Vol 63, No 1 (2025)

The integral luminosity values of the Herzberg I, Chamberlain and Atmospheric bands at mid-latitudes and in the equatorial zone of the Earth are calculated. The correlation of the results of theoretical calculations of the intensity of excited molecular oxygen glow on Earth with experimental data on the night glow of O₂ obtained from space shuttles, from the ground-based Kitt Peak Observatory (USA) for the Herzberg I and Chamberlain bands is discussed. For the Atmospheric bands, the correlation of the results of theoretical calculations with similar calculations based on measurement data from the ground-based Keck Observatory (USA) is analyzed. The integral luminosity values of the Herzberg I and Atmospheric bands for the northern latitudes of Mars are calculated.

The material presented in the paper continues a series of studies on the development of the use of the vector graph method for analyzing the characteristics of complex field and plasma structures generated by the Sun in interplanetary space. With a simplified approach to describing such systems using statistical methods, the collective processes of plasma and field interactions may remain undetected, in particular, complex multicomponent structures in the spatiotemporal distribution functions may be missed. The main problem of statistical methods is the neglect of the order of the states of the system being studied and the loss of information contained in this order. Based on the data blocks obtained by the detectors of the WIND apparatus in the CWE research complex and provided by the Coordinated Data Analyzes Web database, implementations of graphs for magnetic field induction vectors and solar wind particle velocity vectors reconstructed on the basis of experimental samples are discussed. The regimes of magnetic storms, the formation of magnetic clouds, and events associated with coronal mass ejections, both ICME and CME, are considered. The presented new method of synchronized pairs of graphs allows us to move from a phenomenological description of the process to a classification of the types of observed and studied multi-processes based on the structural implementations of graphs.

The article presents the results of studies of the emission coronal line λ = 6374 Å (FeX) for the period of solar cycle 24. The spectral data were obtained with an out-of-eclipse Lyot coronagraph at the Mountain Astronomical Station of the Pulkovo Observatory, Russian Academy of Sciences (near Kislovodsk). Based on the processing of the results of out-of-eclipse observations, a database of three types of daily coronal maps with a distribution by altitude h from 1 R_ʘ to 1.38 R_ʘ (R_ʘ is the radius of the Sun) of the red line intensity (I₆₃₇₄) was created. Throughout the solar cycle, spectral observations demonstrating a Doppler shift along the red line λ = 6374 Å were found. The extension of the red line from the limb position angle of the Sun was calculated. It was shown that the maximum value of the average extension of the coronal line over the entire limb falls on the ascent branch of solar cycle 24. For different phases of the considered solar cycle (for the ascending branch, the period of maximum, the descending branch and the minimum of solar activity) and for different regions of solar activity, the dependences of the change in I₆₃₇₄ values with altitude were plotted and explained. A regression analysis of the obtained relationships is carried out. The regression equations are presented. The changes in I₆₃₇₄ with altitude for the polar regions (for all phases of the cycle except for the maximum and the descending branch) and for the middle latitudes (for the minimum of activity) most likely have a logarithmic dependence, and the approximating trend curves for the remaining latitudinal zones are determined by a third-order power function.

The radiation from galactic and solar cosmic rays as they pass through the modern and rarefied (as a result of multiple reversals) atmosphere during solar proton events and at the time of geomagnetic reversal is studied. We assume that during the reversal process the geomagnetic field weakens and takes on an axisymmetric quadrupole configuration. It is shown that in the case of a single reversal, when the atmosphere does not have time to change, radiation dose powers increase only at low latitudes and are identical to the modern radiation at the poles. However, during the period of multiple inversions, when the atmosphere is rarefied, the level of radiation at the moment of reversal on the Earth's surface increases, on average, twice as much as today's radiation at all latitudes, which can affect the biosphere.

The paper considers the prerequisites for the creation of satellite systems of small spacecraft of the cubesat type for heliogeophysical purposes. The history of the appearance and features of this type of platform are described, and examples of their implementation are given. The domestic satellite group of the small spacecraft, developed under the programs “Universat” and “Space-Pi”, are also considered. Small spacecraft with magnetometric measuring equipment on board are described. Based on the results of the analysis, the main relevant directions for the development of on-board heliogeophysical and, in particular, magnetometric equipment have been identified. Problems have also been identified in the implementation system of the received data. As examples of modern developments in the field of satellite heliogeophysical observations, the activities of Institute of Applied Geophysics as a thematic customer, expert and manufacturer of equipment are described. The possibilities of analyzing data from already in use devices are described, and prospects for further development are also stated.

Stand testing of an autonomous optical navigation system for operation in circumlunar orbits and during Earth-Moon transfer was performed. The system includes a wide-angle navigation camera for estimation of spacecraft position using observations of the planet’s horizon and of ground control points on its surface, a narrow-angle navigation camera for refinement the SC position using ground control points in higher resolution images, and two star trackers for determination of system orientation. The navigation software was also tested using the image of the lunar surface obtained by the television system STS-L installed on the Luna-25 spacecraft. All the control points from the developed catalog that were located in the imaged area were confidently recognized. The diversion in the spacecraft coordinates as obtained from the optical navigation measurements and from the ballistic forecast was within the expected measurement and forecast errors.