硫源种类对微波合成CZTS颗粒与薄膜性能的影响

研究不同硫源对微波液相合成的Cu２ＺｎＳｎＳ４（CZTS）纳米颗粒尺寸及形貌的影响。结果表明：当采用硫脲作为硫源时,所制备的CZTS纳米颗粒为平均尺寸500 nm的球状结构纳米颗粒;采用L 半胱氨酸作为硫源所制备的CZTS纳米颗粒为50 nm的空心球状纳米颗粒;而当使用硫代乙酰胺作为硫源制备CZTS纳米颗粒,其平均尺寸仅为3 nm。采用 平均尺寸为500 nm或50 nm的纳米颗粒制备墨水,将墨水旋涂到衬底上时,其致密性很差,明显存在许多孔洞。当采用平均尺寸为3 nm的纳米颗粒制作墨水,并将其制成薄膜时,薄膜致密性与均匀性都比较好。将最佳的预制薄膜进行硫化处理,其结晶性明显提高,并得到转化效率为2.1%的CZTS太阳电池。     

Moment-tensor inversion and decomposition for cracks in thin plates

The knowledge of crack type and dislocation orientation is helpful for the lifetime prediction of thin plates on aircrafts. The moment-tensor inversion utilizes the Acoustic Emission (AE) signals to detect cracks and the source mechanisms can be interpreted by the decomposition of moment tensors. Since the traditional moment-tensor inversion is implemented for the AE sources inside infinite elastic bodies, the inversion needs to be modified for the cracks in thin plates. In this study, the moment tensors of cracks in thin plates are derived and the inversion equation is provided based on the Green's function of second kind. A method of modifying the moment tensors to adapt to the existing decomposition processes and source-type plots is provided. By employing the Finite Element Method (FEM), the wave fields generated by the AE sources are computed. The AE sources continuously changing from pure tensile type (Model I) to shear type (Model II) are achieved in the FE models and the moment tensors are recovered. By the comparison between the reference values and recovered solutions, the source type can be accurately identified in the source-type plot and the applicability of the moment-tensor inversion for cracks in thin plates is confirmed.     

The optical emission lines of type 1 X-ray bright Active Galactic Nuclei

A strong X-ray emission is one of the defining signatures of nuclear activity in galaxies. According to the Unified Model for Active Galactic Nuclei (AGN), both the X-ray radiation and the prominent broad emission lines, characterizing the optical and UV spectra of Type 1 AGNs, are originated in the innermost regions of the sources, close to the Super Massive Black Holes (SMBH), which power the central engine. Since the emission is concentrated in a very compact region (with typical size r?0.1$r?0.1$ pc) and it is not possible to obtain resolved images of the source, spectroscopic studies of this radiation represent the only valuable key to constrain the physical properties of matter and its structure in the center of active galaxies. Based on previous studies on the physics of the Broad Line Region (BLR) and on the X-ray spectra of broad (FWHM_Hβ ? 2000 km s⁻¹) and narrow line (1000 km s⁻¹ ?FWHM_Hβ ? 2000 km s⁻¹) emitting objects, it has been observed that the kinematic and ionization properties of matter close to the SMBHs are related together, and, in particular, that ionization is higher in narrow line sources. Here we report on the study of the optical and X-ray spectra of a sample of Type 1 AGNs, selected from the Sloan Digital Sky Survey (SDSS) database, within an upper redshift limit of z=0.35$z=0.35$, and detected at X-ray energies. We present analysis of the broad emission line fluxes and profiles, as well as the properties of the X-ray continuum and Fe Kα emission and we use these parameters to assess the consistency of our current AGN understanding.     

A model for the Balmer pseudocontinuum in spectra of type 1 AGNs

Here we present a new method for subtracting the Balmer pseudocontinuum in the UV part of type 1 AGN spectra. We calculate the intensity of the Balmer pseudocontinuum using the prominent Balmer lines in AGN spectra. We apply the model on a sample of 293 type 1 AGNs from SDSS database, and found that our model of Balmer pseudocontinuum + power law continuum very well fits the majority of AGN spectra from the sample, while in ∼$\sim$15% of AGNs, the model fits reasonable the UV continuum, but a discrepancy between the observed and fitted spectra is noted. Some of the possible reasons for the discrepancy may be a different value for the optical depth in these spectra than used in our model or the influence of the intrinsic reddening.     

