用衰减全反射(ATR)研究金属薄膜的物理性质

本文作者所设计的实验是利用光学中全反射衰减特性方法测量在介质上蒸镀的金属薄膜的厚度和各种频率下的复介电常数等物理性质，它可以精确测定１００～１０００范围内金属膜层的厚度和ε（ω）值，以及一些其它性质，是研究固体表面物理的一种有效的方法和技术。     

飞机结冰热力学行为研究综述

热力学现象是制约飞机结冰特性的重要现象之一。开展飞机结冰过程热力学行为的研究旨在深入把握结冰过程的规律特征,从而为建立科学有效的结冰防护手段、保障结冰条件下的飞行安全奠定基础。本文回顾和介绍了飞机结冰热力学研究所涉及的过冷水滴存在的物理机制、结冰热力学条件、形核与晶体生长、耦合液/固相变的复合传热传质特性,以及热力学效应作用下的结冰物理特性等相关领域的研究进展及发展现状,并基于国外相关研究的发展趋势,提出了中国未来飞机结冰热力学研究需重点关注的方向。     

介质涂覆位置对球面收敛喷管电磁散射特性影响

外形设计和隐身材料使用是缩减目标雷达散射截面积(RCS)的两种常用方法。为了研究雷达吸波材料(RAM)对于球面收敛矢量喷管(SCFN)的RCS减缩效果,采用引入阻抗边界条件后的迭代物理光学(IPO)法,研究了球面收敛二元喷管及8种吸波材料涂覆方案的电磁散射特性,并获得了X波段下9种模型的后向RCS随探测角度的变化规律。研究结果表明:吸波材料涂覆可以有效地缩减球面收敛喷管的RCS;合理的涂覆方案可以在保证RCS缩减效果的基础上,降低吸波材料的使用量;相比全涂覆方案,仅在喷管出口和球面段进行涂覆,可以在吸波材料减少30%使用量的情况下,达到全涂覆方案80%的缩减效果。     

He-like Ar xvii triplet observed by RESIK

We present the observations of He-like Ar triplet lines obtained by RESIK spectrometer aboard CORONAS-F. Interpretation of intensity ratios between triplet lines of lower Z elements is known to provide useful diagnostics of plasma conditions within the emitting source. Here, we investigate whether triplet line ratios are useful for interpretation of higher Z element spectra. A high sensitivity, low background and precise absolute calibration of RESIK allow to consider in addition also the continuum contribution. This provides a way to determine the Ar absolute abundance from the observed triplet component ratios. The method is presented and the results are shown for two selected flares. Derived values of Ar absolute abundance for these flares are found to be similar: 2.6 × 10⁻⁶ and 2.9 × 10⁻⁶. They fall in the range between presently accepted Ar photospheric and coronal abundances.     

Progress on Solar Physics in China During 2004 - 2006

The solar physics studies in China during 2004-2006 from solar interior to solar atmospheres and solar-interplanetary space are summarized. These researches are arranged under the topics of solar interior, photosphere, chromosphere and transition region, corona, flares and CMEs (and the associated radio bursts, X-ray/γ-ray bursts and particle acceleration), solar wind, solar cycle, and ground-based instrumentation.     

Research on a complex CME event including Hα, LASCO, radio and MDI observations

We present our research on a fast and decelerating partial halo coronal mass ejection (CME) event detected in multi-wavelengths in the chromosphere and the corona on 14 October, 1999. The event involved a whole complex active area which spanned more than 40° of heliolongitude. It included a strong solar flare (XI/1N) and a complex eruptive filament within an active region of the entire complex. Especially, several radio sources were detected in the decimetric range prior to the CME by the Nançay Radioheliograph (NRH). A linear force-free field extrapolation of the Michelson Doppler Imager (MDI) magnetogram was performed to calculate the magnetic topology of the complex prior to the triggering of the event. The presence of a coronal null point combined with the occurrence of two distant and nearly simultaneous radio sources put strong arguments in favor of the generalized breakout model for the triggering of the eruption. The analysis of the subsequent development of the event suggests that large interconnecting loops were ejected together with the CME.     

Geoeffectivity of Coronal Mass Ejections

Coronal mass ejections and post-shock streams driven by them are the most efficient drivers of strong magnetospheric activity, magnetic storms. For this reason there is considerable interest in trying to make reliable forecasts for the effects of CMEs as much in advance as possible. To succeed this requires understanding of all aspects related to CMEs, starting from their emergence on the Sun to their propagation to the vicinity of the Earth and to effects within the magnetosphere. In this article we discuss some recent results on the geoeffectivity of different types of CME/shock structures. A particularly intriguing observation is that smoothly rotating magnetic fields within CMEs are most efficient in driving storm activity seen in the inner magnetosphere due to enhanced ring current, whereas the sheath regions between the shock and the ejecta tend to favour high-latitude activity.     

End-to-End Modeling of the Solar Terrestrial System

Traditionally modeling for space science has concentrated on developing simulations for individual components of the solar terrestrial system. In reality these regions are coupled together. This coupling can be as simple as the driving of the magnetosphere – ionosphere – thermosphere system by the solar wind or as a complicated as the feedback of the ionospheric conductivity and currents on the magnetosphere. As part of the CISM project we are beginning a concentrated effort to compressively model the entire system. This approach includes chains of models. In the first chain physics based numerical models are utilized while in the second chain empirical models are coupled together. The first half of this paper discusses the numerical modeling approach by highlighting the coupling of pairs of regions within the system. In the second section we present results from empirical models which are combined to make long term forecasts of conditions in the geospace environment. It is expected that a validated and reliable forecast model for space weather can be obtained by combining the strongest elements of each chain.     

Keck observations of ROSAT ultra-luminous X-ray source candidates

We present results of optical follow-up observations of candidate ultra-luminous X-ray sources (ULXs). Using Keck optical spectroscopy, 17 of the candidates from the Colbert and Ptak [Colbert, E.J.M., Ptak, A.F. A catalog of candidate intermediate-luminosity X-ray objects. ApJS 143, 25–45, 2002] catalog have been identified; this is one of the largest sets of optical identifications of such objects thus far. Fifteen are background active galactic nuclei (AGN); two are foreground stars in our Galaxy. These findings are consistent with background and foreground object expectations, as derived from log N–log S relations. Also, the results are briefly discussed in terms of the spiral-galaxy/ULX connection.     

Properties of Interplanetary Coronal Mass Ejections

Interplanetary coronal mass ejections (ICMEs) originating from closed field regions on the Sun are the most energetic phenomenon in the heliosphere. They cause intense geomagnetic storms and drive fast mode shocks that accelerate charged particles. ICMEs are the interplanetary manifestations of CMEs typically remote-sensed by coronagraphs. This paper summarizes the observational properties of ICMEs with reference to the ordinary solar wind and the progenitor CMEs.