冕环中扭转Alfvén波和快波的耦合共振

推广完备正交函数系(OFSE)展开方法,应用它研究冕环中无耗散扭转Alfven波和快波耦合的时变过程.采用这种方法,从数学上描述了总体波模的固有角频率,从理论和数值计算结果两方面分析了Alfven波和快波耦合时冕环中磁力线Alfven波固有角频率.采用这种方法,分析了耦合驱动项和Alfven波共振的关系.计算结果给出了耦合共振出现位置Alfven波和快波的波幅特征,发现如果足点驱动角频率不等于冕环总体波模的固有角频率,在耦合共振位置当扭转Alfven波幅出现δ断面时,快波振幅沿径向梯度很大,有时近似为一个间断,非常有利于快波耗散;如果足点驱动角频率等于总有体波模的固有角频率,Alfvn波振幅出现δ断面时在径向出现丰富的小尺度结构,共振位置近似为一个间断,非常有利于Alfven波耗散.     

Wind asymmetries in massive stars

We are in the process of surveying the linear polarization in luminous, early-type stars. We here report on new observations of the B [e] stars S 18 and R 50, and of the Luminous Blue Variables HR Car, R 143, and HD 160529. Together with previously published data, these observations provide clear evidence for the presence of intrinsic polarization in 1 B[e] star (HD 34664) and in 5 LBVs ( Car, P Cyg, R 127, AG Car, and HR Car). The data indicate that anisotropic stellar winds are a common occurrence among massive stars in these particular evolutionary stages. For such stars, mass-loss rates estimated using the assumption of a spherical, homogeneous and stationary outflow may be in error.     

10 Gbit/s伪随机序列光纤通信系统PMD补偿

光纤通信线路检测到的电功率随差分群延迟变化,可作为PMD补偿的反馈控制信号。给出了这一变化关系的理论计算和曲线并通过实验验证这一关系,确定电压信号与DGD的变化关系。建立了一套完整的实验系统,并考虑了影响反馈电压信号的多种因素以及减小这些影响的措施。通过眼图给出的实验结果说明了补偿的效果,还通过误码测试仪测量了补偿前后的接收灵敏度的改变以定量说明补偿的效果,最后比较了不同情况下的补偿结果。     

Orientations of LASCO Halo CMEs and their connection to the flux rope structure of interplanetary CMEs

Coronal mass ejections (CMEs) observed near the Sun via LASCO coronographic imaging are the most important solar drivers of geomagnetic storms. ICMEs, their interplanetary, near-Earth counterparts, can be detected in situ, for example, by the Wind and ACE spacecraft. An ICME usually exhibits a complex structure that very often includes a magnetic cloud (MC). They can be commonly modelled as magnetic flux ropes and there is observational evidence to expect that the orientation of a halo CME elongation corresponds to the orientation of the flux rope. In this study, we compare orientations of elongated CME halos and the corresponding MCs, measured by Wind and ACE spacecraft. We characterize the MC structures by using the Grad–Shafranov reconstruction technique and three MC fitting methods to obtain their axis directions. The CME tilt angles and MC fitted axis angles were compared without taking into account handedness of the underlying flux rope field and the polarity of its axial field. We report that for about 64% of CME–MC events, we found a good correspondence between the orientation angles implying that for the majority of interplanetary ejecta their orientations do not change significantly (less than 45 deg rotation) while travelling from the Sun to the near-Earth environment.     

Coronal mass ejection detection using wavelets,curvelets and ridgelets: Applications for space weather monitoring

Coronal mass ejections (CMEs) are large-scale eruptions of plasma and magnetic field that can produce adverse space weather at Earth and other locations in the Heliosphere. Due to the intrinsic multiscale nature of features in coronagraph images, wavelet and multiscale image processing techniques are well suited to enhancing the visibility of CMEs and suppressing noise. However, wavelets are better suited to identifying point-like features, such as noise or background stars, than to enhancing the visibility of the curved form of a typical CME front. Higher order multiscale techniques, such as ridgelets and curvelets, were therefore explored to characterise the morphology (width, curvature) and kinematics (position, velocity, acceleration) of CMEs. Curvelets in particular were found to be well suited to characterising CME properties in a self-consistent manner. Curvelets are thus likely to be of benefit to autonomous monitoring of CME properties for space weather applications.     

Elemental Abundances in Coronal Structures

A great deal of evidence for elemental abundance variations among different structures in the solar corona has accumulated over the years. Many of the observations show changes in the relative abundances of high- and low-First Ionization Potential elements, but relatively few show the absolute elemental abundances. Recent observations from the SOHO satellite give absolute abundances in coronal streamers. Along the streamer edges, and at low heights in the streamer, they show roughly photospheric abundances for the low-FIP elements, and a factor of 3 depletion of high-FIP elements. In the streamer core at 1.5 R·, both high- and low-FIP elements are depleted by an additional factor of 3, which appears to result from gravitational settling. This revised version was published online in June 2006 with corrections to the Cover Date.     

无氰亚硫酸盐镀金

重点论述了无氰亚硫酸钠镀金的优点、配方及工作条件、配置程序，应用于实际生产中的效果及优点．     

Broadening of Fe X (6374 Å) profiles above the limb in a coronal hole

Profiles of the visible Fe X (6374 Å) coronal emission line as a function of height above the limb were obtained out to 1.16 solar radii in a coronal hole using the NSO/Sacramento Peak Observatory Coronagraph, Universal Spectrograph and a CCD camera. These are the first coronal line profiles obtained as a function of height in a coronal hole from the ground. Analysis of the line widths suggests a large component of nonthermal broadening which increases with height ranging from 40 to 60 km/s, depending upon the assumed temperature or thermal component of the profile.     

光纤环内部应力试验研究

光纤环是光纤陀螺的核心敏感部件,其内部应力值的大小和分布对光纤陀螺的整体性能有很大影响.光纤环的内部应力主要包含拉伸应力、弯曲应力和固化应力等,光纤环的绕制工艺和固化工艺等都会对光纤环的应力产生影响.通过测量不同绕制工艺下光纤环的应力分布和偏振串扰分布,得出光纤环绕制张力越小、光纤环直径越大、固化胶的收缩率越小,光纤环的应力也越小,相应的偏振串扰值也越小,为光纤环绕制技术的提高提供依据.     

原子传感用垂直腔面发射激光器研究进展

垂直腔面发射激光器(Vertical-cavity Surface-emitting Laser,VCSEL)是半导体激光器家族中的最重要成员之一,因其具有单纵模、低功耗、光束易整形等一系列独特优势,是多种微型化原子传感器的理想光源。围绕原子传感这一应用需求,国内外多个科研机构和企业对Rb原子和Cs原子传感用VCSEL开展了不同层次的研究,主要对其中的代表性研究进展进行综述。