The issues of the application of operational amplifiers that are manufactured in Russia in systems for spectrometric measurements of the solar flux, which are designed for use in promising space projects, are considered. The results of experimental studies of prototypes of circuit units that perform the functions of a precision charge integrator for the formation of a video signal on the basis of a highly stable 554UD1 operational amplifier when processing signals from a linear photodetector are presented.

The first 2‐D distributions of the polarization angle and of the relative color index for the K‐corona of 29 March 2006 are presented. The distributions illustrate the efficiency of the total solar eclipse approach for high‐precision measurements of the K‐corona continuum in the range < 1.4 R⊙. Natural ground and space total solar eclipses caused by external occulting the bright solar‐disk light by the Moon or Earth group planets are discussed. Calculations of the eclipse magnitude m are carried out to show ideal conditions for total solar eclipse observations in space from Lagrange point L2 for Mars (m ≈ 1.025). The illumination in Mars' shadow is estimated to equal 5.6 × 10−11 for the wavelength of 550 nm. No internal or external occulting coronagraphs are needed. Partial solar eclipses with m > 0.91 can be observed from Lagrange points L2 for Mercury, Venus, and Earth.

In this paper was demonstrated the possibility of the use of FAB mass spectrometry on an impulse mass spectrometer VG-70 SEQ ("Fisons VG Analytical", USA) for the study of biosynthetic pathways of 2 H-labeled purine ribonucleoside inosine secreted into the liquid culture (LC) by Gram-positive chemoheterotrophic bacterium Bacillus subtilis VKPM B-3157 when grown on heavy water (HW) medium with 2 % hydrolyzate of deuterated biomass of methylotrophic bacterium Brevibacterium methylicum VKPM B-5662 as a source of growth 2 H-labeled substrates.Isolation of 2 H-labeled inosine from the LC was performed by adsorption/desorption on activated carbon with following extraction by 0.3 M ammonium-formate buffer (pH = 8.9), crystallization in 80 % ethanol and ion exchange chromatography (IEC) on a column with AG50WX 4 cation exchange resin equilibrated with 0.3 M ammonium-formate buffer and 0.045 M NH 4 Cl.The investigation of deuterium incorporation into the molecule of biosynthetic [ 2 H]inosine by FAB mass spectrometry demonstrated the incorporation of 5 deuterium atoms into the molecule (the total level of deuterium enrichment -62.5 atom.% 2 H) with incorporation of 3 deuterium atoms into the ribose and 2 deuterium atoms -into the hypoxanthine residue of the molecule.Three non-exchangeable deuterium atoms were incorporated into the ribose residue owing to reactions of enzymatic izomerization of glucose in 2 H 2 O-medium due to reactions of glycolysis, associated with the Embden-Meyerhof pathway with participation of reactions of isotope ( 1 Н-2 Н) exchange, while two other deuterium atoms at C2, C8-positions in the hypoxanthine residue were synthesized from [ 2 H]amino acids that originated from the deuterated hydrolysate of the methylotrophic bacterium Brevibacterium methylicum VKPM B-5662.

Two approaches are suggested for recording the continuum corona in the range < 1.4 Rsun. They are different from the classical coronagraphic ones. Current state in the thin film technology allows discussing a new generation coronagraph with a variable transmission of an entrance aperture. The estimated coronagraphic factor is 2 orders of magnitude higher compared to a Lyot-type coronagraph. Another approach is based on the use of total solar eclipses at near-Mercury orbits. The instrumental background is decreased at least 3 orders of magnitude. That allows using a more simplified optical sketch.

Measurements of the linear polarization degree (p) of the emission in the inner corona (<1.5 R ⊙) in the green and red continuum ranges are discussed. “Excess p” (Δp = pgreen — pred), which reaches its maximum at 1.2–1.3 R ⊙ (<5%) in the polar regions and 20% within large-scale streamers, is present everywhere in the corona. It has been mentioned that excess p can be explained by the presence of neutral hydrogen in the corona.

