Geothermal fields of Hengill Volcano,Iceland

This paper provides a review of geological, geophysical, and geochemical studies for three geothermal zones of Hengill Volcano, Iceland: Nesjavellir, Hellisheidi, and Hveragerdi. We discuss the relationships between global tectonics and high-temperature geothermal systems in Iceland. The bulk of this review is devoted to studies of the physical, geochemical, and mineralogic parameters for the three areas. A separate discussion concerns surface phenomena, as well as the origin of thermal water. This review covers studies of the main aquifer complexes: Miocene/Lower Pliocene plateau basalts, Upper Pliocene/Pleistocene lavas and volcanoclastics involving tillite horizons, an aquifer complex of Holocene lava sheets as thick as 1 km, and an aquifer complex of Upper Pleistocene/Holocene alluvial eolian deposits and formations of bottom moraines. We consider a conceptual model of geothermal reservoirs characteristic for the Hengill geothermal fields.     

Models of deep electrical conductivity obtained from data on global magnetic variational sounding

An analysis of published papers containing magnetovariation sounding data (MVS) is carried out. A catalogue of the most trustworthy MVS parameters' values covering periods from 6 hours up to 11 years is compiled. With the help of averaged data of the magnetovariation sounding a planetary geoelectric profile is constructed meeting the requirements of up-to-date understanding of the physical processes in the Earth.     

Photometry of the intermediate polar 1RXS J062518.2+733433: Characteristics of its periodic brightness variations

We present the results of our photometry of the recently discovered intermediate polar 1RXS J062518.2+733433. The observations were made using the 70 cm telescope of the Astronomical Observatory of the Ural State University with a multichannel photometer, and were carried out during 13 nights in March–May 2004. Our analysis reveals brightness variations with periods of 19.788 ± 0.003 min, corresponding to the rotational period of the white dwarf, 21.273 ± 0.003 min, corresponding to the orbital sideband, and 283.3 ± 0.5 min, which is the orbital period. The variations with the white dwarf’s rotational period show a stable amplitude and a quasi-sinusoidal pulse shape persistent over a long time. In contrast, the orbital-sideband variations have an unstable amplitude and a significantly nonsinusoidal pulse shape that varies with time. Variations of the amplitude and pulse shape of the orbital-sideband variations can be related to structural changes of the accretion disk surrounding the white dwarf.     

Fractionation of Colloidal Matter of Stratal Waters during Deep Burial of Radioactive Wastes

The paper presents ultrafiltration and microscopic study of colloidal matter from radioactive waste disposal site at the Siberian Chemical Plant. It is established that most part of actinides (55–90%) are mainly bonded to colloidal particles, whereas only 20% natural uranium are bonded to >5–µm particles at the background site. In general, the retention of transuranium elements (TUE) from contaminated waters by membranes with pore size from 200 to 5 nm increases with increase of anthropogenic uranium content in water     

Sea Ice Leads Detection Using SARAL/AltiKa Altimeter

Sea ice leads play an essential role in ocean-ice-atmosphere exchange, in ocean circulation, geochemistry, and in ice dynamics. Their precise detection is crucial for altimetric estimations of sea ice thickness and volume. This study evaluates the performance of the SARAL/AltiKa (Satellite with ARgos and ALtiKa) altimeter to detect leads and to monitor their spatio-temporal dynamics. We show that a pulse peakiness parameter (PP) used to detect leads by Envisat RA-2 and ERS-1,-2 altimeters is not suitable because of saturation of AltiKa return echoes over the leads. The signal saturation results in loss of 6–10% of PP data over sea ice. We propose a different parameter—maximal power of waveform—and define the threshold to discriminate the leads. Our algorithm can be applied from December until May. It detects well the leads of small and medium size from 200 m to 3–4 km. So the combination of the high-resolution altimetric estimates with low-resolution thermal infra-red or radiometric lead fraction products could enhance the capability of remote sensing to monitor sea ice fracturing.     

Study of Lake Baikal Ice Cover from Radar Altimetry and In–Situ Observations

Comparison of ENVISAT and SARAL missions data shows that AltiKa can be successfully used for ice discrimination methodology and extension of ice conditions time series. Due to shorter wavelength and large bandwidth (480 MHz) which leads to a higher sensitivity to different surface conditions, AltiKa shows more clearly the separation between open water and various ice types. We observe significant decrease of backscatter (25–30 dB) in late spring for both ENVISAT and SARAL and discuss it in the context of ice metamorphism. There is a clear need to continue and expand our dedicated field studies of lake Baikal ice cover to better assess influence of ice structure on altimetric signal.     

The eclipsing variable CM Dra: Surface activity and orbital elements

A long series of observations of the low-mass eclipsing system CM Dra (M ₁, M _⊙<0.25M _⊙, dM4.5e, V=12.9^m, P _orb=1.27^d) was obtained in 1996–1997 as part of the international TEP (Search for Transits of Extrasolar Planets) project. The observations were obtained on the 70-cm telescope of the Astronomical Observatory of Ural State University with an automatic two-star photometer. The total duration of the data series was 155 h. We construct and analyze a master light curve, including calculation of the photometric and absolute orbital elements. Evidence for surface activity was detected. The light curve of CM Dra outside eclipses shows low-amplitude (0.024^m) brightness variations, suggesting the presence of a starspot on one of the components. The amplitude of these variations stayed the same over 20 years, but the phase of the brightness maximum shifted by one-third of the orbital period, possibly reflecting changes in the longitude or asymmetry of a single large polar spot. We detected four flares whose energies were factors of several hundred higher than those of solar flares. The derived flare rate agrees with data for CM Dra in the literature but is much lower than is typical for Population I stars in our Galaxy.