空间太阳能电站地球同步拉普拉斯轨道动力学特性

现有关于空间太阳能电站(SpaceSolarPowerStation,SSPS)轨道动力学的研究中,均将其放置于地球静止轨道（GeostationaryOrbit,GEO〖BF〗）,然而这并非最优的工作轨道。文章提出了一种优于ＧＥＯ的地球同步拉普拉斯（GeosynchronousLaplacePlane,GLP）轨道。首先,建立了轨道运动模型及影响轨道运动的摄动模型,包括地球非球形引力摄动、日月引力摄动、太阳光压力摄动及微波反冲力摄动;然后,提出了评估空间太阳能电站轨道的3个指标：接收功率、轨道适用性和安全性,并据此分析了GLP轨道相对于ＧＥＯ的优势。最后,给出了数值仿真算例。结果表明：在发电功率大致相同且满足供电需求的情况下,工作在GLP上的SSPS每年大约能节省用于轨道保持的燃料364534kg。     

利用T矩阵法实现非程控步进衰减器的测量

针对现有衰减校准系统量程小、难以满足步进衰减器等大衰减量计量需求的问题,通过对T矩阵法的分析研究,提出了利用T矩阵法实现非程控步进衰减器测量的方案,详细介绍了T矩阵法的原理和实现过程,经过实测验证,所述方法可为大衰减量的计量测试提供一套切实可行的解决方案。     

加力燃烧室NOx排放生成规律试验分析

实现航空发动机大推力通常采用加力燃烧室设计,燃烧室进气温度升高会同步导致排放尾气中NO_x浓度提高.采用典型加力燃烧室主稳定器的V型结构试验件,测试加力燃烧前后(进口600 ℃,出口600~1 200 ℃)燃烧室排放断面的NO_x浓度分布,通过相同流场4种试验工况的NO_x生成浓度组分和氧含量变化分析,验证了加力燃烧室NO_x生成以热力型NO为主的"高温、富氧、贫油"燃烧特性.结果表明加力燃烧室燃烧过程中消耗的氧含量大多贡献于CO₂增量,在800~1 000 ℃燃气排放温度范围内,不完全燃烧产物CO对NO的热力生成有明显抑制作用.     

一种微波关联成像的新方法

将强度关联量子成像理论引入到雷达成像技术中,提出了一种全新的微波关联成像方法。向目标发射多个幅度、相位可控的单元信号,同时记录各个信号的状态并结合距离信息制作＂成像底版＂,通过对回波信号和＂成像底版＂的关联结果进行数理统计后可实现雷达高分辨成像。     

环形腔室径向宽度对加力燃油泵内流及性能影响

对某加力燃油泵内部非定常流动开展了系统的数值模拟,研究了不同环形腔室径向宽度条件下泵的外特性和内流特征.计算结果表明,缩小径向宽度可有效提高泵在不同流量下的扬程,且小流量工况增幅显著高于大流量,明显改善了小流量工作的不稳定性.对于大流量工况,环形腔室截面变小导致腔室内循环流量降低、沿程损失明显减小,是泵出口扬程提高的主要因素;而对于小流量工况,环形腔室截面变小使得扩散管主流贴近环形腔室,显著降低了叶轮流道扬程损失,有效提升了泵出口扬程.      

大飞机风切变探测告警系统

介绍了国内外在机载风切变告警系统方面的研究进展,通过对比国内外的研究情况,发现由于国内的需求不足,使得在具体产品的研究进展上与国外存在较大差距。由于中国大飞机研究项目的全面展开．也必然为包括机载风切变告警系统在内的、与大飞机有关的各种机载产品的发展提供了很好的机会。指出为了尽快弥补国内研究的差距,需在风切变建模、风切变探测及风切变告警系统的试飞验证方面做出进一步努力。