Eruptive prominences as sources of magnetic clouds in the solar wind

Large amounts of coronal material are propelled outward into interplanetary space by Coronal Mass Ejections (CMEs). Thus one might expect to find evidence for expanding flux ropes in the solar wind as well. To prove this assumption magnetic clouds were analyzed and correlated with H-observations of disappearing filaments. When clouds were found to be directly associated with a disappearing filament, the magnetic structure of the cloud was compared with that of the associated filament. Additionally the expansion of magnetic clouds was examined over a wide range of the heliosphere and compared with the expansion observed for erupting prominences.     

Observations of loops and prominences

We review recent observations by the Yohkoh-SXT in collaboration with other spacecraft and ground-based observatories of coronal loops and prominences. These new results point to problems that SoHO will be able to address. With a unique combination of rapid-cadence digital imaging (32 s full-disk and 2 s partial-frame images), high spatial resolution (2.5 arcsec pixels), high sensitivity (EM 10⁴² cm^–3), a low-scatter mirror, and large dynamic range, SXT can observe a vast range of targets on the Sun. Over the first 21 months of Yohkoh operations, SXT has taken over one million images of the corona and so is building up an invaluable long-term database on the large-scale corona and loop geometry. The most striking thing about the SXT images is the range of loop sizes and shapes. The active regions are a bright tangle of magnetic field lines, surrounded by a network of large-scale quiet-Sun loops stretching over distances in excess of 10⁵ km. The cross-section of most loops seems to be constant. Loops displaying significant increase in the ratio of the footpoint to loop-top diameter () are the exception, not the rule, implying the presence of widespread currents in the corona.All magnetic structures show changes. Time scales range from seconds to months. The question of how these structures are formed, become filled with hot plasma, and are maintained is still open. While we see the propagation of brightenings along the length of active-region loops and in X-ray jets with velocities of several hundred km/s, much higher velocities are seen in the quiet Sun. In XBP flares, for example, velocities of over 1000 km/s are common. Active-region loops seem to be in constant motion, moving slowly outward, carrying plasma with them. During flares, loops often produce localized brightenings at the base and later at the apex of the loop. Quiescent filaments and prominences have been observed regularly. Their coronal manifestation seems to be an extended arcade of loops overlying the filament. Reliable alignment of the ground-based data with the X-ray images make it possible to make a detailed intercomparison of the hot and cold plasma structures over extended periods. Hence we are able to follow the long-term evolution of these structures and see how they become destabilized and erupt.     

Orientations of LASCO Halo CMEs and their connection to the flux rope structure of interplanetary CMEs

Coronal mass ejections (CMEs) observed near the Sun via LASCO coronographic imaging are the most important solar drivers of geomagnetic storms. ICMEs, their interplanetary, near-Earth counterparts, can be detected in situ, for example, by the Wind and ACE spacecraft. An ICME usually exhibits a complex structure that very often includes a magnetic cloud (MC). They can be commonly modelled as magnetic flux ropes and there is observational evidence to expect that the orientation of a halo CME elongation corresponds to the orientation of the flux rope. In this study, we compare orientations of elongated CME halos and the corresponding MCs, measured by Wind and ACE spacecraft. We characterize the MC structures by using the Grad–Shafranov reconstruction technique and three MC fitting methods to obtain their axis directions. The CME tilt angles and MC fitted axis angles were compared without taking into account handedness of the underlying flux rope field and the polarity of its axial field. We report that for about 64% of CME–MC events, we found a good correspondence between the orientation angles implying that for the majority of interplanetary ejecta their orientations do not change significantly (less than 45 deg rotation) while travelling from the Sun to the near-Earth environment.     

