— The results of polarimetric observations of blazar S5 0716+714, carried out with the 6-meter BTA telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences, are presented. The polarized emission microvariability of blazar S5 0716+714 was observed in the R band with an initial time resolution of 3–5 seconds. Exposures were integrated at 1-minute intervals with a total observation time of several hours over two nights. Microvariability of the polarization degree with amplitude of 3–4% was detected during 7–11 minutes and flux oscillations within 9–10% during 25 minutes. A partial synchronism of the flux oscillations and the polarization degree of this blazar was found. Possible interpretations of the detected microvariability are briefly described.

The active core of the galaxy AO0235+164 is monitored in the optical and radio bands at millimeter wavelengths. Using the multifrequency data obtained in gamma, optical and radio bands, the characteristics of its radiation in the active phase of 2015–2016 are studied. The cross-correlation method was used to determine the delays of the 2015 flare that took place in AO0235+164 in different bands. The analysis made it possible to establish that, in comparison with the previous flare phenomena, changes in the orientation of the emissions (jets) have occurred. The angle θ between the jets and the direction towards the observer has decreased by a factor of \(\sqrt 2 \), resulting in a twofold increase in the γ-factor. The obtained value γ ≈ 40 is the most extreme value ever observed in AO0235+164 over the entire span of observations.

Data from long-term multi-frequency monitoring are used to analyze variations in the flux density of the active galactic nucleus S4 0954+658. These data were obtained at the CrimeanAstrophysical Observatory, the Metsähovi Radio Observatory of Aalto University, the University of Michigan Radio Astronomy Observatory, the Cavendish Laboratory of Cambridge University, the Special Astrophysical Observatory, and the National Institute of Astrophysics, Optics, and Electronics; 0.1–300-GeV data from the Fermi space gamma-ray observatory were also used. Radio data at 4.8, 8, 14.5, 15, 22.2, and 36.8 GHz are considered together with optical and near-infrared data in the R, J, H, and K filters.

Long-term, multi-frequency optical and radio monitoring data for the Active Galactic Nuclei (AGNs) AO 0235+164 and S5 0716+714 are used to derive the characteristics of their radiation on time scales from hours to decades. Structure-function and harmonic analyses are carried out to determine the parameters of the radiation of these AGNs and explain their physical characteristics. Periodic components that could be associated with the motion of companions along an orbit in a close binary system of two supermassive black holes are identified. Both of the analysis methods used yield consistent results for the harmonic components. The results obtained are consistent with the idea that we are viewing systems of two supermassive black holes in a stage of their evolution that is close to coalescence. The substantial energy release of these AGNs can be interpreted as dynamical losses arising during the motion of the companion about the common center of gravity in a dense accreting medium, sometimes crossing through the accretion disk.

The Russian Academy of Sciences and Federal Space Agency, together with the participation of many international organizations, worked toward the launch of the RadioAstron orbiting space observatory with its onboard 10-m reflector radio telescope from the Baikonur cosmodrome on July 18, 2011. Together with some of the largest ground-based radio telescopes and a set of stations for tracking, collecting, and reducing the data obtained, this space radio telescope forms a multi-antenna ground-space radio interferometer with extremely long baselines, making it possible for the first time to study various objects in the Universe with angular resolutions a million times better than is possible with the human eye. The project is targeted at systematic studies of compact radio-emitting sources and their dynamics. Objects to be studied include supermassive black holes, accretion disks, and relativistic jets in active galactic nuclei, stellar-mass black holes, neutron stars and hypothetical quark stars, regions of formation of stars and planetary systems in our and other galaxies, interplanetary and interstellar plasma, and the gravitational field of the Earth. The results of ground-based and inflight tests of the space radio telescope carried out in both autonomous and ground-space interferometric regimes are reported. The derived characteristics are in agreement with the main requirements of the project. The astrophysical science program has begun.

We present the results of long-term radio and optical monitoring of two radio-loud quasars. The aim of the work was to study the objects’ variability on various time scales and search for correlations between the radio and optical emission. The monitoring was performed in 2002–2010. The radio observations were carried out using the 22-m telescope of the Crimean AstrophysicalObservatory, 26-m telescope of the University of Michigan Radio Astronomy Observatory, and 14-m telescope of the Metsahovi Radio Observatory at 4.8, 8.0, 14.5, 22.2, and 36.8 GHz. The optical observations were obtained in the B, V,R bands using the Zeiss-1000 telescope of the Special Astrophysical Observatory with a CCD photometer. Light curves of the quasars 4C 38.41 (1633+382) and S5 0716+714 are presented. Radio flares of 4C 38.41 with amplitudes of 0.5–1.0 Jy at 4.8 and 8 GHz and 1–3 Jy at 22.2 and 36.8 GHz were detected on time scales of about 100 days. The amplitude of the optical brightness variations varied between 0.5 m and 1.5 m over about 200 days. The amplitudes of the flux variations for S5 0716+714 for the period of two months were 0.5–1.6 Jy at centimeter and 1–7 Jy at millimeter wavelengths. The amplitudes of flares in the optical reached 2 m in the B and V filters and 2.5 m in the R filter, on time scales of 200 days. The color indices of these objects did not change during the period covered by observations, i.e., the objects did not become bluer when they brightened. The detected delays between the variations atmillimeter and centimeter wavelengths are several days, which is within the interval between observations during the long-term monitoring. The absence of a distinct correlation between the optical and radio brightness variations was probably due to the presence of substantial time delays between the phenomena occurring in these different wavelength ranges.

