Effects of sector structure of the interplanetary magnetic field on the upper mesosphere–lower thermosphere dynamics

In this paper we study the influence of the interplanetary magnetic field (IMF) polarity changes caused by the Earth passing through the IMF sector boundary on the dynamic processes taking place in neutral atmosphere within the altitude interval of the upper mesosphere–lower thermosphere (83–101 km). The analysis has revealed the influence of the IMF sector structure on dynamics of the upper mesosphere–lower thermosphere. There has been a significant seasonal variation of the wind reaction to the IMF polarity changes observed. The influence of the IMF polarity changes on neutral atmosphere dynamics within the altitude range of 83–101 km is most pronounced in the zonal component of neural wind when the IMF polarity changes from negative to positive in all the seasons except for spring and when IMF polarity changes from positive to negative – in spring only.     

激光标线仪校准方法研究CSCD

激光标线仪可以输出相互垂直的水平激光线和铅垂激光线,被广泛应用于建筑工程和装修装饰施工中,然而仪器的误差会直接影响工程质量。通过对输出激光线水平度、倾斜度和直线度等多项误差来源进行理论分析,研究并设计了针对各项误差的校准方法。     

Study of the 28 October 2003 and 20 January 2005 solar flares by means of 2.223 MeV gamma-emission line

By the data on intensity-time profiles of the neutron capture line of 2.223 MeV we have studied some characteristics of two solar flares, 28 October 2003 and 20 January 2005 (INTEGRAL and CORONAS-F observations, respectively). The SINP code was applied making allowance for the main processes of neutron interactions and deceleration in the solar plasma, character of neutron source, losses of neutrons and density model of the solar atmosphere. Comparison of the computed time profiles of 2.223 MeV line with observed ones for the flare of 28 October 2003 confirms the results obtained earlier for three other flares. Namely, the effect of density enhancement (EDE) in the sub-flare region, as well as the variations (hardening) of accelerated particle spectrum in the course of the event have been confirmed. The usual modeling procedure by the SINP code, however, seems to be inapplicable to the event of 20 January 2005. Possible causes of density enhancements during some flares and peculiarities of the 20 January 2005 flare are discussed.     

电磁超介质研究进展

电磁超介质是当前电磁学和物理研究领域中的前沿与热点，文章将左手材料、复合左／右手传输线、光子晶体统一在电磁超介质的体系下进行介绍，并论述了电磁超介质的发展现状。     

基于DIY理念的苏州旅行社线路配置现状研究

DIY作为时尚消费理念风靡全世界，而随着休闲性、体验性等新的旅游元素渗入传统旅游方式．DIY旅游在各大城市城市兴起。本文通过在线调查和咨询的方式，对国家级旅游城市——苏州旅行社DIY旅游线路配置的现状进行了研究，进而提出自己的意见和看法。     

实现程控化焊接两圆形管件的几何建模及计算方法

将圆形管件焊接成三通、四通等是焊接行业经常遇到的工艺。采用传统的手工式切割与焊接不仅工艺粗糙，而且效率也低。现代的焊接设备以其高效、自动化、程控化逐步取代手工操作。将提供各种形状的管件以不同连接形式焊接与切割以实现自动化、程控化的计算方法。     

Comparison of Polar and Equatorial Coronal Holes Observed by UVCS/SOHO: Geometry and Physical Properties

We analyzed UVCS/SOHO data and compared the H I Lyα (121.6 nm) and O VI (103.2 nm, 103.7 nm) emission in the polar and equatorial coronal holes. We found that the emission lines have similar characteristics in these two types of coronal holes. Both types show evidence for superradially diverging boundaries. The latitudinal distribution of the O VI line ratio may indicate that the equatorial coronal hole has O⁺⁵ outflow velocities lower than in the polar coronal holes. This revised version was published online in June 2006 with corrections to the Cover Date.     

四杆机构转折圆及其应用

介绍了转折圆的运动学特性，论述了求铰链四杆机构的转折圆，以及利用转折圆进行铰链四杆机构近似直线导向设计的方法。     

UVCS/SOHO Observations of H I Lyman Alpha Line Profiles in Coronal Holes at Heliocentric Heights Above 3.0 R⊙

The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO) has been used to measure spectral line profiles for H I Lyα in the south polar coronal hole at projected heliocentric heights from 3.5 to 6.0 R_⊙ during 1998 January 5–11. Observations from 1.5 to 2.5 R_⊙ were made for comparison. The H I Lyα profile is the only one observable with UVCS above 3.5 R_⊙ in coronal holes. Within this region the outflowing coronal plasma becomes nearly collisionless and the ionization balance is believed to become frozen. In this paper, the 1/e half widths of the coronal velocity distributions are provided for the observed heights. The velocity distributions include all motions contributing to the velocities along the line of sight (LOS). The observations have been corrected for instrumental effects and interplanetary H I Lyα. The half widths were found to increase with projected heliographic height from 1.5 to 2.5 R_⊙ and decrease with height from 3.5 to 5 R_⊙. This revised version was published online in June 2006 with corrections to the Cover Date.