<Emphasis Type="Italic">BVRI</Emphasis> CCD-photometry of comparison stars in the neighborhoods of galaxies with active nuclei. III     

V. T. Doroshenko  S. G. Sergeev  Yu. S. Efimov  S. Nazarov  V. I. Pronik  E. A. Sergeeva  G. A. Sivtsov 《Astrophysics》2007,50(1):40-53

Observations with a matrix photometer are reported. The stellar magnitudes in the BVRcIc bands are estimated for 80 comparison stars in the neighborhoods of 10 galaxies with active nuclei: 2 Seyfert galaxies, 4 quasars, and 4 BL Lac objects. The stellar magnitudes of the observed stars range from 11 to 19^m.5. For stars with magnitudes of 14–15^m the typical photometric errors are 0^m.011, 0^m.008, 0^m.006, and 0^m.007 in the B, V, R, and I bands, respectively. The BVRI magnitudes for most of these stars were not known previously. 14′ × 14′ finding charts for these stars are included. These results can be used for differential BVRI photometry of active galactic nuclei. __________ Translated from Astrofizika, Vol. 50, No. 1, pp. 57–72 (February 2007).  相似文献   

Study of interaction of ELF–ULF range (0.1–200 Hz) electromagnetic waves with the earth’s crust and the ionosphere in the field of industrial power transmission lines (FENICS experiment)     

A. A. Zhamaletdinov  A. N. Shevtsov  E. P. Velikhov  A. A. Skorokhodov  V. E. Kolesnikov  T. G. Korotkova  P. A. Ryazantsev  B. V. Efimov  V. V. Kolobov  M. B. Barannik  P. I. Prokopchuk  V. N. Selivanov  Yu. A. Kopytenko  E. A. Kopytenko  V. S. Ismagilov  M. S. Petrishchev  P. A. Sergushin  P. E. Tereshchenko  B. V. Samsonov  M. A. Birulya  M. Yu. Smirnov  T. Korja  Yu. M. Yampolski  A. V. Koloskov  N. A. Baru  S. V. Poljakov  A. V. Shchennikov  G. I. Druzhin  W. Jozwiak  J. Reda  Yu. G. Shchors 《Izvestiya Atmospheric and Oceanic Physics》2015,51(8):826-857

  相似文献   

Properties of solar wind turbulence from radio occultation experiments with the NOZOMI spacecraft     

A. I. Efimov  T. Imamura  K. -I. Oyama  K. Noguchi  L. N. Samoznaev  A. S. Nabatov  M. K. Bird  I. V. Chashei 《Astronomy Reports》2010,54(11):1032-1041

Radio-sounding experiments using signals from the Japanese NOZOMI spacecraft to probe the circum solar plasma were performed from December 2000 through January 2001. They can be used to obtain information about the properties of the solar wind plasma in the region where it is accelerated at heliocentric distances of 12.8–36.9R _s (where R _s is the radius of the Sun). Measurements of the intensity and frequency of the received signals were carried out with high time resolution (～0.05 s for the frequency and ～0.0064 s for the intensity), making it possible to investigate the anisotropy of inhomogeneities and the spatial spectrum of the turbulence of the circum solar plasma. Analysis of these radio-sounding data has shown that the scintillation index and intensity of the frequency fluctuations decrease approximately according to a power law with increasing distance of the line of sight from the Sun. Measurements of the amplitude fluctuations and estimates of the solar wind velocity derived from spatially separated observations indicate the presence of small-scale inhomogeneities with sizes of the order of 50 km at heliocentric distances less than 25R _s , which are elongated in the radial direction with anisotropy coefficients from 2.3 to 3.0. The inhomogeneities at heliocentric distances exceeding 30R _s become close to isotropic.  相似文献   

Photopolarimetry of 3C 66A in 2003     

Yu. S. Efimov  N. V. Primak 《Astrophysics》2006,49(1):36-53

The BL Lac-type object 3C 66A was observed at the Crimean Astrophysical Observatory during the international project OJ-94. Observations were made over 10 nights from February through December 2003 at the Cassegrain focus of the 125-cm AZT-11 telescope with a photopolarimeter capable of simultaneous measurements in the UBVRI bands. In the course of our measurements the brightness of the object increased by more than 1 magnitude in all these bands. Its color indices varied and the degree of polarization decreased from ∼16% in February to ∼3% at the end of our observations. In December 2003 a rapid change in the position angle from 15° to 40° was noticed. The spectral energy distribution F_n is well described by a power law with a spectral index a (F_ν ∝ ν ^−α . The increase in brightness was accompanied by a reduction in the spectral index. The most probable mechanism for the observed changes in the brightness, degree of polarization, and spectral index may be a decrease in the magnetic field strength or a change in its configuration owing to a increase in the chaotic component of the field. __________ Translated from Astrofizika, Vol. 49, No. 1, pp. 41–59 (February 2006).  相似文献   

