C/ C-PAA 与C/ C-FA 弯曲性能对比

通过PIP工艺制备了C/C-PAA、C/C-FA复合材料,对PAA、FA裂解碳的XRD、浸渍效果以及C/C-PAA和C/C-FA的弯曲强度进行了分析.结果表明:PAA裂解碳的炭质量、浸渍效果较好,C/C-PAA弯曲强度比C/C-FA弯曲强度高34.9％,弯曲模量对比不明显.     

M40J/CE/EP复合材料出气性能研究

通过地面环境模拟实验,分析了高模碳纤维/环氧树脂改性氰酸酯复合材料(M40J/CE/EP)的表面元素,研究了高真空加热环境下复合材料的真空出气性能和出气气体成分.结果表明,M40J/CE/EP复合材料的表面主要由C、O、N元素构成;经高真空加热后,复合材料的出气气体成分以小分子挥发物和碳氢化合物电离碎片为主,有可能在空间低温条件下冷凝在航天器的敏感器件表面而造成污染;通过真空出气性能实验测得,M40J/CE/EP复合材料的总质量损失(TML)的平均值为0.27%,收集到的可凝挥发物(CVCM)为0,完全达到出气筛选合格的指标要求.     

高浓度颗粒流冲刷条件下硅橡胶和EPDM绝热材料动态烧蚀实验

利用X射线实时诊断技术(RTR)针对硅橡胶和EPDM绝热材料,开展了高浓度颗粒流冲刷条件下动态烧蚀实验研究,成功获得了绝热材料烧蚀表面退移过程的序列图像。研究表明:(1)在本实验条件下,硅橡胶绝热材料颗粒冲刷区域的瞬时烧蚀率在0～2s内迅速增加,2s之后瞬时烧蚀率略有下降并趋于稳定;EPDM绝热材料颗粒冲刷区域的瞬时烧蚀率在0～1s内迅速增加,1s之后瞬时烧蚀率趋于稳定;(2)相同冲刷条件下硅橡胶绝热材料抗颗粒流冲刷性能比EPDM绝热材料差,硅橡胶绝热材料不适合在高过载发动机中应用;(3)高浓度颗粒流冲刷条件下绝热材料的烧蚀率比常规条件下要严重的多,其机理主要是高温颗粒流对炭化层有强烈的机械剥蚀效应和热化学烧蚀作用。实验结果对硅橡胶和EPDM绝热材料烧蚀机理研究及烧蚀建模具有重要参考价值。     

不同工件超光滑表面残余应力的测试研究

通过对玻璃、陶瓷、金属3个试件进行超精密加工,使试件表面粗糙度达到纳米级,采用非破坏性的X射线衍射sin2ψ法测量原理对不同试件的残余应力进行了测试研究。结果表明:在本试验条件下,3个试件都只存在残余压应力,并且陶瓷的残余压应力最大,金属残余压应力最小。     

MESSENGER and the Chemistry of Mercury’s Surface

The instrument suite on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft is well suited to address several of Mercury’s outstanding geochemical problems. A combination of data from the Gamma-Ray and Neutron Spectrometer (GRNS) and X-Ray Spectrometer (XRS) instruments will yield the surface abundances of both volatile (K) and refractory (Al, Ca, and Th) elements, which will test the three competing hypotheses for the origin of Mercury’s high bulk metal fraction: aerodynamic drag in the early solar nebula, preferential vaporization of silicates, or giant impact. These same elements, with the addition of Mg, Si, and Fe, will put significant constraints on geochemical processes that have formed the crust and produced any later volcanism. The Neutron Spectrometer sensor on the GRNS instrument will yield estimates of the amount of H in surface materials and may ascertain if the permanently shadowed polar craters have a significant excess of H due to water ice. A comparison of the FeO content of olivine and pyroxene determined by the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) instrument with the total Fe determined through both GRNS and XRS will permit an estimate of the amount of Fe present in other forms, including metal and sulfides.     

Stellar Coronal Astronomy

Coronal astronomy is by now a fairly mature discipline, with a quarter century having gone by since the detection of the first stellar X-ray coronal source (Capella), and having benefitted from a series of major orbiting observing facilities. Serveral observational characteristics of coronal X-ray and EUV emission have been solidly established through extensive observations, and are by now common, almost text-book, knowledge. At the same time the implications of coronal astronomy for broader astrophysical questions (e.g.Galactic structure, stellar formation, stellar structure, etc.) have become appreciated. The interpretation of stellar coronal properties is however still often open to debate, and will need qualitatively new observational data to book further progress. In the present review we try to recapitulate our view on the status of the field at the beginning of a new era, in which the high sensitivity and the high spectral resolution provided by Chandra and SMM-Newton will address new questions which were not accessible before. This revised version was published online in August 2006 with corrections to the Cover Date.     

Coronal Mass Ejections

This workshop summary tries to distill the key difficulties and questions in the art of (I)CME physics and strategies to address them. (I)CMEs are multi-dimensional, multi-parameter, and multi-scale phenomena related to the solar dynamo, corona, and heliosphere. This workshop illustrates the immense progress made in describing and modeling these spectacular energetic solar events, but also shows clear shortcomings in our understanding of them.     

Black-hole transients: From QPOs to relativistic jets

Due to the impressive amount of new data provided by the RXTE satellite in the past decade, our knowledge of the phenomenology of accretion onto black holes has increased considerably. In particular, it has been possible to schematize the outburst evolution of transient systems on the basis of their spectral and timing properties, and link them to the ejection of relativistic jets as observed in the radio. Here, I present this scheme, concentrating on the properties of the quasi-periodic oscillations observed in the light curves and on the link with jet ejection.     

Observations of compact X-ray binaries with the Chandra X-ray Observatory

The Chandra X-ray Observatory was launched on July 23, 1999. The first X-ray photons were detected on August 12 of that same year. Subsequently observations with the Observatory, which features sub-arcsecond angular resolution, have revolutionized our understanding of the X-ray emitting sky providing hosts of spectacular energy-resolved images and high-resolution spectra. Here we present a brief overview of Chandra X-ray Observatory observations of compact X-ray binaries.     

High resolution X-ray spectrum of AM Her

We present the analysis of archival Chandra high resolution X-ray spectra of AM Her. Emission lines from several hydrogen-like ions, helium-like ions, Fe-L shell transitions and Fe-K fluorescent are identified. Using the resonance, intercombination and forbidden lines of the few prominent helium-like ions, we infer a density greater than 2 × 10¹² cm⁻³ and a temperature of 2 MK for the oxygen and neon line emitting regions in the accretion column of AM Her.