Ascending flows in the solar atmosphere and formation of the solar wind

Some morphological features of solar magnetic fields in the chromosphere and corona are considered based on studying various observational data. These data are compared to the results of observation of the solar wind and interplanetary magnetic field, as well as to the data on fluxes of solar cosmic rays. New specific features are found in the solar wind structure, and new additional indications of sources of the solar wind are obtained. The properties of the active regions and coronal holes are considered. A model of the ascending stream-like plasma flow is suggested. It flows around the discrete arched magnetic field tubes in the solar atmosphere and stretches them out into interplanetary space.     

电磁环境卫星系统及在地震短临预测中的应用

论述了近地空间电磁场和电离层探测的要素及其在地磁模型、电离层模型建立等方面的应用需求,并结合地震短临预测中的具体应用分析,阐述了我国建立近地空间电磁探测系统的初步研究结果,包括电磁环境探测要素、星载探测仪器配置、卫星系统组成设想和卫星平台技术需求等。     

Dust Plasma Dynamics in the Geomagnetic Tail

The results of numerical modeling of dust plasma dynamics in the geomagnetic tail are presented for the southward and northward orientations of the interplanetary magnetic field in the model with reconnection of magnetic field lines of geomagnetic and interplanetary magnetic fields. It is shown that in reconnection regions the compression shock waves arise, at the fronts of which the dust plasma fluxes with higher-than-background density are generated.     

Manned exploration and exploitation of solar system: Passive and active shielding for protecting astronauts from ionizing radiation—A short overview

In deep space manned missions for the exploration and exploitation of celestial bodies of Solar System astronauts are not shielded by the terrestrial magnetic field and must be protected against the action of Solar Cosmic Rays (SCRs) and Galactic Cosmic Rays (GCRs). SCRs are sporadically emitted, and in very rare but possible events, their fluence can be so high to be lethal to a unprotected crew. Their relatively low energy allows us to conceive fully passive shields, also if active systems can somewhat reduce the needed mass penalty. GCRs continuously flow without intensity peaks, and are dangerous to the health and operability of the crew in long duration (>1year) missions. Their very high energy excludes the possible use of passive systems, so that recourse must be made to electromagnetic fields for preventing ionizing particles to reach the habitat where astronauts spend most of their living and working time. A short overview is presented of the many ideas developed in last decades of last century; ideas are mainly based on very intense electrostatic shields, flowing plasma bubbles, or enormous superconducting coil systems for producing high magnetic fields. In the first decade of this century the problem began to be afforded in more realistic scenarios, taking into account the present and foreseeable possibilities of launchers (payload mass, diameter and length of the shroud of the rocket, etc.) and of assembling and/or inflating structures in space. Driving parameters are the volume of the habitat to be protected and the level of mitigation of the radiation dose to be guaranteed to the crew. Superconducting magnet systems based on multi-solenoid complexes or on one huge magnetic torus surrounding the habitat are being evaluated for defining the needed parameters: masses, mechanical structures for supporting the huge magnetic forces, needed equipments and safety systems. Technological tests are in preparation or planned for improving density of the current, lightness and stability, to increase working temperature of superconducting cables, and for finding light supporting structures and suitable safety architectures, delineating a possible development program for affording this difficult problem.     

Space weather forecast: Principles of the construction and boundaries of the implementation (experience of three cycles)

All significant short-term disturbances of the near-Earth space are caused exclusively by solar flare events and regions in the solar corona with the magnetic field open into the interplanetary space (coronal holes). Flare processes occur as a consequence of the interactions of new emerging magnetic fluxes within (flares) and outside (filament ejections) the active regions with already existing magnetic fields. The observation of emerging new magnetic fluxes and the estimate of their magnitude and the emerging rate allow one to forecast solar flares and filament ejections and estimate their degree of geoeffectiveness. The main agents that visualize the propagation of disturbance from solar flares and filaments in the solar corona and the interplanetary space are coronal mass ejections, the characteristics of which ideally allow one to estimate the possible disturbance of the geomagnetic field, the possible growth of high-energy charged particle fluxes in the near-Earth space. For successful forecast of geoeffective active phenomena on the Sun and their consequences in the near-Earth space, it is necessary to know the situation on the Sun for the last 3 days taking into account the development and characteristics of the current cycle and the epoch of solar activity.     

Eddy currents induced migration of droplets in electrically conducting fluid in microgravity environments

Electrical eddy currents induced migration of droplets, whose conductivity differs from that of surrounding fluid, is analysed. Eddy currents in a dilute suspension under consideration, which fills the dielectric tube, are induced by alternating magnetic field parallel to the tube axis. In the case where the droplet radius is small as compared to the skin depth, the distributions of magnetic fields, currents and electromagnetic forces inside and outside the droplet have been calculated. For small Reynolds numbers, with neglecting inertial and thermocapillary effects and the gravity, the flow of fluids around the droplet and inside it, caused by electromagnetic forces, has been studied. The formula is obtained, which relates the droplet migration velocity to the electro-magnetic field, the droplet size and physical properties of fluids.     

