酚醛树脂固化度的X射线衍射分析

发展使用Ｘ射线衍技术对酚醛树脂固化度进行研究，确定了酚醛树脂固化度与Ｘ射线散射最大值的 关系，得出了利用２θ角来标定树脂固化度的公式。该方法具有快速、无损、灵敏度主同的优点，并可适用于各种不同的酚醛树脂。     

飞机噪声预测和分析

根据中国民航规章中有关飞机适航噪声审定的要求和噪声预测原理建立了飞机噪声预测系统软件。该软件除可预测飞机适航噪声审定的起飞、进场和边线有效感觉噪声级外,还可计算巡航过程机体表面声压分布。各种噪声源的声功率在软件中均可单独计算,因此改变发动机和飞机参数可以考查这些参数对声功率的影响;对发动机和飞机设计有参考价值。通过算例计算出的起飞、进场和边线有效感觉噪声级与实测结果符合较好,能很好地满足工程应用需要。     

质子交换膜燃料电池及其空间应用

介绍了质子交换膜燃料电池(PEMFC)、可再生燃料电池(RFC)的工作原理、性能和空间应用特点，以及发展航空航天器用可再生PEMFC系统的必要性和可行性。讨论了PEMFC和可再生PEMFC系统所面临的技术难点。最后，针对我国的实际情况，提出了分阶段发展PEMFC和可再生PEMFC的建议。     

相关噪声背景下相干信源DOA估计算法研究

根据信号和噪声的非圆对称特性,利用除第一个阵元外的其它阵元接收数据的共轭信息,对原阵列进行有效地扩展,提出了一种相关噪声背景下相干信源波达方向（DOA）估计的新算法。由于对阵列进行了虚拟扩展并运用斜投影算法将非相干信源与相干信源分开分辨,因此该算法具有很强的信源过载能力及阵元节省能力,在一定程度上提高了空间分辨率DOA估计的性能,并可对消空间具有非圆对称性的相关噪声,适用于低信噪比环境。仿真结果证明了算法理论的正确性和有效性。     

The gas pixel detector as a solar X-ray polarimeter and imager

The Sun is the nearest astrophysical source with a very intense emission in the X-ray band. The study of energetic events, such as solar flares, can help us to understand the behaviour of the magnetic field of our star. There are in the literature numerous studies published about polarization predictions, for a wide range of solar flares models involving the emission from thermal and/or non-thermal processes, but observations in the X-ray band have never been exhaustive.The gas pixel detector (GPD) was designed to achieve X-ray polarimetric measurements as well as X-ray images for far astrophysical sources. Here we present the possibility to employ this instrument for the observation of our Sun in the X-ray band.     

XMM-Newton study of soft excess X-ray emission in clusters of galaxies

We discuss the detection of soft excess X-ray emission in a sample of 19 clusters of galaxies observed by XMM-Newton. In 6/19 clusters evidence for a soft X-ray excess is found. Four of these clusters show soft X-ray and O VII line emission from gas with a temperature of 0.2 keV. The centroid of this oxygen line is consistent with the redshift of the cluster. The intensity and spatial extend of the soft excess agrees with previous PSPC measurements. These observations are interpreted as emission from warm-hot intergalactic medium filaments, with density enhancements near the cluster centers, consistent with theoretical predictions. In the other two soft excess clusters a non-thermal origin is consistent with the data.     

Evolution of galaxy cluster scaling from XMM-Newton observation of the galaxy clusters at z ⩾ 0.4

We present here new XMM-Newton observations of 3 relatively cool clusters at z ≈ 0.4, complemented by archival observations of 3 other clusters at similar redshift. We derived the M–T and R–T relations from the hydrostatic equation using an isothermal temperature distribution.     

XMM-Newton survey of non-thermal shell candidates: Preliminary results on DA 530

The investigation of the general properties of non-thermal (NT) X-ray shell supernova remnants (SNRs), of which SN 1006 is the prototype, is important to understand how electrons are accelerated in SNR shocks and what is the origin of cosmic rays. Using the XMM-Newton satellite, we are carrying on a survey of putative non-thermal SNR candidates previously unknown or little studied in the X-ray band, in order to investigate the different manifestations of NT emission in SNR shells. The SNRs we have selected are likely to expand in a low density medium, and therefore to have a low thermal X-ray emission, that usually outshines the non-thermal one. We report here preliminary results obtained on the SNR shell DA 530.     

金属多层膜超晶格结构研究

用高分辨的三晶体x—射线衍射仪测量了Zr、Cu金属交替的多层膜的x—射线小角反射谱。用扩展了的Born—wolf光学模型对Zr、Cu多层膜的x—射线小角反射数据进行了定量分析。结果表明，该金属多层膜在其生长方向具有超晶格结构。在两层金属膜之间的界面上，由于内扩散，形成了界面交混层，它使x—射线小角反射所产生的高阶Bragg峰的强度减弱。由于两种金属膜的晶格不匹配，使高阶Bragg峰加宽。界面的粗糙度可用来模拟x—射线小角反射曲线的阻尼振荡效应。     

基于DCT-CS的脉冲星周期超快速估计方法

受快速傅里叶变换（fast Fourier transform，FFT）的影响，基于FFT和压缩感知（compressive sensing, CS）的脉冲星周期快速估计算法的计算量大。为进一步减小计算量并提高计算精度，利用离散余弦变换（discrete cosine transform，DCT)取代FFT，提出了一种基于DCT-CS的脉冲星周期超快速估计算法。在该方法中，利用DCT提取脉冲星信号的低频部分构建低频DCT矩阵；构建畸变轮廓字典并获取累积轮廓；提出了利用最大值超分辨率稀疏恢复估计脉冲星周期的方法。仿真结果表明，DCT-CS的脉冲星周期估计精度达到了3.82×10-12 s，计算时间达到了9.31 ms。与FFT-CS相比，周期估计精度提高了约16%，计算时间缩短了约37.5%，实现了实时高精度的脉冲星周期估计。