Quasi-space totality sky brightness, the portable coronagraph-polarimeter, uniformity of a polarizer transmission for each point of the image, use of 24 orientations of a polarizer, and a specific algorithm for data reduction allowed to get the 2D distributions of the linear polarization degree ill the green and red spectral intervals with actual accuracy of 1-2% for the corona of March 29, 2006. The diffuse and structural components are revealed in the polarization degree images. Polar plumes are selected in the distributions. The systematical difference of 5-15% between the green and red polarization degrees is revealed for both diffuse and structural components. Abnormal polarization degrees of 65% are found in the green distribution for the features with the size of 8 - 30 '' below the top of the NW large-scale helmet streamer. It is noted that researches of the electron component of coronal plasma should be carried out in selected spectral intervals that are free of any absorption and emission lines.

The scientific purpose of the SPIRIT experiment is to study the space-time structures of phenomena of the solar activity using a set of X-ray instruments aboard the Koronas-F satellite. The system consists of the SRT-C six-channel telescope and the RES-C four-channel spectroheliometer for 8.4- to 335-Å wavelengths and the SPR-N five-range polarimeter for 20- to 100-keV energies. For a 3.5-yr flight (since July, 2001 to January, 2005), over 40000 observation sessions were conducted and over 1 million spectral pictures were obtained during the SPIRIT experiment. The volume of electronic archive of the experiment reached 220 Gbyte. The software package was developed for prompt control of the scientific system and used in the semiautomatic mode to form the sequence diagrams of energizing, create control files (CFs) via the dialog line, and schedule CF delivery. The software package is based both on the electronic table in the Excel-2000 format, which displays the basic procedures and control events, and on the database in the Access-2000 format, which is automatically filled with the information on all created CFs. For archiving, viewing, and selecting scientific data of the experiment, a graphic database in the Access-2000 format was created. The software for automatic filling of the database and a graphic interface for prompt viewing of the database and retrieval of pictures based on some parameters were designed. An automatic augmentable ballistic database containing basic parameters of the satellite orbit over the full flight period was created.

We describe the RESIK (REntgenovsky Spektrometr s Izognutymi Kristalami) instrument, consisting of two double-channel X-ray spectrometers, designed to observe solar active region and flare plasmas. RESIK is one of the instruments making up the scientific payload of the Russian CORONAS-F solar mission. The uncollimated spectrometer uses two silicon and two quartz bent crystals observing flare, active region and coronal spectra in four wavelength bands with a resolving power (λ/Δ λ) of ∼1000. The wavelength coverage, 3.3–6.1 Å, includes emission lines of Si, S, Cl, Ar, and K and in the third diffraction order, the wavelength range includes He-like Fe lines (1.85 Å) and Ni lines (1.55 Å) with dielectronic satellites, emitted during intense, hot flares. The instrument is believed to be the best calibrated space-borne crystal spectrometer flown to date. The spectrometer dynamically adjusts the data gathering intervals from 1 s to 5 minutes, depending on the level of solar X-ray emission at the time of observation. The principal aims of RESIK are the measurements of relative and absolute element abundances in the emitting plasma and the temperature distribution of plasma (differential emission measure) over the temperature interval 3 and 50 MK. This paper summarizes the scientific objectives of RESIK and describes the design, characteristics, and performance of the instrument.

The paper presents a brief review of the instruments developed for measurement of ionizing extreme UV solar radiation at wavelengths of less than 130 nm onboard the CORONAS-I and CORONAS-F satellites and summarizes the observation data. The main goal of the study was to obtain information concerning variations of fluxes of solar radiation and solar flares at various wavelengths in the extreme ultraviolet. SUFR radiometers based on the thermoluminescent method were mounted onboard both CORONAS satellites (CORONAS-I and CORONAS-F). They performed measurements at λ < 130 nm. Spectral measurements in the 30.4-nm line were made by the photoelectronic spectrometer VUSS tested on CORONAS-I. Spectral measurements in the waveband including the H Lα line (121.6 nm) were conducted by the VUSS-L instrument (a Lyman alpha spectrophotometer) onboard the CORONAS-F satellite. The basic characteristics of the instruments, which were supposed to be used in a system of space weather monitoring on patrol satellites of the hydrometeorological service of Russia, are presented. The main data on the solar radiation flux at λ < 130 nm for minimum and maximum solar activity are given for quiet conditions and during solar flares.

