Spectral and photometric observations are a unique tool for studying the Resident Space Objects (RSO). Spectral observations are of particular value. They are precious sources of information in identifying and classifying RSO by their spectral features and studying the variation of these features caused by the influence of space weathering. The paper we present shows the results of the geostationary satellite (GEO) reflection spectra analysis. We use spectral observations to analyze reflective spectra and relevant parameters to develop the methodology of satellite identification. Spectral observations were obtained on the spectrograph mounted on a 1.5-meter telescope AZT-20 of the Assy-Turgen Observatory. Photometric characteristics derived from spectral observations show signs of dependence on the platform of a satellite and its service life in orbit. Comparison of observed and model reflective spectra indicates the possibility of identifying the satellite shape and its composite materials. The results of the work will be of interest for the study of space weathering on materials, will allow us to better understand the situation in GEO orbits, and refine the methods for near-miss events prediction, taking into account the geometry of objects and the properties of their surfaces.

Фотометрические и спектральные наблюдения 11-ти звезд Вольфа-Райе WN последовательности выполнялись в АФИФ в 2021-2022гг. На основе проведенных наблюдений получены оценки блеска объектов в фильтрах BVRc и абсолютные потоки излучения в эмиссионных линиях. Изменения блеска в пределах 0m.1 - 0m.15 зарегистрированы в звездах WR 1, WR 120, WR 151, WR 152. Изменения эмиссионных потоков обнаружены в спектрах нескольких объектов: WR 120, WR 128, WR 145. Photometric and spectral observations of 11 W-R stars were carried out at the FAI in 2021-2022. The studied group included representatives of the WN, WC, and WO sequences. Based on the observations estimates of the brightness of objects in the B V Rc filters and absolute fluxes of radiation in the emission lines were obtained. Changes in brightness within 0m.1 - 0m.15 were detected in the stars WR 1, WR 120, WR 151, and WR 152. Changes in the emission fluxes were detected in the spectra of several objects: WR 120, WR 128, and WR 145.

We report on the results of the analysis of spectral observations of the asteroid Didymos at the time of impact of the DART mission probe, obtained a few minutes before, directly at the moment, and within a few minutes after the spacecraft hit the surface of the Dimorphos. We found evidence of alkali metal emissions that appeared at the moment and continued for several minutes after the impact. The observation evidence of the appearance of Na, Li and K atoms as a result of the impact of the DART probe on the Dimorphos in a relative amount close to the abundance of these elements in the Solar System are reliably established. We conclude that the main contribution to alkaline emissions is atoms bound to the dust cloud ejected during the impact. This dust cloud is a steady source of alkaline metal atoms. We did not detect the presence of alkaline mater not bound to the dust cloud and moved independently.

Abstract 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.

На базе многолетних наблюдений представлены результаты спектральных исследований пятнадцати сейфертовских галактик в красной области длин волн. В данном диапазоне расположены линии водорода Hα, [NII], [OI] и [SII]. Представлены данные об абсолютных потоках излучения в эмиссионных линиях и в непрерывном спектре на длине волны λ= 6400Å . Для того, чтобы объективно сравнивать исследуемые галактики друг с другом, получены значения их светимостей в абсолютных единицах, рассчитанные с учетом расстояний до этих объектов. The results of spectral studies of fifteen Seyfert galaxies in the red wavelength region based on the long-term observations, are presented. Some emission lines Hα , [NII], [OI] и [SII] are located in this wavelength range. Data on the absolute fluxes of radiation in emission lines and in continuum at the wavelength of λ= 6400Å are presented. In order to objectively compare the studied galaxies with each other, the values of their luminosities in absolute units were calculated, taking into account the distances to these objects.

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.

Massive stars of spectral class O, leaving the Main Sequence (MS), are capable to lose their hydrogen envelopes. The remaining core begins to shrink, starting a sequence of nuclear reactions, the products of which are heavy elements C, N and O. The WR stage is an intermediate stage in the evolutionary path of massive stars to their final state: a neutron star or a black hole. WR stars play an important role in evolution: firstly, they enrich the interstellar medium with heavy elements, and secondly, they are considered as progenitors of supernovae and as possible sources of X-ray flares. This article presents preliminary results of observations of the group of WR stars. The spectra were obtained for three WC-type stars: WR 4, WR5, and WR154, and two WN-type stars: WR2 and WR3. On the basis of observational data, the absolute fluxes in the emission lines were obtained, the equivalent widths and half-widths of their profiles were determined. Comparison of our results for WR4, obtained over 2 nights, shows that in January 2021 the absolute fluxes in the emission lines decreased by 20% compared to the data of December 2020. Comparison with the data obtained in 1983-1984 did not reveal serious discrepancies in the results for WR4, but our values of the equivalent widths for WR5 turned out to be half as much. This may be due to an increase in the level of the continuum or due to decrease of the emission lines fluxes. Photometric observations were carried out for four WR stars, with WR4 and WR5 observed over three nights. Comparison with the earlier data shows an increase in the brightness of objects over the past 20 years: by 0m.2 - 0m.3 for WR2 and WR5 and by 0m.6 -0m. 8 for WR4 and WR3. So, at this stage, we have established the photometric variability of 4 WR stars: WR2, WR3, WR4, and WR5, as well as the spectral variability of at least two objects: WR4 and WR5.

