构建廊坊市基层群众体育科学管理体制的相关研究

通过对廊坊市现行的基层群众体育管理体制及其运行机制现状的调查,总结廊坊市基层群众体育工作所面临的困难,及其管理体制存在的问题.系统分析与完善各群众体育组织的结构职能,根据社会发展的需要,为廊坊市基层群众体育科学合理管理体制的构建提出合理化建议与参考.     

液体火箭发动机高速采集数据工程数据库设计及应用

叙述了基于SQLSever数据库平台的液体火箭发动机高速采集数据工程数据库的架构设计及海量存储技术在试验数据分析过程中的应用.该数据库对提高数据管理水平、提高数据利用率及发动机的研制具有极大的帮助.数据库的架构设计较好的满足了试车高速采集数据及分析结果的分类存储、检索及查询.海量存储技术的应用解决了非结构化数据的快速存...     

Why should the latitude of the observer be considered when modeling gradual proton events? An insight using the concept of cobpoint

The shape of flux profiles of gradual solar energetic particle (SEP) events depends on several not well-understood factors, such as the strength of the associated shock, the relative position of the observer in space with respect to the traveling shock, the existence of a background seed particle population, the interplanetary conditions for particle transport, as well as the particle energy. Here, we focus on two of these factors: the influence of the shock strength and the relative position of the observer. We performed a 3D simulation of the propagation of a coronal/interplanetary CME-driven shock in the framework of ideal MHD modeling. We analyze the passage of this shock by nine spacecraft located at ∼0.4 AU (Mercury’s orbit) and at different longitudes and latitudes. We study the evolution of the plasma conditions in the shock front region magnetically connected to each spacecraft, that is the region of the shock front scanned by the “cobpoint” (Heras et al., 1995), as the shock propagates away from the Sun. Particularly, we discuss the influence of the latitude of the observer on the injection rate of shock-accelerated particles and, hence, on the resulting proton flux profiles to be detected by each spacecraft.     

小型二冲程航空发动机燃烧循环变动研究

利用峰值压力、最大压力上升率、燃烧百分率以及它们各自所对应的曲轴转角和相空间重构投影法评价小型二冲程航空发动机的燃烧循环变动.通过比较,认为燃烧百分率所对应的曲轴转角能更好地表征发动机的燃烧循环变动.针对发动机在中速和不同负荷条件下的燃烧循环变动分析,结果表明随负荷的加大,缸内燃烧的循环变动会变小,认为是负荷加大,气体...     

Large geomagnetic storms of extreme solar event periods in solar cycle 23

During extreme solar events such as big flares or/and energetic coronal mass ejections (CMEs) high energy particles are accelerated by the shocks formed in front of fast interplanetary coronal mass ejections (ICMEs). The ICMEs (and their sheaths) also give rise to large geomagnetic storms which have significant effects on the Earth’s environment and human life. Around 14 solar cosmic ray ground level enhancement (GLE) events in solar cycle 23 we examined the cosmic ray variation, solar wind speed, ions density, interplanetary magnetic field, and geomagnetic disturbance storm time index (D_st). We found that all but one of GLEs are always followed by a geomagnetic storm with D_st  −50 nT within 1–5 days later. Most(10/14) geomagnetic storms have D_st index  −100  nT therefore generally belong to strong geomagnetic storms. This suggests that GLE event prediction of geomagnetic storms is 93% for moderate storms and 71% for large storms when geomagnetic storms preceded by GLEs. All D_st depressions are associated with cosmic ray decreases which occur nearly simultaneously with geomagnetic storms. We also investigated the interplanetary plasma features. Most geomagnetic storm correspond significant periods of southward B_z and in close to 80% of the cases that the B_z was first northward then turning southward after storm sudden commencement (SSC). Plasma flow speed, ion number density and interplanetary plasma temperature near 1 AU also have a peak at interplanetary shock arrival. Solar cause and energetic particle signatures of large geomagnetic storms and a possible prediction scheme are discussed.     

Solar Energetic Particle Composition, Energy Spectra, and Space Weather

Recent progress in measuring the composition and energy spectra of solar energetic particles (SEPs) accelerated by CME-driven shocks is reviewed, including a comparison of the observed charge-to-mass dependence of breaks in SEP spectra with model predictions. Also discussed is a comparison of SEP and CME kinetic energies in seventeen large SEP events, and estimates of the SEP radiation dose that astronauts would be subject to once they venture outside the protective cover of Earth’s magnetosphere.     

On the Differences in Composition between Solar Energetic Particles and Solar Wind

Although the average composition of solar energetic particles (SEPs) and the bulk solar wind are similar in a number of ways, there are key differences which imply that solar wind is not the principal seed population for SEPs accelerated by coronal mass ejection (CME) driven shocks. This paper reviews these composition differences and considers the composition of other possible seed populations, including coronal material, impulsive flare material, and interplanetary CME material.     

Intrinsic parameters of massive OB stars

We present the results of our observations of stars of type O5 and earlier and show that inclusion of the line blocking between 228 and 912 A solves the problem found by Herrero et al. (1992) in the determination of their stellar parameters. We study the influence of the line blocking and other effects on the mass and helium discrepancies and show that the first one is reduced by the use of spherical, non hydrostatic model atmospheres and that the second one is probably due to exposure of CNO material.The INT is operated on the island of La Palma by the RGO in the Spanish Observatorio de El Roque de los Muchachos of the Instituto de Astrofsica de Canarias     

Characteristics of solar particle events at Mars relative to Earth

While not specifically designed to detect solar energetic particle radiation, the Electron Reflectometer onboard Mars Global Surveyor (MGS/ER) collected such data from January 1999 through October 2006. Energetic protons (?25 MeV) and other ions penetrated the MGS/ER shielding and registered counts within the instrument’s electronics. During solar particle events (SPE’s), prolonged enhancements in the particle background were observed at Mars with time intensity profiles similar to Earth based SPE observations. Throughout the lifespan of MGS/ER, 85 distinct SPE’s were observed. Basic characteristics of Mars based SPE observations and the frequency of SPE occurrences at Mars are compared to corresponding Earth based observations. Approximately 22% of SPE’s that occurred during MGS/ER operation were observed at Earth but not Mars. Similarly, 19% of SPE’s were observed at Mars but not Earth. Time intensity profiles at Earth and Mars match predictions provided in the literature, based on the physical location of the detector with respect to the motion of the interplanetary shock wave. Note: The work described herein was largely conducted as part of a doctoral dissertation produced by the author.     

固体运载火箭抗强电磁脉冲优化设计方法

本文分析了火箭在飞行过程中的强电磁脉冲(EMP)环境，建立了箭上敏感设备受强电磁脉冲干扰的优化设计模型，包括传导干扰及辐射干扰两种设计模型。针对起飞质量对火箭总体参数设计的制约问题，以最小质量增量为目标函数，采用模拟退火(SA)算法，对箭上典型电气系统抗强电磁脉冲防护进行优化设计研究，为箭上敏感设备抗强电磁脉冲指标与质量增量提供了平衡选取方法。优化结果表明,火箭在飞行过程中典型电气系统的抗强电磁脉冲性能指标达到要求的同时，实现了火箭质量增量最小的目标。