Scientific investigations at a lunar base.

Scientific investigations to be carried out at a lunar base can have significant impact on the location, extent, and complexity of lunar surface facilities. Among the potential research activities to be carried out are: (1) Lunar Science: Studies of the origin and history of the Moon and early solar system, based on lunar field investigations, operation of networks of seismic and other instruments, and collection and analysis of materials; (2) Space Plasma Physics: Studies of the time variation of the charged particles of the solar wind, solar flares and cosmic rays that impact the Moon as it moves in and out of the magnetotail of the Earth; (3) Astronomy: Utilizing the lunar environment and stability of the surface to emplace arrays of astronomical instruments across the electromagnetic spectrum to improve spectral and spatial resolution by several orders of magnitude beyond the Hubble Space Telescope and other space observatories; (4) Fundamental physics and chemistry: Research that takes advantage of the lunar environment, such as high vacuum, low magnetic field, and thermal properties to carry out new investigations in chemistry and physics. This includes material sciences and applications; (5) Life Sciences: Experiments, such as those that require extreme isolation, highly sterile conditions, or very low natural background of organic materials may be possible; and (6) Lunar environmental science: Because many of the experiments proposed for the lunar surface depend on the special environment of the Moon, it will be necessary to understand the mechanisms that are active and which determine the major aspects of that environment, particularly the maintenance of high-vacuum conditions. From a large range of experiments, investigations and facilities that have been suggested, three specific classes of investigations are described in greater detail to show how site selection and base complexity may be affected: (1) Extended geological investigation of a complex region up to 250 kilometers from the base requires long range mobility, with transportable life support systems and laboratory facilities for the analysis of rocks and soil. Selection of an optimum base site would depend heavily on an evaluation of the degree to which science objectives could be met. These objectives could include lunar cratering, volcanism, resource surveys or other investigations; (2) An astronomical observatory initially instrumented with a VLF radio telescope, but later expanding to include other instruments, requires site preparation capability, "line shack" life support systems, instrument maintenance and storage facilities, and sortie mode transportation. A site perpetually shielded from Earth is optimum for the advanced stages of a lunar observatory; (3) an experimental physics laboratory conducting studies requiring high vacuum facilities and heavily instrumented experiments, is not highly dependent on lunar location, but will require much more flexibility in experiment operation and EVA capability, and more sophisticated instrument maintenance and fabrication facilities.     

Energy cycling and hypothetical organisms in Europa's ocean

While Europa has emerged as a leading candidate for harboring extraterrestrial life, the apparent lack of a source of free energy for sustaining living systems has been argued. In this theoretical analysis, we have quantified the amount of energy that could in principle be obtained from chemical cycling, heat, osmotic gradients, kinetic motion, magnetic fields, and gravity in Europa's subsurface ocean. Using reasonable assumptions based on known organisms on Earth, our calculations suggest that chemical oxidation-reduction cycles in Europa's subsurface ocean could support life. Osmotic and thermal gradients, as well as the kinetic energy of convection currents, also represent plausible alternative sources of energy for living systems at Europa. Organisms thriving on these gradients could interact with each other to form the complex energy cycling necessary for establishing a stable ecosystem.     

Calculation of the Initial Magnetic Field for Mercury’s Magnetosphere Hybrid Model

Several types of numerical models are used to analyze the interactions of the solar wind flow with Mercury’s magnetosphere, including kinetic models that determine magnetic and electric fields based on the spatial distribution of charges and currents, magnetohydrodynamic models that describe plasma as a conductive liquid, and hybrid models that describe ions kinetically in collisionless mode and represent electrons as a massless neutralizing liquid. The structure of resulting solutions is determined not only by the chosen set of equations that govern the behavior of plasma, but also by the initial and boundary conditions; i.e., their effects are not limited to the amount of computational work required to achieve a quasi-stationary solution. In this work, we have proposed using the magnetic field computed by the paraboloid model of Mercury’s magnetosphere as the initial condition for subsequent hybrid modeling. The results of the model have been compared to measurements performed by the Messenger spacecraft during a single crossing of the magnetosheath and the magnetosphere. The selected orbit lies in the terminator plane, which allows us to observe two crossings of the bow shock and the magnetopause. In our calculations, we have defined the initial parameters of the global magnetospheric current systems in a way that allows us to minimize paraboloid magnetic field deviation along the trajectory of the Messenger from the experimental data. We have shown that the optimal initial field parameters include setting the penetration of a partial interplanetary magnetic field into the magnetosphere with a penetration coefficient of 0.2.     