We present the results of multi-years optical and radio monitoring of radio-loud quasars 0716+714 and 1633+382, aimed at searching the flux variations and possible correlation at different wave bands. Our radio observations were performed with a 22-m radio telescope of the Crimean Astrophysical Observatory, 14-m radio telescope of the Metsahovi Radio Observatory and 26-m telescope of the Michigan Radio Astronomy Observatory at 4.8, 8.0, 14.5, 22.2 and 36.8 GHz. The optical observations were performed with a Zeiss-1000 reflector of the Special Astrophysical Observatory in the B, V, R filters.

We present coordinated synchronous observations of Active Galactic Nuclei in the radio and optical, aimed at searching for fast (intraday) flux variations and possible correlations in the flux variations in different wavebands. Our observations were performed with the 22-m radio telescope of the Crimean Astrophysical Observatory at 22.2 and 36.8 GHz and the Zeiss-1000 reflector of the Special Astrophysical Observatory in the R filter, using a CCD photometer. We performed five observing runs of 7–10 nights each in 2004–2006. We obtained radio and optical light curves for the variable extragalactic radio sources DA 55, 1633+382, 2134+004, 2145+067, and 2251+158. We detected short-duration flares of DA 55 and 2134+004 in the R band with variations of 0.2 m within about 15 minutes. The other sources did not show any considerable flux variations. The radio flux variations of DA 55 and 2134+004 reached 1.5 Jy in about 15 minutes, and those of 2145+067 reached 2 Jy in 2 hours. We observed chaotic flux variations in 2251+158, by 2–2.5 Jy in half an hour. We detected no correlation between the radiation in the optical and radio.

S (alphabetically ordered) PECULIARITIES OF QPOS OF MICROWAVE EMISSION OF THE FLARING SOLAR ACTIVE REGIONS V.E. Abramov-Maximov, G.B. Gelfreikh Central Astronomical Observatory at Pulkovo, Saint-Petersburg, Russia gbg@saoran.spb.su Quasi-periodic oscillations of solar coronal structures are effectively registered in particular at microwave waves. The physical nature of periodical processes in the corona is clearly connected with plasma structures of the solar atmosphere. On the other hand, the modern conception is that processes leading to eruption of energy in solar flares are results of energy accumulation in the corona or chromosphere produced by some reconstruction of plasma structures. In spite of developments of the modern observations predominantly using cosmic techniques, we are still far from a satisfactory observational understanding of the above processes. The QPOs of solar active regions were found decades ago and their connections with the flares were detected. Nevertheless, the physical nature and possible forecasting applications are still far from a reasonable level of knowledge. New development of microwave instruments with a high spatial resolution and regular observations (NoRH, RATAN–600, SSRT at Badary) opened a new era in such studies. Oscillations with periods from few minutes to hours were investigated and their time variations were specially analysed. So, we may conclude that investigations of these parameters for ARs with different levels of flare activity, time variations including, may lead to a better understanding of the physics of the problem. Some preliminary results of such studies are presented in this report, based on an analysis of the Nobeyama radio maps of the Sun with the 10 sec averaging and covering periods of hours of observations (dates 11 Sep 2001, 07 Oct 2002, including), and comparing these with spectral parameters of the regions obtained with RATAN–600. This study was partially supported by the Program of the Presidium or the Russian Academy of Sciences. A LINK BETWEEN VARIABLE OPTICAL CONTINUUM AND RADIO EMISSION OF A COMPACT JET IN THE RADIO-LOUD SEYFERT GALAXY 3C390.3 T.G. Arshakian, A.P. Lobanov, V.H. Chavushyan , A.I. Shapovalova, J.A. Zensus , N.G. Bochkarev, A.N. Burenkov Max-Planck-Institut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germany, Instituto Nacional de Astrof́ısica, Optica y Electrónica, Apartado Postal 51. C.P. 72000. Puebla, Pue., México, Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia, Sternberg Astronomical Institute, University of Moscow, Universitetskij Prospect 13, Moscow 119899, Russia tigar@mpifr-bonn.mpg.de We present an observational evidence for a relation between variability of radio emission of the compact jet, nucleus optical continuum emission and ejections of new jet components