This paper presents the architecture of the Kazakhstani National Virtual Observatory (KazVO)—an International Virtual Observatory Alliance (IVOA) compliant node that unifies the heterogeneous observational datasets of the Fesenkov Astrophysical Institute (FAI). The architectural foundation of the system is built upon a partitioned Data Lake, a German Astrophysical Virtual Observatory (GAVO) Data Center Helper Suite (DaCHS) publishing backend, and a PostgreSQL database in which metadata for published observational products are mapped to IVOA ObsCore, while catalogs and simulation grids use dedicated relational tables. We follow Open Science principles by introducing a metadata-only showcase model based on a four-class data embargo mechanism. Machine-to-Machine services deployed via IVOA protocols are exposed through the KazVO publishing registry registered in the global Registry of Registries (RofR), enabling analysis of Kazakhstani observational assets within external clients such as Tool for OPerations on Catalogues And Tables (TOPCAT), Aladin, and PyVO. The current implementation combines operational VO publication services and targeted photometric processing with scheduled, batch-mode data ingestion, supporting access to published historical and modern observational holdings. Replication has been validated on pilot datasets, while routine deployment at the observing sites and automated reduction of modern spectroscopic streams remain under development. The architecture provides a framework for progressively integrating these components into a complete data lifecycle.