CRYOGENIC TECHNOLOGY TO IMPROVE ELECTRIC THRUSTERS

This paper analyzes superconducting (SC) coils technology to improve satellite electric propulsion. SC magnets can generate very high magnetic fields with extremely low ohmic losses, low electric power and PCU weight. Moreover, the weight of SC magnet coils is quite low compared with conventional or permanent magnets capable of producing the same field strength. For instance, to obtain a 0.4 T magnetic field strength, typical of applied field magnetoplasmadynamic thrusters (AF-MPD), based on the Lorentz force, and with thrust in the range of 1 N, this paper shows that only a 40 g coil SC weight is needed, whereas an equivalent field copper winding would weigh about 36 kg. Using SC technology it is shown that the limited magnetic induction provided by a permanent magnet may be raised and also that it is possible to obtain high magnetic fields (of order of several Tesla) with fewer turns, drastically reducing coil volume, weight and complexity compared to conventional winding.

Superconductivity at low temperature (LTSC) requires liquid helium at 4.2 K to produce very high current densities: the thermal analysis in this paper shows that, depending on satellite and thruster, high temperature superconductors (HTSC) wires are sometimes better than LTSC because these can support lower current densities but with a critical superconductivity temperature higher than for LHe, requiring LN₂ at 77 K, easier to maintain during the whole mission.

Finally, this paper shows that implementing SC cryogenic technology on a satellite can be achieved with current active coolers technology.     

An analysis of magnetic protection of spacecraft against penetrating radiation

Negative effect of cosmic ray particles is a serious danger for astronauts and onboard equipment. When planning interplanetary flights it becomes one of the main obstacles. The aim of this work is to analyze currently available methods of protecting spacecraft against cosmic rays using magnetic fields and to choose the most effective method. Three variants of protection systems were considered, two of which had been described in scientific literature: with azimuth and axial magnetic filed. The third, more general method (with helical magnetic field) is suggested here for the first time. The first two variants are extreme special cases of the third one. The exact solution is obtained for the problem of motion of a charged relativistic particle in the helical magnetic field, and a criterion of particle reflection is determined. A comparative analysis of reflection characteristics of the chosen systems has been performed, and the conclusion about the optimal configuration of the magnetic protection is drawn.     

The Fields of Magnetospheric Current Systems on the Earth's Surface in an Interval of the Magnetic Storm Studied under the International Program on Solar–Terrestrial Physics

Using the magnetic storm in January 1997 as an example, we examined the possibilities to employ the magnetospheric field T96 [1, 2] and the dynamic paraboloid model PM of the magnetosphere [3] for modeling the D _st variation. We have revealed the necessity to refine the results of normalizing the free parameters of the model T96 according to the solar wind parameters. The contributions to the D _st variation of magnetic fields of basic large-scale magnetospheric current systems (the field DCF on the magnetopause, the field DR of the ring current, and the field DT in the magnetotail) are estimated for different phases of the storm from model calculations. Possible causes of a discrepancy between the results of modeling D _st using the T96 and PM models are discussed. Special emphasis is made on the ratios of contributions into the D _st variation of the fields of the magnetotail and the ring current in the main phase of magnetic storms and on the contributions to D _st of the fields of various current systems at the recovery phase.     

Excitation and propagation of an electromagnetic pulse in magnetized plasma in the low-hybrid frequency range

We analyze specific features of slow quasi-static waves excited in the low-hybrid frequency band by a source whose dimensions are much smaller than electromagnetic wavelength. Main attention in this paper is given to an analysis of emission of harmonic signals by a dipole source in pulsed mode. First, the issue of influence of electromagnetic, thermal, and collision corrections in the dispersion equation on the field structure has been studied. Second, the structure of electric and magnetic fields near the resonant cone has been analyzed: in particular, effects of group delay and anomalous spreading of signals are considered. Thus constructed theory explains results of the OEDIPUS-C experiment, in which, for example, already at distances of order of ten wavelengths a signal delay of approximately 10^?4 s was observed. Finally, we have studied some aspects of the inverse problem of electrodynamics: the role played in field formation by smoothness of charge distribution over antenna is demonstrated, and a class of smooth distributions of charge on antenna is found that form a preset field structure.     

The electromagnetic rocket gun

A novel propulsion concept is proposed which has the potential of accelerating large masses to velocities substantially higher than what is possible with chemical rockets. The novel concept is an electromagnetic gun, where the projectile is a rocket. The proposed concept solves the old problem of magnetic propulsion, which is the resistive dissipation of the induced electric currents into heat which will vaporize the projectile long before it can reach a high velocity. As in a rocket, where the propellant cools and thereby prevents the rocket from burning up, the same happens in the proposed concept where the propellent also cools the projectile and prevents its vaporization. The propellant, however, not only cools the projectile but in addition is resistively heated by the magnetic field and ejected from the projectile with high velocity. The resulting recoil produces an additional thrust which is approximately as large as the thrust exerted by the magnetic field alone. The energy to drive the jet is externally supplied, making the specific impulse much larger than for chemical rockets.     

