Real-Time Specifications of the Geospace Environment

We report the recent progress in our joint program of real-time mapping of ionospheric electric fields and currents and field-aligned currents through the Geospace Environment Data Analysis System (GEDAS) at the Solar-Terrestrial Environment Laboratory and similar computer systems in the world. Data from individual ground magnetometers as well as from the solar wind are collected by these systems and are used as input for the KRM and AMIE magnetogram-inversion algorithms, which calculate the two-dimensional distribution of the ionospheric parameters. One of the goals of this program is to specify the solar-terrestrial environment in terms of ionospheric processes, providing the scientific community with more than what geomagnetic activity indices and statistical models provide. This revised version was published online in August 2006 with corrections to the Cover Date.     

Modelling of the electromagnetic field in the interplanetary space and in the Earth's magnetosphere

A magnetohydrodynamic model of the solar wind flow is constructed using a kinematic approach. It is shown that a phenomenological conductivity of the solar wind plasma plays a key role in the forming of the interplanetary magnetic field (IMF) component normal to the ecliptic plane. This component is mostly important for the magnetospheric dynamics which is controlled by the solar wind electric field. A simple analytical solution for the problem of the solar wind flow past the magnetosphere is presented. In this approach the magnetopause and the Earth's bow shock are approximated by the paraboloids of revolution. Superposition of the effects of the bulk solar wind plasma motion and the magnetic field diffusion results in an incomplete screening of the IMF by the magnetopause. It is shown that the normal to the magnetopause component of the solar wind magnetic field and the tangential component of the electric field penetrated into the magnetosphere are determined by the quarter square of the magnetic Reynolds number. In final, a dynamic model of the magnetospheric magnetic field is constructed. This model can describe the magnetosphere in the course of the severe magnetic storm. The conditions under which the magnetospheric magnetic flux structure is unstable and can drive the magnetospheric substorm are discussed. The model calculations are compared with the observational data for September 24–26, 1998 magnetic storm (Dst _min=−205 nT) and substorm occurred at 02:30 UT on January 10, 1997. This revised version was published online in August 2006 with corrections to the Cover Date.     

高空台间接加热试验

用同一种发动机在不同模拟状态下，采用技改措施及加热器的火焰筒不同个数进行了试验，获得了模拟温度、气源压力与时间的关系。设备的总压系数为0．67；加热系统的总效率为0．41－0．55。与另一高空台使用同一间接加热系统的总效率（约为0．62）相比有所不同。分析了原因，并指出了解决问题的途径。上述试验方法及试验结果可供类拟发动机试验参考使用。     

高温相变单元管蓄热过程数值模拟

对以高温共晶盐 Li F-Ca F2 为相变材料 (PCM)和以干空气为工质的相变蓄热系统 ,采用焓方法建立了以控制体单元为对象的单管相变蓄热模型。在模拟空间站太阳能吸热 /储热器轨道运行参数下进行了数值计算。计算结果与地面模拟试验数据进行了比较 ,吻合良好。     

Composition Variations in the Solar Corona and Solar Wind

Order of magnitude variations in relative elemental abundances are observed in the solar corona and solar wind. The instruments aboard SOHO make it possible to explore these variations in detail to determine whether they arise near the solar surface or higher in the corona. A substantial enhancement of low First Ionization Potential (FIP) elements relative to high FIP elements is often seen in both the corona and the solar wind, and that must arise in the chromosphere. Several theoretical models have been put forward to account for the FIP effect, but as yet even the basic physical mechanism responsible remains an open question. Evidence for gravitational settling is also found at larger heights in quiescent streamers. The question is why the heavier elements don't settle out completely. This revised version was published online in June 2006 with corrections to the Cover Date.     

UVCS/SOHO Observations of Spectral Line Profiles in Polar Coronal Holes

Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights ? (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for ? = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at ? = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at ? = 1.34, but are significantly larger at ? = 1.5 and much larger for ? > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least ? = 2.0, but never reach the values of O VI.     

气相爆轰波传播特性的数值模拟及实验对照

本文应用基元反应模型和频散可控耗散格式(DCD)对氢氧爆轰波进行了二维数值模拟.氢氧混合物的化学反应模型考虑了8种组分20个反应方程式.在处理化学反应引起的刚性问题时采用了时间算子分裂的方法.本文首先对爆轰波数值结果和实验结果进行了对照验证,然后对爆轰波在楔面反射由马赫反射向规则反射转变的过程进行了数值分析,得到了反射转变临界角,并和实验结果及理论分析进行了比较,结果是令人满意的;本文还对爆轰波的多波结构进行了初步的数值分析.     

用胞映射法分析双线性结构刚度的机翼颤振

将映射轨迹追踪技术引入基于空间Poincar啨截面的胞映射方法中 ,并定义初值分析空间 ,以适应分析高维动力系统运动类型初值域的需要。改进后胞空间中胞的数目大大减少 ,计算时间缩短 ,运动特征的确认更为准确。应用该方法研究扭转方向具有双线性结构刚度因素的机翼颤振问题 ,结果显示 ,初始条件对系统动力学行为有着很大的影响。当两段刚度之比小于某临界值时 ,随着机翼颤振速度增大 ,不同的初始条件会导致平衡点、极限环振动、复杂的周期运动、混沌和发散运动等不同的运动形式     

三维四向编织复合材料等效热特性数值分析和试验研究

 采用“米”字型枝状胞体有限元模型和试验方法对三维四向编织复合材料的整体等效热膨胀系数和等效热传导系数进行了分析并将计算结果和试验值进行了比较。研究表明枝状胞体模型能较为真实的反映三维四向编织复合材料的结构构形;有限元方法在分析热膨胀、热传导方面具有较好的精度;三维四向编织复合材料编织方向的热膨胀系数随着纤维体积比的增加而减小,随着编织角的增加而减小;热传导系数随着纤维体积比的增加而增大,随着编织角的增大而增大。     

太阳能火箭发动机聚光器设计方法

对工程上常用聚光器进行了性能比较,得出了适合于太阳能火箭发动机(STP)的聚光器及其具有的性能优点,研究了此种聚光器的的设计方法,并推出了相关公式和其中的关键技术,这对STP聚光器的工程设计具有重要的指导价值。