挠性卫星大角度机动变结构控制的全物理仿真实验研究

以具有大面积太阳帆板的卫星大角度机动为背景，针对常用的“飞轮－喷气”执行机械模式研究了变结构控制方案，考虑了控制精度和喷气消耗量问题，并成功地进行了国内首次挠性卫星大角度机动控制的全物理仿真实验，取得了显著的效果。     

基于Lyapunov方法的空间飞行器大角度姿态机动控制

本文研究空间飞行器大角度资态机动的控制问题，为了克服大角度机动时使用欧拉角可能产生的奇异问题，文中使用四元参形式的微分方程来描述飞行器的运动，飞行器的动力学方程具有不确定性和非线性。本文应用Lyapunov方法设计在大角度姿态机动控制器，这个控制器具有按指数规律变化的增益，它大大减小了对初始力矩的要求，最后，本文给出一个例子来说明所导出的控制器的优点。     

放置倾角对轴向槽道热管传热特性影响的实验研究

对常温梯形轴向槽道热管在不同放置倾角下的传热特性进行了实验研究，着重分析了热管的放置倾角对轴向温度分布、最大轴向温差、总热阻、当量换热系数、最大传热量的影响，旨在为航空热管的地面性能测试提供参考。实验结果表明：热源在下垂直放置热管的蒸发段和冷凝段的当量换热系数分别是水平放置热管的1．5倍和2．5倍。热源在上倾斜放置的热管，水平放置的热管、热源在下倾斜放置的热管的平均总热阻成一个数量级递减，蒸发段的最大输入热流量依次递增一个数量级。     

子午面太阳风结构及其对日冕抛射物运动的影响

本文提出了一种求解二维理想磁流体力学方程组的组合格式-网格方法。该方法在保证一定精度的前提下稳定性好,计算量小。文中使用该方法算得了子午面太阳风的盔状流动解。以该解作为初态,研究了盔状冕旒位形对日冕抛射物运动的影响,发现该位形使得抛射物向低纬赤道方向偏转,较好地解释了观测结果。     

日地共转扰动似稳结构及其反相和漂移规律的最新证据

日地共转扰动似稳结构及其反相现象在第２１及２２周再次显现，从而证实了上述发现是一种在长达世记的时间尺度内存在的普遍规律。包括１９９１－１９９２年内的百年地磁扰动资料还说明偶数太阳周的共转似稳结构扰动峰有逆太阳自转而线性性漂移的趋向。对即将来临的极小年前可能出现的共转扰动作了试验性的预测。     

一种获取耀斑光变曲线的高精度,高分辨方法

一种获取耀斑光变曲线的高精度、高分辨方法栗志，周卫红（中国科学院云南天文台，昆明６５００１１）关键词太阳耀斑，光变曲线，测量方法太阳耀斑物理机制的研究，需要得到耀斑核的辐射的演化，在光学波段常用耀斑在单色光的辐射强度的时间变化曲线作为分析依据［１］．...     

On the correlation of the solar wind observed at the L5 point and at the Earth

The L5 point is a promising location for forecasting co-rotating high-speed streams in the solar wind arriving at the Earth. We correlated the solar wind data obtained by the Nozomi spacecraft in interplanetary space and by the Advanced Composition Explorer (ACE) at the L1 point, and found that the correlation is significantly improved from that of the 27-day recurrence of ACE data. Based on the correlation between the two spacecraft observations, we estimated the correlation of the solar wind velocity between the L5 point and at the Earth, and found that the correlation coefficient was about 0.78 in late 1999, while that of the 27-day recurrence was 0.51. Eighty-eight percent of the velocity difference falls within 100 km/s between the L5 point and the Earth. This demonstrates the potential capability of solar wind monitoring at the L5 point to forecast the geomagnetic disturbances 4.5 days in advance.     

Chromospheric line emission in seismically active flares

Some flares are known to drive seismic transients into the solar interior. The effects of these seismic transients are seen in helioseismic observations of the Sun’s surface thousands of km from their sources in the hour succeeding the impulsive phase of the flare. Energetic particles impinging from the corona into the chromosphere are known to drive strong, downward-propagating shocks in active region chromospheres during the impulsive phases of flares. H observations have served as an important diagnostic of these shocks, showing intense emission with characteristic transient redshifts. In most flares no detectable transients penetrate beneath the active region photosphere. In those that do, there is a strong correlation between compact white-light emission and the signature of seismic emission. This study introduces the first known H observations of acoustically active flares, centered in the core of the line. The morphology of line-core emission H in the impulsive phase of the flare is similar to that of co-spatial line-core emission in NaD₁, encompassing the site of seismic emission but more extended. The latter shows a compact red shift in the region of seismic emission, but a similar feature is known to appear in a conjugate magnetic footpoint from which no seismic emission emanates. Radiative MHD modelling based on the profiles of chromospheric line emission during the impulsive phases of flares can contribute significantly to our understanding of the mechanics of flare acoustic emission penetrating into the solar interior and the conditions under which it occurs.     

Relationships between energetic storm particle events and interplanetary shocks driven by full and partial halo coronal mass ejections

We have analysed energetic storm particle (ESP) events in 116 interplanetary (IP) shocks driven by front-side full and partial halo coronal mass ejections (CMEs) with speeds $>$400 km s^?1during the years 1996–2015. We investigated the occurrence and relationships of ESP events with several parameters describing the IP shocks, and the associated CMEs, type II radio bursts, and solar energetic particle (SEP) events. Most of the shocks (57 %) were associated with an ESP event at proton energies $>$1 MeV.The shock transit speeds from the Sun to 1 AU of the shocks associated with an ESP event were significantly greater than those of the shocks without an ESP event, and best distinguished these two groups of shocks from each other. The occurrence and maximum intensity of the ESP events also had the strongest dependence on the shock transit speed compared to the other parameters investigated. The correlation coefficient between ESP peak intensities and shock transit speeds was highest (0.73 $\pm$ 0.04) at 6.2 MeV. Weaker dependences were found on the shock speed at 1 AU, Alfvénic and magnetosonic Mach numbers, shock compression ratio, and CME speed. On average all these parameters were significantly different for shocks capable to accelerate ESPs compared to shocks not associated with ESPs, while the differences in the shock normal angle and in the width and longitude of the CMEs were insignificant.The CME-driven shocks producing energetic decametric–hectometric (DH) type II radio bursts and high-intensity SEP events proved to produce also more frequently ESP events with larger particle flux enhancements than other shocks. Together with the shock transit speed, the characteristics of solar DH type II radio bursts and SEP events play an important role in the occurrence and maximum intensity of ESP events at 1 AU.     

平流层飞艇的能源技术和平衡分析

平流层飞艇作为近空间对地观测平台的一种实现方案，主要依靠自身庞大体积产生的静浮力而不像其它飞行器依靠相对空气运动产生升力，所以飞艇能够以较慢的速度飞行甚至能够在空中长期保持定点悬停即相对地面静止。具有长时间在平流层自主飞行的能力，是平流层飞艇设计的一个重要目标。文章对平流层飞艇能源系统的构成、部件及能源平衡分析方法作了介绍。