A multi-channel SPIRIT telescope/spectroheliograph aboard the CORONAS-F satellite operating in soft X-ray and EUV ranges ($T \sim $0.05–15 MK) is an effective instrument for complex studies of CME-associated phenomena such as eruptive filaments, dimmings, coronal waves, posteruptive arcades, etc. In particular, SRIRIT observations of high-temperature (T = 5–15 MK) plasma structures in the MgXII 8.42 Å line show specific pre-CME sigmoid magnetic field configurations. Eruptions of filaments (prominences) and dimmings in a CME process are seen with a high contrast in the coronal 175 Å band (FeIX–XI) and the transition-region 304 Å (HeII) images. Our results are illustrated by several powerful eruptive events of the current solar cycle. We compare SPIRIT data with observations at other spaceborne and ground-based instruments (SOHO/EIT, Yohkoh/SXT, and H$\alpha$ images, etc.)To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

RESIK is the bent crystal spectrometer aboard the CORONAS-F satellite. It is equipped with four PIN diode detectors. These detectors were used in order to detect background counts due to energetic particle contamination present within polar regions and SAA belts. At altitudes above 300 km (Coronas-F altitude is about 500 km) the population of charged particles trapped by the Earth's magnetic field consists of protons (energies between 100 keV and several hundred MeV) and electrons (energies between few tens of keV and 10 MeV). The construction of RESIK PIN diode detectors allows to sense particles with the energy above 1 MeV. We present diagrams illustrating the coupling of the Coronas-F particle environment and selected proxies of solar activity. The data shown have been collected during initial phase of mission.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The first results of the experiment with the SPR-N hard X-ray (20–100 keV) polarimeter onboard the Coronas-F observatory (the experiment started on August 15, 2001) are presented. Hard X-ray radiation was detected from several solar flares. The spectral and temporal parameters were determined and the polarization was estimated. Comparison with the GOES observations of thermal X-ray radiation shows that hard X-ray bursts occur at the growth phase of the thermal radiation and that they are associated with the bremsstrahlung of energetic electrons precipitating into the solar atmosphere.

Based on X-ray, gamma-ray, and charged-particle measurements with several instruments onboard the Coronas-F satellite and on ACE and GOES experimental data presented on the Internet, we investigate the parameters of the solar flare of November 4, 2001, and the energetic-particle fluxes produced by it in circumterrestrial space. The increase in relativistic-electron fluxes for about 1.5 days points to a moving source (shock front). The structure of the energetic-particles fluxes in the second half of November 5, 2001, can be explained by the passage of the coronal mass ejection that was ejected on November 1, 2001, and that interacted with the shock wave from the flare of November 4, 2001.

SPIRIT (SPectroheliographIc soft X-Ray Imaging Telescope) is the current experiment on board the CORONAS-F satellite launched on July 31, 2001 (Oraevskii & Sobelman, 2002). The main goal of this experiment is to study a structure and dynamics of the solar atmosphere in the wide scale of heights (from the chromosphere to a far corona) and of temperatures (from ten thousands through thirty millions Kelvins) by means of the XUV imaging spectroscopy. Since the launch of the CORONAS-F satellite more than three hundred thousands of images and spectroheliograms have been recorded, For the first time continuous series of monochromatic full Sun images in MgXII lines at 8.42 Angstrom (doublet: 8.418 and 8.423 Angstrom) were obtained. These series include long-term continuous observations of duration up to 10 days with the cadence of 100 sec as well as temporal sequences with duration of a few minutes and high resolution of 7 sec, synchronized with flares. The spectroheliograms for the whole disk and off-limb regions are also recorded in the spectral bands 177 - 207 and 285 - 335 A providing spectra with high resolution of various coronal structures including eruptive and transient events. This paper presents preliminary results of quick-look analysis of some observational data obtained by means of the SPIRIT spectroheliographs. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved.