CMEs and active regions on the sun

The relationship between active regions (ARs) and coronal mass ejections (CMEs) is studied. For this purpose a statistical analysis of 694 CMEs associated with ARs was carried out. We considered the relationship between properties of the CMEs and ARs characterized using the McIntosh classification. We demonstrated that CMEs are likely to be launched from ARs in the mature phase of their evolution when they have complex magnetic field. The fastest and halo CMEs can be ejected only from the most complex ARs (when an AR is a bipolar group of spots with large asymmetric penumbras around the main spot with many smaller spots in the group). We also showed that the wider events have a tendency to originate from uncomplicated magnetic structures. This tendency was used for estimation of the real angular widths of the halo CMEs. The probability of launching of fast CMEs increases together with increase of the complexity and size of ARs. The widest, but slow, CMEs originate from the simplest magnetic structure which are still able to produce CMEs. Our results could be useful for forecasting of space weather.     

Cut-off features in interplanetary solar radio type IV emission

Solar radio type IV bursts can sometimes show directivity, so that no burst is observed when the source region in located far from the solar disk center. This has recently been verified also from space observations, at decameter wavelengths, using a 3D-view to the Sun with STEREO and Wind satellites. It is unclear whether the directivity is caused by the emission mechanism, by reduced radio wave formation toward certain directions, or by absorption/blocking of radio waves along the line of sight. We present here observations of three type IV burst events that occurred on 23, 25, and 29 July 2004, and originated from the same active region. The source location of the first event was near the solar disk center and in the third event near the west limb. Our analysis shows that in the last two events the type IV bursts experienced partial cut-offs in their emission, that coincided with the appearance of shock-related type II bursts. The type II bursts were formed at the flanks and leading fronts of propagating coronal mass ejections (CMEs). These events support the suggestion of absorption toward directions where the type II shock regions are located.     

用于量子保密通信系统的偏振控制算法研究

量子保密通信是近年来逐渐发展成熟的一种新型保密通信机制,其安全性建立在量子力学基本原理上,被证明具有信息论条件下的绝对安全性。偏振编码光纤量子保密通信系统使用光子的偏振态进行信息编码。当环境变化时,光纤传输特性的改变将导致光子偏振态变化。因此,光子偏振态的补偿控制是光纤量子保密通信系统的一项关键技术,能否快速、准确的对偏振态进行补偿将直接影响系统的通信性能。本文提出一种基于光纤偏振控制器和扫描控制算法的偏振补偿方案。该方案通过控制光纤偏振控制器的电压大小,将量子误码率最小化,实现偏振光的补偿控制,满足量子通信系统自动控制的要求。     

"动中通"系统中极化角的计算

根据"动中通"卫星移动通信中极化角计算的情况,分析了极化角的产生机理,并详细推导了其计算公式.在"动中通"系统实际应用中,由于载体位置不断发生改变,极化角随之改变.本文进一步推导了极化角的补偿算法,为工程应用提供了理论参考,并且已经在"动中通"系统中取得较好的应用效果.     

星载光学遥感系统偏振耦合误差分析与修正方法研究

星载遥感器偏振灵敏度带来的偏振测量误差会影响获取数据的准确性,该误差作为系统误差将直接影响到数据应用.文章采用矢量辐射传输模型模拟遥感器(以中等分辨率成像光谱仪为例)入瞳处信号偏振与遥感器偏振耦合特性,分析了遥感器偏振灵敏度分别为2%、5%、7%时,遥感系统的测量误差分布情况,发现偏振耦合误差直接影响获取数据的真实性和...     

PROGRESS IN HELIOSPHERIC PHYSICS

This is an overview of progresses in heliospheric physics made in China in the period of June, 2000 to May, 2002. The report is focused on theoretical studies,modelling and observational analysis of interplanetary physical phenomena, and consists of five sections: the acceleration and heating of the solar wind, corona structures, coronal mass ejections, magnetic reconnection phenomena, and in terplanetary transient phenomena. The main achievements made recently by Chinese scientists in related areas are simply listed in corresponding sections without any priority, only certain editorial consideration.     

磷化底漆与阿洛丁化学转化膜耐蚀性能的对比研究

通过电化学阻抗谱和恒电位稳态阳极极化曲线2种电化学测试方法,对磷化底漆和阿洛丁化学转化膜进行了测试,发现磷化底漆的耐蚀性明显优于阿洛丁化学转化膜,其极化电阻RP比阿洛丁转化膜高一个数量级,钝化区电位范围在-0.75～ 1.0V之间,而阿洛丁化学转化膜钝化区电位范围明显偏低,在-2.0～0.00V之间。     

偏振稳定器的理论分析与实验研究

对于高速率(40Gb／s以上)的光纤通信系统，其偏振相关特性显得尤为重要。推导并验证了偏振控制器的琼斯矩阵及穆勒矩阵，对于任意输入光偏振态，实验得到了任意希望输出的偏振态。分析并设计了以偏振控制器为核心器件的偏振稳定器，通过实时地控制偏振控制器．使稳定器输出端的偏振态不随输入端偏振态的扰动而改变，并且不受环境因素的干扰。     

Relation between solar wind velocity and properties of its source region

Different kinds of coronal holes are sources of different kind of solar winds. A successful solar wind acceleration model should be able to explain all those solar winds. For the modeling it is important to find a universal relation between the solar wind physical parameters, such as velocity, and coronal physical parameters such as magnetic field energy. To clarify the physical parameters which control the solar wind velocity, we have studied the relation between solar wind velocity and properties of its source region such as photospheric/coronal magnetic field and the size of each coronal hole during the solar minimum. The solar wind velocity structures were derived by using interplanetary scintillation tomography obtained at Solar-Terrestrial Environment Laboratory, Japan. Potential magnetic fields were calculated to identify the source region of the solar wind. HeI 1083 nm absorption line maps obtained at Kitt Peak National Solar Observatory were used to identify coronal holes. As a result, we found a relation during solar minimum between the solar wind velocity and the coronal magnetic condition which is applicable to different kind of solar winds from different kind of coronal holes.     

Heliosphereic Physics Research in China:2002-2003

This brief report summarized the latest advances of the heliospheric physics research in China during the period of 2002-2003, made independently by Chinese space physicists and through international collaboration. The report covers all aspects of the heliospheric physics, including theoretical studies, numerical simulation and data analysis.