The Strength and Structure of the Coronal Magnetic Field

I discuss a method for determining the strength and spatial structure of the coronal magnetic field by observations of the Faraday rotation of a radio galaxy which is in conjunction with the Sun. Given a knowledge of the plasma density in the outer corona, and the magnetic field sector structure (both independently available), the strength of the coronal field can be determined, as well as the magnitude of spatial variations on scales of 1000 km to several solar radii. Such knowledge is crucial for testing computational models of the solar corona, which are prominently featured in this meeting. Results are presented from observations with the Very Large Array radio telescope of the radio galaxy 3C228 on August 16, 2003, when the line of sight to the source was at heliocentic distances of 7.1−6.2R _⊙. The observations are consistent with a coronal magnetic field which is proportional to the inverse square of the distance in the range 6 ≤ r ≤ 10R _⊙, and has a value of 39 mG at 6.2R _⊙. The Faraday rotation is uniform across the source, indicating an absence of strong plasma inhomogeneity on spatial scales up to 35,000 km.     

Large geomagnetic storms of extreme solar event periods in solar cycle 23

During extreme solar events such as big flares or/and energetic coronal mass ejections (CMEs) high energy particles are accelerated by the shocks formed in front of fast interplanetary coronal mass ejections (ICMEs). The ICMEs (and their sheaths) also give rise to large geomagnetic storms which have significant effects on the Earth’s environment and human life. Around 14 solar cosmic ray ground level enhancement (GLE) events in solar cycle 23 we examined the cosmic ray variation, solar wind speed, ions density, interplanetary magnetic field, and geomagnetic disturbance storm time index (D_st). We found that all but one of GLEs are always followed by a geomagnetic storm with D_st  −50 nT within 1–5 days later. Most(10/14) geomagnetic storms have D_st index  −100  nT therefore generally belong to strong geomagnetic storms. This suggests that GLE event prediction of geomagnetic storms is 93% for moderate storms and 71% for large storms when geomagnetic storms preceded by GLEs. All D_st depressions are associated with cosmic ray decreases which occur nearly simultaneously with geomagnetic storms. We also investigated the interplanetary plasma features. Most geomagnetic storm correspond significant periods of southward B_z and in close to 80% of the cases that the B_z was first northward then turning southward after storm sudden commencement (SSC). Plasma flow speed, ion number density and interplanetary plasma temperature near 1 AU also have a peak at interplanetary shock arrival. Solar cause and energetic particle signatures of large geomagnetic storms and a possible prediction scheme are discussed.     

Dynamic processes in the outer heliosphere: voyager observations and models

We review recent Voyager 2 observations in the vicinity of 70 AU. The character of the solar wind plasma data between 2002 and 2003 changed to a regime in which the speed, density and magnetic field magnitude are positively correlated. The average speed of the solar wind at Voyager 2 increased between early 2003 and mid-2004, which we attribute to a return of fast coronal hole flow. We use solar wind data at Earth as input to numerical models which include the effect of pickup ions to model the radial evolution of the solar wind. The model reproduces the basic features of the observations. As a specific example, we investigate the propagation of the Halloween (Oct.–Nov.), 2003 storms in the outer heliosphere. The model predictions are in reasonable agreement with Voyager 2 observations.     

RPC-IES: The Ion and Electron Sensor of the Rosetta Plasma Consortium

The ion and electron sensor (IES) is part of the Rosetta Plasma Consortium (RPC). The IES consists of two electrostatic plasma analyzers, one each for ions and electrons, which share a common entrance aperture. Each analyzer covers an energy/charge range from 1 eV/e to 22 keV/e with a resolution of 4%. Electrostatic deflection is used at the entrance aperture to achieve a field of view of 90°× 360° (2.8π sr). Angular resolution is 5°× 22.5° for electrons and 5°× 45° for ions with the sector containing the solar wind being further segmented to 5°× 5°. The three-dimensional plasma distributions obtained by IES will be used to investigate the interaction of the solar wind with asteroids Steins and Lutetia and the coma and nucleus of comet 67P/Churyumov–Gerasimenko (CG). In addition, photoelectron spectra obtained at these bodies will help determine their composition.     

开槽钝锥体及等离子体鞘套的RCS特性研究

采用时域有限差分（FDTD）方法研究了等离子体鞘套包覆目标的电磁散射特性,发展了超高速飞行器及其等离子体鞘套RCS特性并行计算软件。采用发展的软件完成了超高速开槽钝锥后向远区时域特性和0°入射角附近的电磁散射截面积（RCS）的计算分析,并在中国空气动力研究与发展中心的气动物理靶上进行了超高速开槽钝锥体的RCS验证试验。研究表明：在钝锥体表面开环槽并填充透波性能良好的介质材料相当于在钝锥体表面人为地增加了一个散射中心;在低频区和谐振区,开槽后钝锥体的RCS在原值周围变化,而在高频区,钝锥体的RCS在0°入射角附近很宽的范围内均显著增大。     

Ionospheric storm of September 2017 observed at ionospheric station Pruhonice,the Czech Republic

The ionospheric effects induced by the September 2017 storm have been exceptional compared to other events in the solar cycle 24. This paper gathers results of the ionospheric observations at the European middle latitude station Pruhonice. It consists of evaluation of ionospheric vertical and oblique sounding, Digisonde drift measurement, and data obtained from the Continuous Doppler Sounding System. We observed strong ionospheric response with an unusual stratification of ionospheric layers, Large Scale Traveling ionospheric disturbances, changes in electron density, and increase and oscillations in plasma drift velocity.     

翼型动态失速影响因素及流动控制研究进展

深入认识翼型动态失速，结合有效流动控制手段，对解决直升机、风力机桨叶等动态失速引起的高阻力、大低头力矩等气动问题具有重要意义。本文首先介绍了翼型动态失速的流场特点和危害，进而分析了缩减频率、雷诺数、马赫数以及翼型型面等参数对动态失速的影响，并在此基础上总结了常见的动态失速流动控制方法及其研究进展。等离子体气动激励易于产生快速、可控的宽频带气动激励，在动态失速控制领域具有潜力，本文着重介绍了等离子体气动激励动态失速控制的概念和流动控制原理，总结了近来年等离子体激励在翼型动态失速控制上的进展。     

放电等离子烧结法制备多孔铝材料

采用等离子脉冲烧结(SPS)进行了多孔铝块体材料的制备。结果表明采用该方法在350℃时可以制备出结构与尺寸可控性好、粉体颗粒无明显长大、孔隙率(54.07%)较高的多孔金属铝块体材料。该制备方法对于开孔性与颗粒连接性要求较高的多孔金属材料具有较高的技术优势。     

介质阻挡放电等离子体气动激励的动量特性

从诱导气流速度和体积力两个方面开展了介质阻挡放电等离子体气动激励的动量特性研究,对不同激励参数下的诱导气流速度进行了测量与结果分析;通过对体积力的实验测量与理论计算,对比研究了体积力的变化规律与主要影响因素.结果表明:等离子体气动激励可以增大气流速度,但随着气流速度的增大,等离子体气动激励的加速效果减弱;激励电压或激励频率增大,体积力均表现为线性增加,但激励电压增大时可以更好的增大体积力;与增大电极内间距相比,增大下层电极宽度可以产生更大的体积力.