Бас редактор: МҰТАНОВ Ғалымқайыр Мұтанұлы, техника ғылымдарының докторы, профессор, ҚР ҰҒА академигі, ҚР БҒМ ҒК «Ақпараттық және есептеу технологиялары институты» бас директорының м.а.(Алматы, Қазақстан) Н=5 Редакция алқасы: ҚАЛИМОЛДАЕВ Мақсат Нұрәділұлы (бас редактордың орынбасары), физика-математика ғылымдарының докторы, профессор, ҚР ҰҒА академигі, ҚР БҒМ ҒК «Ақпараттық және есептеу технологиялары институты» бас директорының кеңесшісі, зертхана меңгерушісі (Алматы, Қазақстан) Н=7 БАЙГУНЧЕКОВ Жұмаділ Жаңабайұлы (бас редактордың орынбасары), техника ғылымдарының докторы, профессор, ҚР ҰҒА академигі, Кибернетика және ақпараттық технологиялар институты, Сатпаев университетінің Қолданбалы механика және инженерлік графика кафедрасы, (Алматы, Қазақстан) Н=3 ВОЙЧИК Вальдемар, техника ғылымдарының докторы (физика), Люблин технологиялық университетінің профессоры (Люблин, Польша) H=23 БОШКАЕВ Қуантай Авғазыұлы, Ph.D. Теориялық және ядролық физика кафедрасының доценті, әл-Фараби атындағы Қазақ ұлттық университеті (Алматы

The objects IRAS 06053+1837 and IRAS 22023+5249, are considered as planetary nebula candidates. They have far infrared colors, which are typical to planetary nebulae. Their rather cool stars are surronded by envelopes, in which some low-excitation emission lines are formed. BV photometry of the object IRAS 22023+5249, carried out in 2017-2020, resulted the scatter of B and V values within 0(m).25 and 0(m).10 respectively. Moreover a tendency of the gradual increasing of brightness is revealed. Absolute fluxes and equivalent widths of the H beta, H alpha, [NII], 6548, 6583A and HeI, 6678A emission lines in the spectrum of IRAS 22023+5249 are determined. The strengthening of the emission lines is confirmed. Most likely increasing of an effective temperrature of the star is responsible for observable variations. As a whole spectral and photometric characteristics of the object IRAS 22023+5249 correspond to its status as a low-excitation planetary nebula. For the object IRAS 06053+1837observable data are obtained in 2014-2019. Much larger the scatter of B V R values is observed: 0(m).50, 0(m).15 and 0(m).30 respectively. The only HI emission lines are presented in its spectrum. Asymmetrical profiles of lines have broad wings on the short wavelength side. The evolutionary status of the object is not defined; its characteristics, are more similar to those of the young AeBe Herbig stars.

We present the first results of the light curve analysis of variable stars identified in Tien-Shan survey conducted on Tien-Shan Observatory (TSO) using Zeiss-1000 telescope. Here we report on 33 high amplitude variable stars among which 31 is previously uncatalogued variables. Using data from the StarHorse catalog, as well as results from the MIST project, Color-Magnitude Diagram and appropriate evolutionary tracks were constructed for each field and individual variable star, corresponding to the star's mass and metallicity. For two objects, we performed spectral observations on the Zeiss-1000 "Zapadny" telescope using a slit spectrograph. The obtained spectra were compared with synthesized spectra. The preliminary identification of variability type of each star is based on parameters of variability (amplitudes and periods) determined from periodograms analysis, evolution stage based on evolutionary track on Color-Magnitude Diagram and, for some targets, on spectral information.

This is a study of spectral and photometric observations of the binary system with an X-ray component V725 Tauri=A0535+262. It consists of a giant star HDE 245770 of spectral class O9.7 and the pulsar A0535+26 with a pulsation period of ~103 s. Active stages of this object, accompanied by “giant” X-ray outbursts, have been observed repeatedly. The last events occurred during 2009-2011. Our studies in 2017-2020 yielded the following data: over the last three years the B and V band brightness of the object has remained at a high level and began to decrease at the end of 2019. Here, beginning in 2016 a gradual increase in the radiative fluxes in the Hβ and Hα emission lines has been observed. At present the equivalent widths of these lines exceed the values recorded during the time of the gigan X-ray outburst of 2011. Previous studies have shown that a similar combination of the characteristics of this object, specifically an increase in emission line fluxes as the brightness decreases. is detected just before the onset of an active stage.

New outburst of the object BX Mon occurred in the beginning of 2019. The uniqueness of this event lies in its coincidence with the periastron passage by the hot component. This happened for the first time in the history of observations of this object. Previous epochs the moment of periastron passage corresponded to the lower part of the ascending branch of the light curve. Photometric and spectroscopic observations of BX Mon were carried out in the Fesenkov Astrophysical Institute (Republic of Kazakhstan). BVRc magnitudes, absolute fluxes and the profiles of emission lines were obtained. The maximal values B = 9.(m)7 and V = 9.(m)3, obtained in the beginning of 2019, are close to those observed during the previous outburst (2003, February). A high level of brightness was maintained until the middle of April. The absolute fluxes in the emission lines H beta and H alpha, obtained during the current outburst, turned out to be significantly weaker compared to the results, obtained in the previous periastron passages. A possible reason of the anomalous decrease of the emission line fluxes is the destruction of the accretion disk - the source of ionizing radiation.

AbstractObservations of radial velocities in the F-corona in the elongation range from 3 to 6 solar radii were carried out on July 11, 1991 (Mexico, La Paz) by means of a Fabry-Perot spectrograph. The Fraunhofer lines in the spectral region of H and K Call were used. The average velocities to the West and to the East of the Sun within 30° of the ecliptic plane are +30 km/s and -27 km/s respectively. This confirms the main results of the F-corona radial velocity observations by Shcheglov et al. (1987), Shestakova (1987) on July 31, 1981 about predominance of prograde Keplerian motion of the dust near the ecliptic plane and the effective radius of dust grains (≈0.4μm)