FY-1C在地表灾情和环境监测中的应用

介绍了国家气象中心一年来利用FY-1C极轨气象卫星开展地表监测和环境监测包括火情监测、水情监测、积雪监测、海冰监测及植被监测的情况。指出由于该卫星探测通道比美国NOAA卫星多、过境时机适宜，因而在气象卫星应用于地表灾情和环境监测方面具有明显的优势。     

地球同步轨道卫星编队飞行的区域性导航系统方案

卫星编队飞行组成虚拟平台 ,这是当前一个完全崭新和开拓性的研究课题。根据与时俱进 ,开拓创新的精神 ,本文提出一个地球同步轨道卫星编队飞行组成的区域性导航系统方案。这是至今为止在相同精度和相同覆盖区条件下卫星数量最少的 ,也是投资经费最低的导航系统方案     

Closing address

Impressions from the workshop are summarized. Difficulties within the present observational and theoretical context are outlined and directions for fruitful future work are indicated. The workshop subtitle, the interface between MHD and plasma physics, still appears to be a goal for the future, though some encouraging results have been reported at this workshop.     

高速数据总线研究

通过对美国军用标准MIL-STD-1553 B总线协议在高速数据通讯中受到限制的分析,提出了现实解决办法。利用同步信号检出电路的改进和微程序控制器工作模式变化,使码速率提高一倍。上述两种技术的应用较好地解决了计算机高速处理能力和高速信息传输介质之间的瓶颈问题。     

1990年7月30日太阳射电大爆发中的脉动现象

本文讨论了1990年7月30日伴随日面2B级双带光学耀斑发生的3.2cm波微波大爆发事件的观测特征,它呈现为显著的脉动形态。并对它进行了数据处理,发现射电爆发流量S与脉动的特征参量:平均重复率R,调制度△S/S和能量△E之间有良好的统计相关性。对此作了讨论和初步的解释。     

What is the role of magnetic null points in large flares?

We have performed the analysis of the magnetic topology of active region NOAA 10486 before two large flares occurring on October 26 and 28, 2003. The 3D extrapolation of the photospheric magnetic field shows the existence of magnetic null points when using two different methods. We use TRACE 1600 Å and 195 Å brightenings as tracers of the energy release due to magnetic reconnections. We conclude on the three following points:

1. The small events observed before the flares are related to low lying null points. They are long lasting and associated with low energy release. They are not triggering the large flares.

2. On October 26, a high altitude null point is found. We look for bright patches that could correspond to the signatures of coronal reconnection at the null point in TRACE 1600 Å images. However, such bright patches are not observed before the main flare, they are only observed after it.

3. On October 28, four ribbons are observed in TRACE images before the X17 flare. We interpret them as due to a magnetic breakout reconnection in a quadrupolar configuration. There is no magnetic null point related to these four ribbons, and this reconnection rather occurs at quasi-separatrix layers (QSLs).

We conclude that the existence of a null point in the corona is neither a sufficient nor a necessary condition to give rise to large flares.     

From solar nanoflares to stellar giant flares: Scaling laws and non-implications for coronal heating

In this study we explore physical scaling laws applied to solar nanoflares, microflares, and large flares, as well as to stellar giant flares. Solar flare phenomena exhibit a fractal volume scaling, V(L)  L^1.9, with L being the flare loop length scale, which explains the observed correlation between the total emission measure EM_p and flare peak temperature T_p in both solar and stellar flares. However, the detected stellar flares have higher emission measures EM_p than solar flares at the same flare peak temperature T_p, which can be explained by a higher electron density that is caused by shorter heating scale height ratios s_H/L ≈ 0.04–0.1. Using these scaling laws we calculate the total radiated flare energies E_X and thermal flare energies E_T and find that the total counts C are a good proxy for both parameters. Comparing the energies of solar and stellar flares we find that even the smallest observed stellar flares exceed the largest solar flares, and thus their observed frequency distributions are hypothetically affected by an upper cutoff caused by the maximum active region size limit. The powerlaw slopes fitted near the upper cutoff can then not reliably be extrapolated to the microflare regime to evaluate their contribution to coronal heating.     

稀土永磁方波无刷直流电动机调速系统的实验研究

稀土永磁方波无刷直流电动机是静止功率变换器和电机设计相结合的产物，本文分析了稀土永磁方波无刷直流电动机的控制性能，指出它具有电机磁定向控制简化为磁极位置控制的特点，从而控制简单又提高控制性能，为此在稀土永磁方波无刷直流电动机调速系统中，采用了两态稳频电流调节器，ＰＷＭ电子换向器，电流分时反馈等具有特色的线路设计，实验结果表明，该调速系统体现了静止功率变换器与电机配合运行的特点，验证了稀土永磁方波无     

“Oblique” Bernstein modes in solar preflare plasma: Generation of second harmonics

Process of second harmonics generation due to development of corresponding instability has been investigated for pure electron weakly oblique Bernstein mode. This mode was supposed to be modified by taking into account the influence of pair Coulomb collisions and weak large-scale electric field in flare loop. Investigated area was located near the loop foot-point in the “lower–middle” chromosphere of active region. It has been shown, that for the Fontenla–Avrett–Loeser model of solar atmosphere the investigated process of second harmonics generation starts at the extremely low threshold values of subdreicer electric field, well before the beginning of “preheating” phase of flare process.     

Three-dimensional global simulation of multiple ICMEs’ interaction and propagation from the Sun to the heliosphere following the 25–28 October 2003 solar events

This study performs simulations of interplanetary coronal mass ejection (ICME) propagation in a realistic three-dimensional (3D) solar wind structure from the Sun to the Earth by using the newly developed hybrid code, HAFv.2+3DMHD. This model combines two simulation codes, Hakamada–Akasofu–Fry code version 2 (HAFv.2) and a fully 3D, time-dependent MHD simulation code. The solar wind structure is simulated out to 0.08 AU (18 Rs) from source surface maps using the HAFv.2 code. The outputs at 0.08 AU are then used to provide inputs for the lower boundary, at that location, of the 3D MHD code to calculate solar wind and its evolution to 1 AU and beyond. A dynamic disturbance, mimicking a particular flare’s energy output, is delivered to this non-uniform structure to model the evolution and interplanetary propagation of ICMEs (including their shocks). We then show the interaction between two ICMEs and the dynamic process during the overtaking of one shock by the other. The results show that both CMEs and heliosphere current sheet/plasma sheet were deformed by interacting with each other.