Determining CME parameters by fitting heliospheric observations: Numerical investigation of the accuracy of the methods

Transients in the heliosphere, including coronal mass ejections (CMEs) and corotating interaction regions can be imaged to large heliocentric distances by heliospheric imagers (HIs), such as the HIs onboard STEREO and SMEI onboard Coriolis. These observations can be analyzed using different techniques to derive the CME speed and direction. In this paper, we use a three-dimensional (3-D) magneto-hydrodynamic (MHD) numerical simulation to investigate one of these methods, the fitting method of  and . Because we use a 3-D simulation, we can determine with great accuracy the CME initial speed, its speed at 1 AU and its average transit speed as well as its size and direction of propagation. We are able to compare the results of the fitting method with the values from the simulation for different viewing angles between the CME direction of propagation and the Sun-spacecraft line. We focus on one simulation of a wide (120–140°) CME, whose initial speed is about 800 km s⁻¹. For this case, we find that the best-fit speed is in good agreement with the speed of the CME at 1 AU, and this, independently of the viewing angle. The fitted direction of propagation is not in good agreement with the viewing angle in the simulation, although smaller viewing angles result in smaller fitted directions. This is due to the extremely wide nature of the ejection. A new fitting method, proposed to take into account the CME width, results in better agreement between fitted and actual directions for directions close to the Sun–Earth line. For other directions, it gives results comparable to the fitting method of Sheeley et al. (1999). The CME deceleration has only a small effect on the fitted direction, resulting in fitted values about 1–4° higher than the actual values.     

Kappa distribution functions and the main properties of auroral particle acceleration

The problem of auroral particle acceleration is analyzed taking into account the filling of the magnetosphere by accelerated particles of ionospheric origin and the trapping of particles between the magnetic and electrostatic barriers. It is taken into account that kappa distributions describe experimentally measured distribution functions better than do maxwellians. The existence of conjugate field-aligned potential drops in the north and south hemispheres is suggested. Field-aligned potential drops are formed if the value of field-aligned current is higher than the threshold determined by the free gazodynamic flow of electrons along field lines. Results of experimental observations showing the possibility of field-aligned potential drop concentration in double layers are summarized. The theory of kinetic double layers is developed taking into account the nonmaxwellian forms of distribution functions. It is shown that the kinetic treatment and the existence of nonmaxwellian distributions lead to real changes in the criteria required for double-layer formation.     

Synthesis of CME-Associated Moreton and EIT Wave Features from MHD Simulations

Soft X-ray (SXR) waves, EIT waves, and Hα Moreton waves are all associated with coronal mass ejections (CMEs). The knowledge of the characteristics about these waves is crucial for the understanding of CMEs, and hence for the space weather researches. MHD numerical simulation is performed, with the consideration of the quiet Sun atmosphere, to investigate the CME/flare processes. On the basis of the numerical results, SXR, EUV, and Hα images of the eruption are synthesized, where SXR waves, EIT waves, and Hα Moreton waves are identified. It confirms that the EIT waves, which border the expanding dimmming region, are produced by the successive opening (or stretching) of the closed magnetic field lines. Hα Moreton waves are found to propagate outward synchronously with the SXR waves, lagging behind the latter spatially by ～27 Mm in the simulated scenario. However, the EIT wave velocity is only a third of the Moreton wave velocity. The synthesized results also suggest that Hα± 0.45Å would be the best off-band for the detection of Hα Moreton waves.     

Solar filament eruptions and their physical role in triggering coronal mass ejections

Solar filament eruptions play a crucial role in triggering coronal mass ejections (CMEs). More than 80% of eruptions lead to a CME. This correlation has been studied extensively during the past solar cycles and the last long solar minimum. The statistics made on events occurring during the rising phase of the new solar cycle 24 is in agreement with this finding. Both filaments and CMEs have been related to twisted magnetic fields. Therefore, nearly all the MHD CME models include a twisted flux tube, called a flux rope. Either the flux rope is present long before the eruption, or it is built up by reconnection of a sheared arcade from the beginning of the eruption.     

基于MARC的图书发行管理系统的设计与实现

本文探讨了中小型图书发行企业图书发行的基本工作流程,根据工作流程对图书发行管理系统的开发和实现进行了分析,并针对基于MARC数据间的相互转化进行了探讨和研究。     

高层建筑转换层预应力厚板混凝土温度测试裂缝控制技术

通过对预应力转换层厚板混凝土现场温度测试与计算分析,掌握转换板内的混凝土温度、温度应力变化规律,以控制大体积混凝土裂缝的产生.     

构建廊坊市基层群众体育科学管理体制的相关研究

通过对廊坊市现行的基层群众体育管理体制及其运行机制现状的调查,总结廊坊市基层群众体育工作所面临的困难,及其管理体制存在的问题.系统分析与完善各群众体育组织的结构职能,根据社会发展的需要,为廊坊市基层群众体育科学合理管理体制的构建提出合理化建议与参考.     

液体火箭发动机高速采集数据工程数据库设计及应用

叙述了基于SQLSever数据库平台的液体火箭发动机高速采集数据工程数据库的架构设计及海量存储技术在试验数据分析过程中的应用.该数据库对提高数据管理水平、提高数据利用率及发动机的研制具有极大的帮助.数据库的架构设计较好的满足了试车高速采集数据及分析结果的分类存储、检索及查询.海量存储技术的应用解决了非结构化数据的快速存...     

Why should the latitude of the observer be considered when modeling gradual proton events? An insight using the concept of cobpoint

The shape of flux profiles of gradual solar energetic particle (SEP) events depends on several not well-understood factors, such as the strength of the associated shock, the relative position of the observer in space with respect to the traveling shock, the existence of a background seed particle population, the interplanetary conditions for particle transport, as well as the particle energy. Here, we focus on two of these factors: the influence of the shock strength and the relative position of the observer. We performed a 3D simulation of the propagation of a coronal/interplanetary CME-driven shock in the framework of ideal MHD modeling. We analyze the passage of this shock by nine spacecraft located at ∼0.4 AU (Mercury’s orbit) and at different longitudes and latitudes. We study the evolution of the plasma conditions in the shock front region magnetically connected to each spacecraft, that is the region of the shock front scanned by the “cobpoint” (Heras et al., 1995), as the shock propagates away from the Sun. Particularly, we discuss the influence of the latitude of the observer on the injection rate of shock-accelerated particles and, hence, on the resulting proton flux profiles to be detected by each spacecraft.     

月球车牵引力优化控制

月球车的运动控制是月球车完成探测任务的前提．为了解决月球车在月球表面上的运动控制问题,针对月壤环境以及月球车驱动系统冗余的特点,研究月球车闭环协调牵引控制问题．对非结构化环境且轮地之间存在滑移的6轮摇臂悬架月球车进行运动学建模与分析,建立相应的动力学方程以及准静态平衡方程,并使用零空间优化的思想对月球车的力分配进行优化配置,最后给出仿真结果,验证了算法的有效性．