Orientation of Sharp Fronts of the Solar Wind Plasma

Based on simultaneous observations performed by several spacecraft, we evaluate the orientation of sharp (with a duration of a few minutes) and large (tens and hundreds percent of the mean value) fronts of the solar wind plasma (changes in the ion flux and ram pressure). The orientation of the fronts is determined with respect to the Sun–Earth line and to two planes in space for several tens of the largest (in amplitude) changes of the ion flux. A considerable fraction of these fronts (about 50%) has an inclination to the plane perpendicular to the Sun–Earth line that exceeds 30°.     

Orientation of Middle-Scale Structures in the Solar Wind Plasma

An estimation of the value and orientation of the inclination of middle-scale structures in the solar wind plasma is obtained on the basis of time lags of simultaneous correlated measurements on three spacecraft: INTERBALL-1, IMP-8, and WIND. It is shown that middle-scale plasma structures, in the majority of cases, are not perpendicular to the Sun–Earth line, but inclined to it (presumably, in the ecliptic plane), on average, at an angle of approximately 63° (or 27° to the Y _SE axis). However, this inclination is significantly less than the inclination of the Parker spiral for the interplanetary magnetic field (45° at the Earth's orbit).     

Sharp Boundaries of Solar Wind Plasma Structures and an Analysis of Their Pressure Balance

This work is devoted to studying the sharp boundaries of small-scale structures of the solar wind according to the data of measurements with high time resolution onboard the INTERBALL-1 satellite and simultaneous measurements of the WIND spacecraft. Such issues as the character of change of various plasma and magnetic field parameters on these boundaries, the duration of boundary passage and the balance of the total (thermal plus magnetic) pressure on the boundaries of the structures are considered. On the basis of the vast statistical material available, the typical conditions in the solar wind are investigated, in which such sharp boundaries are observed.__________Translated from Kosmicheskie Issledovaniya, Vol. 43, No. 3, 2005, pp. 163–170.Original Russian Text Copyright © 2005 by Riazantseva, Khabarova, Zastenker, Richardson.     

Fast measurements of parameters of the Solar Wind using the BMSW instrument

Design of the plasma spectrometer BMSW (Fast Monitor of the Solar Wind, possessing high temporal resolution) is described in the paper, as well as its characteristics and modes of operation. Some examples of measurements of various properties of the solar wind, made with this instrument installed onboard the high-apogee satellite Spektr-R, are presented.     

Influence of Solar Wind Parameters on the Level of Geomagnetic Field Fluctuations

We investigated the dependence of the geomagnetic activity index K _p on the velocity and density of the solar wind and the intensity of the interplanetary magnetic field (IMF). A three-layer neural network was used to create the model. The degree of the influence of input parameters on K _p was determined by the value of the mean and root-mean square deviations of the model index values from the real indices. It was found that the largest contribution to the K _p index is provided by the Z component of the IMF, the velocity and density of the solar wind measured with a delay from 0 to 3 h relative to the studied value of K _p, and the previous value of the index itself. For the model with such a set of input parameters, the correlation coefficient between model and real series is ±0.89. The analysis of deviations from the real values of K _p showed that high indices are simulated worse than low indices. In order to solve this problem the data distribution was reduced to a uniform distribution over K _p, and this considerably decreased the standard deviations for large values of K _p.     

Variations of Protons and Doubly Ionized Helium Ions in the Solar Wind

Cosmic Research - We investigated variations on scales of 104–105 km and local spatial inhomogeneities in the density of protons Np, doubly ionized helium ions (α-particles) Nα, and...     