Effect of large and sharp changes of solar wind dynamic pressure on the earths’s magnetosphere: analysis of several events

The magnetosphere and ionosphere response to arrival of large changes of the solar wind dynamic pressure with sharp fronts to the Earth is considered. It is shown that, under an effect of an impulse of solar wind pressure, the magnetic field at a geosynchronous orbit changes: it grows with increasing solar wind pressure and decreases, when the solar wind pressure drops. Energetic particle fluxes also change: on the dayside of the magnetosphere the fluxes grow with arrival of an impulse of solar wind dynamic pressure, and on the nightside the response of energetic particle fluxes depends on the interplanetary magnetic field (IMF) direction. Under the condition of negative Bz-component of the IMF on the nightside of the magnetosphere, injections of energetic electron fluxes can be observed. It is shown, that large and fast increase of solar wind pressure, accompanied by a weakly negative Bz-component of the IMF, can result in particless’ precipitation on the dayside of the auroral oval, and in the development of a pseudobreakup or substorm on the nightside of the oval. The auroral oval dynamics shows that after passage of an impulse of solar wind dynamic pressure the auroral activity weakens. In other words, the impulse of solar wind pressure in the presence of weakly negative IMF can not only cause the pseudobreakup/substorm development, but control this development as well.     

十字形磁梯度张量结构在多磁偶极子测量中的误差与修正方法

磁场全张量探测技术在多磁源反演中有着重要意义。十字形磁梯度张量结构因其计算简单、精度高等特点被广泛采用,但其在多磁源反演中的全方位误差分析和修正方法有待完善。文章研究多磁偶极子分辨的问题,分析十字形计算结构和误差来源;结果表明磁力仪的精度、整体结构、背景环境和基线选取都会造成误差,甚至导致错误;最后给出修正方法和建议,同时提出可行的扫描方法。     

高精度非接触磁浮机构电磁干扰特性分析

针对因双超平台姿态控制引入非接触磁浮机构这一关键执行机构,而可能引起的卫星平台新的电磁兼容问题,开展了非接触磁浮机构的电磁干扰特性研究。首先,介绍了非接触磁浮机构及其驱动器的工作原理;其次,分别对非接触磁浮机构驱动器的脉冲宽度调制(PWM)控制信号高频干扰特性和传导电磁干扰特性进行了理论和仿真分析,并将其频率特性与星上其他典型单机的工作频率进行了比对。对比分析结果表明:非接触磁浮机构的电磁干扰频率与星上其他典型单机之间间隔较大,其相互之间产生的电磁干扰可忽略,磁浮机构的引入不会产生新的电磁兼容问题。     

线圈磁传感器的发展现状与空间应用

基于电磁感应的线圈磁传感器由于其灵敏度高、工作原理简单、性能可靠,在空间微弱磁场测量方面获得广泛应用。文章介绍了线圈磁传感器性能提高的几项主要技术及其基本原理,以及线圈磁传感器的发展及空间应用现状。通过采用优化设计磁芯,改善线圈结构以及与其他类型磁传感器协同工作等技术,线圈磁传感器的性能已经获得极大提高。随着这些技术的进一步完善,线圈磁传感器将在未来空间环境探测领域中发挥更加重要的作用。     

Excitation of Pc5 pulsations of the geomagnetic field and riometric absorption

We consider in detail the intense Pc5 pulsations of the magnetic field, riometric absorption, and electron fluxes occurred on the recovery phase of the strong magnetic storm on November 21, 2003. The global structure of these disturbances is studied using the world network of magnetometers and riometers supplemented by the data of particle detectors onboard the LANL geosynchronous satellites. The local spatial structure is investigated according to data of the regional network of Finnish vertical riometers and of stations of the IMAGE magnetic network. Though a certain similarity is observed in the frequency composition and time evolution of the variations of magnetic field and riometric absorption, the local spatial structure of these oscillations turns out to be different. It is suggested that these variations can be manifestations of oscillatory properties of two weakly connected systems: the magnetospheric MHD waveguide/resonator and the system cyclotron noise + electrons. The recorded Pc5 oscillations are, presumably, a result of excitation of the magnetospheric waveguide on the morning and evening flanks of the magnetosphere. At high velocities of the solar wind this waveguide can appear in a metastable state. Not only jumps in the solar wind density, but injection of electrons into the magnetosphere as well, can serve as a trigger for the waveguide excitation.