The Solar Quiet Chromosphere—Corona Transition Region

The chromosphere-corona transition region of the Sun enjoys both simplicities of character and complexities of character which result from its very thin geometrical extent. The simplicities derive from the reasonably clear view of the energy balance (both observationally and theoretically), while the complexities derive from both the proximity of the not-so-clearly viewed regions below and above, and the almost certain convolutions and perhaps discontinuities in the three dimensional geometry of the transition sheet. While observational resolution and spectral information has improved greatly in recent years, the problems associated with a single vantage point, the Earth and its environs, have not gone away. To understand the transition region we must resolve structures radially and temporally as well as in the plane of the sky. This revised version was published online in June 2006 with corrections to the Cover Date.     

脉宽调制器中一类振荡器的全面解析结果

用分析法全面讨论脉宽调制器（IC：1842/3/4/5,1842A/3A/4A/5A）中振荡器的振荡特征参数（占空比D和频率f）与外接电阻R和电容C的关系.我们得到以R、C为自变量表达D和f的函数,以D、f为自变量求R、C的函数.并根据这些函数的计算结果绘制描述D、f、R、C（1F）4个参数之间的关系曲线.这些结果,不仅提升了对这类振荡器的认知,而且可供设计时直接引用和参考.     

Soft gamma repeaters

The observational properties of the soft gamma repeaters are reviewed briefly, starting with the time histories and energy spectra of their bursts. The short bursts and giant flares are compared. Their quiescent emission is presented, and the context of the magnetar model is discussed.     

用模糊集方法实现管理系统仿真输入非参数化的研究

以模糊信息优化处理的观点，研究了信息扩散方式实现非参数输入的途径、方法和效果、本文用正态扩散方式处理知识样本，形成参数概率颁上模式，通过ＳＩＭＡＮ仿真语言，对某一高速公路的一部分收费系统进行了仿真研究，结果表明：当人们对系统掌握的资料不多时，新方法有较大的优越性；如有较多的资料，新方法的结果与传统方法一致。     

The ‘Standard’ Sun Modelling and Helioseismology

The ‘standard’ solar model is based on a number of simplifying assumptions and depends on knowledge of the physical properties of matter in the Sun. Given these assumptions, the constraint that the model have the observed surface luminosity provides an estimate of the initial solar helium abundance. From helioseismic analyses further information can be obtained about the present composition, including a fairly precise measure of the envelope helium abundance and an estimate of the hydrogen profile in the radiative interior. It must be emphasized, however, that these inferences may suffer from systematic error arising from incomplete knowledge about the equation of state and opacity of the solar interior. This revised version was published online in June 2006 with corrections to the Cover Date.     

Coronal Heating: a Comparison of Ion-cyclotron and Gravity Damping Models

SOHO/UVCS data indicate that minor ions in the corona are heated more than hydrogen, and that coronal heating results in T_⊥ larger than T_‖. Analogous behavior has been known from in situ measurements in solar wind for many years. Here we compare and contrast two mechanisms which have been proposed to account for the above behavior: ion-cyclotron resonance and gravity damping. This revised version was published online in June 2006 with corrections to the Cover Date.     

Short-Lived Radionuclides in Meteorites: Constraints on Nebular Timescales for the Production of Solids

Variations in the abundances of short-lived radionuclides such as ²⁶Al (τ_1/2 ≈ 0.74 Ma) and ⁵³Mn (τ_1/2 ≈ 3.7 Ma) in meteoritic solids may be used to infer relative formation intervals of these solids in the nebula at precisions of less than 1 Ma. In a strict chronometric interpretation of the isotopic variations, whereby criteria such as spatial and temporal isotopic homogeneity and closed system isotopic evolution are met, solid formation occurred in the nebula for at least several million years. This is longer than some theoretical and astronomical estimates for the duration of the active nebula. The evidence for live ⁴¹Ca (τ_1/2 ≈ 0.10 Ma) in meteoritic inclusions further indicates that the onset of solid formation occurred quite early, perhaps within a few hundred thousand years after the onset of the collapse of the sun's parent molecular cloud. Failure of the chronometric interpretation may arise for a variety of reasons, including but not limited to, the late, inhomogeneous injection of material from a nearby stellar source or the local production of short-lived radionuclides by an energetic particle irradiation, e. g., from T Tauri (X-wind) or galactic cosmic ray sources. Although some isotopic evidence exists that the criteria required for a strict chronometric interpretation are not met by each of the short-lived chronometers, there is no compelling reason to shorten the interval of solid formation in the nebula to less than 1 Ma. This revised version was published online in June 2006 with corrections to the Cover Date.     

韧性材料的冲蚀损伤数值仿真综述

砂尘造成韧性材料的冲蚀损伤现象和损伤演化规律是冲蚀机理研究的重要内容，基于相应冲蚀试验和数值仿真的分析 方法是揭示冲蚀机理的重要手段。回顾了砂尘冲蚀损伤研究的缘起和发展经历，在介绍砂尘冲蚀损伤机理的基础上，总结了当前 数值仿真研究的3种主流方法：有限元方法、无网格方法和计算流体动力学方法。从数值仿真角度针对砂尘对韧性材料造成的破 坏模式、砂尘冲击姿态、砂尘冲击速度和形状、砂尘破碎对材料去除机制的影响等4个方面综述了影响冲蚀损伤机理的主要因素 和当前研究进展。砂尘对韧性材料造成的破坏模式通常分为材料凹陷、滑动、犁削、切削等4种不同机制；砂尘的冲击姿态决定了 材料的损伤模式；砂尘的冲击速度和砂尘的形状决定了材料的损伤严重程度；砂尘破碎现象对材料的去除机制有一定影响。     

航天器空间环境干扰力矩分析与仿真研究

针对航天器在轨运行时所受到的空间环境干扰力矩进行建模分析,并通过实时解算和矢量叠加的方式进行仿真研究,尤其对太阳光压力矩与大气阻力力矩的建模与仿真提出了新的方法,该方法通过建立光照面与迎风面的判断准则,准确地对太阳光压力矩与大气阻力力矩进行了估计。对各种空间环境干扰力矩的精确建模与仿真为航天器精确姿态控制设计及系统姿态控制方案和控制执行机构的选取提供了依据,文中提出的方法简单易用,工程实现性强,为未来的工程应用提供了一定的理论依据。     

The ground-based large-area wide-angle γ-ray and cosmic-ray experiment HiSCORE

The question of the origin of cosmic rays and other questions of astroparticle and particle physics can be addressed with indirect air-shower observations above 10 TeV primary energy. We propose to explore the cosmic ray and γ-ray sky (accelerator sky) in the energy range from 10 TeV to 1 EeV with the new ground-based large-area wide angle (ΔΩ ∼ 0.85 sterad) air-shower detector HiSCORE (Hundred^∗i Square-km Cosmic ORigin Explorer). The HiSCORE detector is based on non-imaging air-shower Cherenkov light-front sampling using an array of light-collecting stations. A full detector simulation and basic reconstruction algorithms have been used to assess the performance of HiSCORE. First prototype studies for different hardware components of the detector array have been carried out. The resulting sensitivity of HiSCORE to γ-rays will be comparable to CTA at 50 TeV and will extend the sensitive energy range for γ-rays up to the PeV regime. HiSCORE will also be sensitive to charged cosmic rays between 100 TeV and 1 EeV.