用太阳舵控制大型挠性体太空帆的控制方法

本文论述了一种用太阳舵控制大型挠性体太空帆的控制方法。介绍了太阳舵控制原理、控制方案,给出了控制规律,推导了解耦控制力矩方程。最后分析了挠性振动的稳定性控制。     

基于形状的火卫一重力场研究

介绍基于形状对不规则小天体重力场建模的原理和方法,并通过解析法和数值法对火卫一的重力场进行正演建模。相比之前的重力场模型,基于解析算法获得的17阶次球谐展开形式重力场模型,在分辨率上有显著提高。进一步结合火卫一动力学参数,分析了火卫一表面加速度。结果显示,火卫一因其轨道十分接近火星,导致表面离心力和潮汐力十分显著,在某些区域与自引力相当,造成火卫一的特殊表面重力环境。这些结果可为未来的火卫一探测和科学研究提供基本输入物理场模型,也可为其他小天体探测中的类似问题提供方法参考。     

The Earth's Magnetosphere Response to Solar Wind Events according to the INTERBALL Project Data

The results of studying the interaction of two types of the solar wind (magnetic clouds and solar wind of extremely low density) with the Earth's magnetosphere are discussed. This study is based of the INTERBALL space project measurements and on the other ground-based and space observations. For moderate variations of the solar wind and interplanetary magnetic field (IMF) parameters, the response of the magnetosphere is similar to its response to similar changes in the absence of magnetic clouds and depends on a previous history of IMF variations. Extremely large density variations on the interplanetary shocks, and on leading and trailing edges of the clouds result in a strong deformation of the magnetosphere, in large-scale motion of the geomagnetic tail, and in the development of magnetic substorms and storms. The important consequences of these processes are: (1) the observation of regions of the magnetosphere and its boundaries at great distances from the average location; (2) density and temperature variations in the outer regions of the magnetosphere; (3) multiple crossings of geomagnetic tail boundaries by a satellite; and (4) bursty fluxes of electrons and ions in the magnetotail, auroral region, and the polar cap. Several polar activations and substorms can develop during a single magnetic cloud arrival; a greater number of these events are accompanied, as a rule, by the development of a stronger magnetic storm. A gradual, but very strong, decrease of the solar wind density on May 10–12, 1999, did not cause noticeable change of geomagnetic indices, though it resulted in considerable expansion of the magnetosphere.     

Properties of Sharp and Large Changes in the Solar Wind Ion Flux (Density)

The results of a detailed study of large (by 20% and more) and sharp (faster than ten minutes) changes of the ion flux in the solar wind are presented. The data are provided by regular measurements onboard the INTERBALL-1 satellite in the period 1996–1999. Using statistical analysis, we obtained the distribution of these changes in their absolute and relative strength. It is shown that, for a considerable proportion of the events, such sharp and large changes of the ion flux (density) take place under conditions of fairly constant values of the solar wind velocity and of both the magnitude and components of the interplanetary magnetic field.     

利用等离子体通道实现空间太阳能无线能量传输

空间太阳能电站是高效利用太阳能的有效途径,受到了国际的广泛关注。空间无线能量传输技术是空间太阳能电站的关键技术之一。文章首先分析了微波与激光无线能量传输技术的问题,根据空间太阳能传输的具体需求进一步提出基于等离子体通道的无线能量传输技术,并对基于此项技术的空间太阳能传输系统进行了论证,完善并发展了空间太阳能传输模型。基于等离子体通道的无线能量传输技术为多个领域的能量补给提供了新颖的技术途径,是具有广阔应用前景的战略选择。     

Quasi-synchronous orbits and their employment for the approach of a spacecraft to Phobos

The problem of construction of quasi-synchronous orbits which pass through a prescribed point over the surface of Phobos at a prescribed instant of time is considered. The orbits should pass as close as possible to the surface of Phobos at each passage above the planned region of landing.     

Transport Characteristics of Macroparticles in Dusty Plasma Induced by Solar Radiation under Microgravity Conditions

The transport characteristics of macroparticles, charged by the solar radiation under microgravity conditions, were investigated by analyzing the videorecords of experiments carried out onboard the Mirorbital station. The temperature, distributions of velocities, charge, friction coefficient, and diffusion coefficient were obtained for bronze particles.     

Characteristics of the Martian Magnetosphere according to the Data of the Mars 3 and Phobos 2 Satellites: Comparison with MGS and MAVEN Results

Cosmic Research - On January 21, 1972, the Mars 3 satellite recorded a strong (~27 nT) regular magnetic field in the region of the spacecraft’s closest approach to the dayside of Mars. Many...