磁选态单束铯束管束光学参数的模拟计算和设计

为提高铯束管跃迁信号强度,在束光学参数设计中,用蒙特卡罗方法模拟计算铯原子通过率和未跃迁比例。通过改变模拟计算中的束光学参数,分析铯原子通过率、未跃迁比例和倍增器首极电流的变化趋势,得到了主要束光学参数的合理取值范围。在铯束管实际装配和试验中使用束光学参数设计结果,有效地增加了倍增器首极电流。     

环电流区能量离子分布特性研究

为了考察环电流区离子的分布情况,采用环电流粒子理论模式,对环电流中10-100 keV的离子进行了模拟研究.这个模式能够根据近地注入区外边界处离子的分布函数得出磁暴主相期间环电流中的主要成分H+,O+,He+3种离子的通量分布.计算结果分析表明,在其他条件相同的情况下,不同种类离子的通量分布的形态结构十分相似.电场强度对环电流离子通量的空间分布具有决定性的作用;晨昏电场强度越强,离子的通量越高;晨昏电场越强,环电流离子的内边界越接近地球.10keV的离子在电场相当弱的时候还是存在着连续的通量分布,但他们的形态和结构随着电场的变化有明显的变化.电场很弱时,离子分布主要集中于内外两个环带,离子通量在晨侧的更多一些,离子通量的最大值基本上是在比较靠近地球的环带上;随着电场的增强,离子分布的内外两个环带逐步合并,离子的分布逐渐靠近地球,通量分布的最大值也移动到了昏侧.环电流离子投掷角分布具有各向异性,投掷角在90°左右的时候,离子通量能达到最大值.      

隐式无网格算法及其应用研究

本文的主要目的在于研究求解Euler方程的隐式无网格算法，并应用于复杂的流场计算。采用无网格算法，计算区域用点云离散代替通常的网格划分；计算点上的空间导数，用当地点云上引入的二次极小曲面逼近。求解的Euler方程用隐式时间后差离散，结合用Roe的近似Riemann解确定通量，并用LU－SGS算法分步计算，数值求解了单翼型或双翼型模拟的复杂绕流。     

稳态等离子体推力器磁场设计与数值分析

首先分析了稳态等离子体推力器性能对磁场的要求，据此介绍了磁路系统的工程设计原则和方法；然后，采用ANSYS大型有限元分析软件对一个具体的稳态等离子体推力器在额定工况下的磁场进行了计算，获得了满意的结果，通过对结果的分析获得了对有关现象的直观深入的认识，为所计算具体推力器的改进设计提供了线索；同时，也证实了以ANSYS为软件平台的稳态等离子体推力器磁路系统计算机数值仿真辅助设计的可行性和有效性。     

3He原子磁强计技术

~3He原子磁强计利用~3He核自旋的拉莫尔进动测量磁场,具有高精度、小体积等特点,可以满足未来网络化磁异常探测对高性能磁强计的需求。围绕~3He原子磁强计的技术特点,重点介绍了该磁强计的基本工作原理及其硬件组成,分析了其理论灵敏度,给出了该磁强计的国内外研究情况,最后对该磁强计技术的未来发展进行了展望。     

无网格法耦合RNG k-ε湍流模型在亚、跨声速翼型黏性绕流中的数值模拟

基于移动最小二乘无网格方法,耦合RNG(Re-Normalisation Group)k-ε湍流模型求解雷诺平均Navier-Stokes方程。采用AUSM(Advection Upstream Splitting Method)+-up迎风格式求解数值通量,应用在高度各向异性点云结构中取得良好结果的点云重构技术结合移动最小二乘法拟合空间导数,并用三阶SSP(Strong Stability Preserving)型Runge-Kutta显式时间推进格式求解离散后的控制方程。在此基础之上,实现了对NACA0012、RAE2822翼型亚、跨声速黏性绕流的数值模拟,给出了翼型表面压力系数分布曲线、不同位置处的平均速度剖面、马赫数等值线等计算结果,并与实验值及相关文献数值模拟结果进行比较,结果吻合较好。表明所发展的结合点云重构技术的无网格方法耦合RNGk-ε湍流模型能够成功模拟翼型亚、跨声速黏性绕流,验证了所提算法的有效性,并拓展了无网格方法求解湍流流动的途径。