Aims. We report results of a quantitative colorimetric UBVRI analysis of two flare events on the red dwarf EV Lac. The photometric data were obtained in September 2004, during the multi-site synchronous monitoring from the four observatories in Ukraine, Russia, Greece, and Bulgaria. These observations confirmed the presence of small-scale high-frequency oscillations (HFO) initially detected by Rodonó (1974, A&A, 32, 337) and recently reconfirmed by the authors. Here we discuss the color characteristics of flares and HFO. Methods. Colorimetric analysis had been performed with the help of the time tracks in the UBVRI color-color diagrams from the earliest phase of flare development. Digital filtering technique was used to evaluate the time-dependent color indices. Results. As can be clearly seen in the diagrams, color indices oscillate on a time scale of seconds, far exceeding instrumental errors. Regarding the HFO, we conclude that the bulk of a flare oscillates during a major part of its lifetime between the states of hydrogen plasma opaque and transparent in the Balmer continuum. We find that at the peaks of oscillations the color tracks drift into the regions of color-color diagrams corresponding to a blackbody radiation, which provides an estimate of color temperatures from 17 000 to 22 000 K. We also find that flares cover ∼1% of the stellar disc.

A new approach for the search of microvariability and high-speed phenomena in variable stars is presented. It gives a new technology of observation and analysis of the data. Statistical photometry stands on the three pillars: the digital filtering technique, the photon counting statistics based on the Mandel equation, and the integral transforms of the light curves. This technique permits to investigate low-amplitude and rapid variability of stars.

We present a new observational campaign, DWARF, aimed at detection of circumbinary extrasolar planets using the timing www.an-journal.org

Abstract.A program of Many-sites Multi Channel simultaneous observations of flare stars by a network of telescops was initiated in 1998. The purpose of this program is to investigate the fine structure of the flares light-curve in UBVRI, depressing atmospheric and instrumental noises. In this paper we present the results of the observations on the Flare star EV Lac in the B color, which were carried out at the Stephanion observatory during the campaign of 1999. Discrete Fourier Transform analysis of the B-light curve of the largest flares reveal the presence of high frequency small amplitude oscillations with periods ranging between 6.9 sec and 20 sec in around the flare maximum phase. The oscillation amplitude ranges from 1.4 to 2.6 % of the star brightness in accordance with the results of the campaign of 1998 (Zhilyaev et al. 2000). In addition there is a tendency the higher frequencies to persist in the late phases of the flare evolution. The observations are consistent with the phenomenology of the evolution of a fast mode magneto-acoustic wave generated at the impulsive phase of the flare and traveling through the magnetic loop.

We present our follow-up observations with GRANDMA of transient sources revealed by the Zwicky Transient Facility (ZTF). Over a period of six months, all ZTF alerts were examined in real time by a dedicated science module implemented in the Fink broker, which will be used filtering of transients discovered by the Vera C. Rubin Observatory. In this article, we present three selection methods to identify kilonova candidates. Out of more than 35 million alerts, a hundred sources have passed our selection criteria. Six were then followed-up by GRANDMA (by both professional and amateur astronomers). The majority were finally classified either as asteroids or as supernovae events. We mobilized 37 telescopes, bringing together a large sample of images, taken under various conditions and quality. To complement the orphan kilonova candidates, we included three additional supernovae alerts to conduct further observations during summer 2021. We demonstrate the importance of the amateur astronomer community that contributed images for scientific analyses of new sources discovered in a magnitude range r′ = 17 − 19 mag. We based our rapid kilonova classification on the decay rate of the optical source that should exceed 0.3 mag/day. GRANDMA’s follow-up determined the fading rate within 1.5 ± 1.2 days post-discovery, without waiting for further observations from ZTF. No confirmed kilonovae were discovered during our observing campaign. This work will be continued in the coming months in the view of preparing for kilonova searches in the next gravitational-wave observing run O4.

The comparison is represented of the results of surface ozone concentration measurements in two megalopolises, Moscow and Kiev. A temporal course of ozone concentration and temperature in both cities is close by the shape and is typical of medium-polluted plain stations. In both megalopolises, two maxima are observed within the seasonal ozone concentration variability, in spring and summer, and during the day, a usual ozone concentration maximum (approximately in 2-3 hours after the local noon) and the night one being typical of big cities. An average ozone concentration and an average temperature in corresponding periods are higher in Kiev than in Moscow. Evidently, the summer maximum is associated with photochemical ozone generation processes, and the spring one, with dynamic processes of its transport in the atmosphere. In both megalopolises, the episodes are observed in the warm period under meteorological conditions being unfavorable for the pollutant scattering in the atmosphere when the ozone concentration exceeds the threshold limit value and is dangerous for health. The repeatability of such episodes is the highest one in July-August. In Kiev, such episodes are more frequent than in Moscow. An effective statistical model is constructed for both megalopolises in which the observed ozone concentration is represented in the form of regression function of temperature and relative humidity.

A review is compiled based on the results of the system of monitoring total ozone (TO) over the CIS and Baltic countries that is operated in real time at the Central Aerological Observatory (CAO). The TO monitoring system uses the data from the national M-124 filter ozonometer network operated under the methodological guidance of the Main Geophysical Observatory. The performance of the system as a whole is operationally verified against the OMI satellite (US NASA) observations. The main TO observational data are summarized for each month of the fourth quarter of 2008, for a quarter, and a year as a whole. Data on the Spring Antarctic Ozone Anomaly in 2008 are presented. Results of regular surface ozone observations in the Moscow region and in Kiev are also considered.

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