Том 34, № 2 (2018)

The results of the analysis of the full Stokes profiles of the photospheric lines Fe I λ 630.15 nm and Fe I λ 630.25 nm in a region of chromospheric dual flows appearance in the vicinity of a small pore are presented. The analysis is based on the spectropolarimetric observations of the active region NOAA 11024 with the THEMIS French–Italian telescope (Tenerife Island, Spain). The temporal variations in the high-resolution Stokes parameters I, Q, U, and V were considered for each pixel. It was found that the dual chromospheric flows appeared in the region of the abnormal Stokes profiles of the photospheric lines. Most of the Stokes profiles Q, U, and V have a complex shape and vary greatly from pixel to pixel, which indicates strong inhomogeneities in the structure of the magnetic field in that region. The amplitude and shape of the Stokes profiles were rapidly changing during the observations. A change in the polarity of the photospheric magnetic field took place during the observations in the region of a bright chromospheric point. The evidence of the emergence of a new small-scale magnetic flux of the opposite polarity is obtained; this could lead to magnetic reconnections, appearance of dual chromospheric flows, and occurrence of a microflare.

The results of the observations of the active region (facula) near the center of the solar disk obtained with the German Vacuum Tower Telescope (VTT; Tenerife, Spain), are discussed. We have determined that the decrease in the contrast (brightness) of the facula with the magnetic field increasing from 130 to 160 mT is due to the fact that the V_V phase shift of waves in this range of magnetic field densities is close to zero (Φ_VV ≈ 0), i.e., the wave becomes stationary and does not transfer energy from the photosphere to the chromosphere. The sound waves that propagate from the chromosphere towards the photosphere significantly affect the temperature characteristics of turbulent vortices at the level of formation of the continuous spectrum. In particular, the contrast of granules under the influence of these waves can increase by 25%.

The altitude dependences of the aerosol and gas scattering components of the effective optical depth in the latitudinal belts of Saturn’s Northern Hemisphere have been obtained from the reflectance spectra in the methane absorption bands at λ = 727 and 619 nm measured in 2015. Zonal characteristics of the vertical structure of the cloud cover of Saturn have been estimated. In the latitudinal belts, the aerosol, the relative concentration of which monotonically decreases with depth in the atmosphere, was found, and no signs of substantial cloud clusterings and rarefactions were observed. The largest and smallest aerosol amounts were determined at the latitudes of 49° N and 80° N, respectively. The altitude levels where the sizes of aerosol particles or their nature may change were revealed. We failed to determine the atmospheric level where the relative concentration of aerosol particles is largest; however, the character of the obtained dependences suggests that such a level is probably in the higher layers of the atmosphere of the giant planet.

A documentary and biographical study is presented of the life and scientific work of Boris Semeykin, an astronomer and planetologist from Kharkiv, Ukraine, who died tragically in NKVD torture chambers in the 1930s.

Incorrect expressions are shown for the Doppler width of spectral lines that occurred in some literature sources that results in different estimates of the corresponding nonthermal velocities. By way of example, it is shown that the values of the nonthermal velocities obtained by Patsouracos and Klimchuk (Astrophys. J., 2006, vol. 647, p. 1452) are overestimated by 30–40% as compared to the true values.