Polarization and brightness opposition effects for the E-type Asteroid 64 Angelina     

Vera K. Rosenbush  Nikolai N. Kiselev  Klaus Jockers  Yuriy S. Efimov 《Icarus》2005,178(1):222-234

We present new polarimetric and photometric observations of the high-albedo Asteroid 64 Angelina in the UBVRI wavebands at phase angles ranging from 0.43° to 13.02° during oppositions in 1995, 1999, and 2000/2001. The polarization opposition effect has been observed in the form of a sharp peak of negative polarization with amplitude of about −0.4% centered at αmin≈1.8°, which is superimposed on the regular negative polarization branch. The amplitude of the polarization opposition effect appears to be apparition-dependent. Our photometric data confirm the early detected by Harris et al. [1989. Phase relations of high-albedo asteroids: The unusual opposition brightening of 44 Nysa and 64 Angelina. Icarus 81, 365-374] of a very strong and unusually narrow opposition spike, i.e., brightness opposition effect, for Angelina. Thus, 64 Angelina is the first asteroid for which both the polarization opposition effect and the brightness opposition effect have been detected. We observed that the polarization opposition effect as well as the regular negative polarization branch depends on the wavelength of scattered light, but in different manners. In addition, the colors B-V and V-R show little phase-angle dependence, while the color U-B increases with increasing phase angle, thus indicating that the amplitude of the brightness opposition effect is larger in the U band and almost the same in the B, V, and R bands. It appears that all colors indices begin to increase with decreasing phase angle to zero. The composite lightcurve computed with a period of 8.752 h has amplitude of 0.13 magnitude.  相似文献   

Optical and infrared observations of SU Tau     

V. T. Doroshenko  Yu. S. Efimov  A. É. Rozenbush  V. Yu. Terebizh  V. I. Shenavrin 《Astrophysics》1978,14(1):1-7

  相似文献   

Estimation of water balance components in the Black Sea     

V. V. Efimov  V. N. Belokopytov  A. E. Anisimov 《Russian Meteorology and Hydrology》2012,37(11-12):769-774

Presented are the estimates of precipitation amount and evaporation for the Black Sea basin based on the data of numerical regional reanalysis. The spatial distribution of considered variables is compared with the results obtained before using the method of extrapolation of measurements at the coastal meteorological stations. The computed water balance components of the Black Sea compared with the available literature data are used for obtaining the estimate of the mean water discharge in the Bosphorus.  相似文献   

Method of determination of heat,moisture, and momentum fluxes in the stratified surface layer     

A. E. Efimov 《Russian Meteorology and Hydrology》2010,35(9):641-649

The method is proposed to determine the main fluxes characterizing the surface stratified layer of plants’ habitat using the Monin-Obukhov length scale. The gradient measurements of the profiles of wind flow speed, relative humidity, and air temperature are carried out. The experimental data are obtained using the mobile automated system. The wavelet analysis of time series is carried out. The nonlinear equation system is numerically solved to determine the heat, moisture, and momentum fluxes which can be used for the optimum control of the plant moisture supply in the agricultural field.  相似文献   

Solar Wind Magnetic Field Turbulence over the Solar Activity Cycle Inferred from Coronal Sounding Experiments with Helios Linear-Polarized Signals     

Efimov  A. I.  Lukanina  L. A.  Chashei  I. V.  Bird  M. K.  Pätzold  M. 《Astronomy Reports》2019,63(3):174-181

Results of experiments on polarized radio sounding of the outer solar corona using the Helios spacecraft from 1975 to 1984 are presented. The characteristic parameters of the temporal spectra of fluctuations in the Faraday rotation of the plane of polarization for heliocentric distances from 3.5 to 5.5 solar radii are obtained. The absolute level of these fluctuations and, consequently, the level of fluctuations of the magnetic field, is almost independent of the solar activity. It is well known that the global structure of the solar wind varies with the solar cycle such that there is slow solar wind at low latitudes and fast solar wind at high latitudes during solar minima. In contrast, a slow solar wind dominates at all latitudes during solar maxima. One explanation for the invariance of the fluctuations observed by sounding the circumsolar plasma is that the mean magnetohydrodynamic turbulence of the low-latitude, slow solar wind depends weakly on the phase of the solar cycle.

  相似文献   

Climate change projections in Russian regions: The detailing in physical and probability spaces     

V. M. Kattsov  I. M. Shkolnik  S. V. Efimov 《Russian Meteorology and Hydrology》2017,42(7):452-460

  相似文献