Research on a complex CME event including Hα, LASCO, radio and MDI observations

We present our research on a fast and decelerating partial halo coronal mass ejection (CME) event detected in multi-wavelengths in the chromosphere and the corona on 14 October, 1999. The event involved a whole complex active area which spanned more than 40° of heliolongitude. It included a strong solar flare (XI/1N) and a complex eruptive filament within an active region of the entire complex. Especially, several radio sources were detected in the decimetric range prior to the CME by the Nançay Radioheliograph (NRH). A linear force-free field extrapolation of the Michelson Doppler Imager (MDI) magnetogram was performed to calculate the magnetic topology of the complex prior to the triggering of the event. The presence of a coronal null point combined with the occurrence of two distant and nearly simultaneous radio sources put strong arguments in favor of the generalized breakout model for the triggering of the eruption. The analysis of the subsequent development of the event suggests that large interconnecting loops were ejected together with the CME.     

水基有机硅憎水剂对A3钢憎水处理的应用

以市售聚硅氧烷乳液为基料,辅以金属盐催化剂和醇胺类改性植酸水溶性缓蚀剂制备的水溶性有机硅憎水剂,用以处理A3钢磷化试样表面.考察了催化剂质量分数、植酸质量分数、植酸溶液的pH值、乳液与改性植酸的比率对憎水剂憎水处理效果及稳定性的影响;探讨了不同热处理温度、浸渍时间及热处理时间等工艺条件下憎水剂对金属表面憎水性的影响并确定了憎水剂配方和憎水处理工艺.结果表明,用该憎水剂处理的A3钢磷化试样接触角可达132°左右,A3钢磷化处理表面的耐腐蚀性能得到明显改善.      

太阳电池阵极月轨道在轨热分析

以极月轨道上太阳电池阵作为研究对象,详细分析了该轨道上电池阵所得各外热流的确定方法.以此为基础,对太阳电池阵进行在轨温度数值模拟,得到月球轨道上电池阵所得外热流以及温度的周期分布.计算结果与地球卫星的相应数据进行比较,明确了月球轨道上电池阵所得外热流以及温度的周期分布特点,为月球卫星上太阳电池阵以及整个卫星的设计提供了有利的数据参考.      

后掠翼对细长体中段大迎角绕流的影响

采用在细长体顶点处添加扰动块的方式使细长体的绕流具有确定性.研究了在大迎角下,后 掠翼对细长体绕流结构和气动力特性的影响.实验结果表明,在30°迎角时,细长体中段背 风侧的流动和压力分布受到后掠翼与头部背涡的双重控制.在迎角α=40°~60°范围内 , 后掠翼对细长体中段绕流起主控作用,使细长体中段背风侧流动呈现完全分离流状态,使得 中段背风侧的压力分布保持为均值.      

接触角法测玄武岩及玻璃纤维表面能实验

通过Wilhelmy吊片法测试液体与玄武岩、玻璃纤维单丝的前进接触角,应用OWRK理论计算得到纤维表面能及其色散与极性分量.实验研究表明:未经表面处理的玄武岩纤维表面能高于S-2玻璃纤维,去除浸润剂后2种纤维表面能的极性分量均明显降低,并且测试液体的极性分量对纤维表面能的测试结果影响甚大.分析结果为纤维与树脂的表面张力合理匹配、形成良好界面浸润和粘接提供了理论依据.      

Sharp boundaries of solar wind plasma structures and their relationship to solar wind turbulence

Sharp (<10 min) and large (>20%) solar wind ion flux changes are common phenomena in turbulent solar wind plasma. These changes are the boundaries of small- and middle-scale solar wind plasma structures which can have a significant influence on Earth’s magnetosphere. These solar wind ion flux changes are typically accompanied by only a small change in the bulk solar wind velocity, hence, the flux changes are driven mainly by plasma density variations. We show that these events occur more frequently in high-density solar wind. A characteristic of solar wind turbulence, intermittency, is determined for time periods with and without these flux changes. The probability distribution functions (PDF) of solar wind ion flux variations for different time scales are calculated for each of these periods and compared. For large time scales, the PDFs are Gaussian for both data sets. For small time scales, the PDFs from both data set are more flat than Gaussian, but the degree of flatness is much larger for the data near the sharp flux change boundaries.     

SOME RESULTS OF UPPER ATMOSPHERIC COMPOSITION MEASUREMENTS BY A MASS-SPECTROMETER ON BOARD "SZ-2":CHANGE OF COMPOSITIONS DURING SOLAR AND GEOMAGNETIC DISTURBANCES

Upper atmosphere composition data were obtained for the last half year with a quadruple mass spectrometer on board spacecraft "SZ-2" launched on 10 Jan uary 2001. Based on the analysis of these data, the variations of atmospheric compositions in solar and geomagnetic quiet conditions are reported first, then a detailed discussion on the atmospheric composition variations under the so lar and geomagnetic disturbed conditions is given. The results show that near the altitude of 400 km the variations of main atmospheric compositions corre sponding to solar disturbances are more remarkable in the sunlit area than in the shade area. On the contrary, in geomagnetic disturbance events the corre sponding variations are more obvious in the shade area, an evident increase of N2 density at relatively higher latitudes was observed.     

单流体二维太阳风结构的磁流体力学模拟

在添加动量项的条件下，对单流体二维磁流体力学方程组进行模拟，得到了子午面上的太阳风结构，结果表明，添加动量项的形式及其被加入的位置对远区太阳风速度和质子密度有重要的影响。本文在适当的区域加入合适的动量项得出了远区太阳风速和质子密度与Ulysses观测基本符合的结果。文中给出了较合适的动量添加区域为3.5-10Rs(Rs为太阳半径）。     

"神舟二号"大气密度探测器的探测结果Ⅱ.在太阳和地磁扰动期间高层大气密度的变化

选用了Sz—2大气密度探测器在2001年2—4月间的探测数据,进行日照和阴影区域热层大气密度对太阳和地磁活动程度的响应变化的探讨．结果表明,日照区大气密度峰值主要随F10.7值而变,在地磁扰动期间,阴影区大气密度对扰动的响应更明显,通常响应变化开始于高纬度地区,然后向低纬度地区推移．     

神经网络方法在太阳质子事件短期预报中的应用

在大量统计结果的基础上,深入研究了太阳质子事件预报机理．总结了质子事件爆发与太阳活动区面积、位置、McIntosh结构、磁结构以及前两天活动区爆发耀斑事件数目之间的关系．然后,在神经网络的基础上建立了太阳质子事件短期预报模型,并对2000年以后12个未参加训练的样本进行测试,结果对事件预报的准确率为83％．此外,我们还利用该模型对2002年1-4月发生的几次质子事件进行了预报试验,结果发现,这期间发生的6次事件都被预报．其中3次质子事件系统预报提前了3天,两次事件预报提前了2天,一次事件提前1天预报．