国产高模量碳纤维抗真空紫外辐照性能试验研究

通过地面模拟试验研究了真空紫外辐照对国产BHM3高模量碳纤维质量损失率的影响,并采用扫描电子显微镜（SEM）、原子力显微镜（AFM）和X射线光电子能谱（XPS）仪对辐照前后的样品进行微观分析。结果表明,随着真空紫外辐照剂量增加,碳纤维质损率呈现先增加后平缓现象,质量损失率较少;紫外辐照作用前后碳纤维表面形貌和元素组成基本未变,说明其具有良好的抗紫外辐照性能。     

基于融合伽马变换全卷积神经网络的火星地貌分割方法

为了让火星巡视器在有限的寿命内能获得更多的科学产出,需要提高巡视器在火星表面的自主通过能力,而火星表面地貌类型是评估巡视器可通过性的重要信息。因此,提出了融合伽马变换的全卷积神经网络(FCN)火星表面地貌分割算法。首先,考虑对巡视器通过性的影响,确认地貌分类的类型,基于好奇号拍摄的火星地表图像Mars32K数据库,构建地貌分割数据集;其次,使用自适应伽马变换(AGT)对灰度单一的火星图像进行预处理,减弱了光照等因素干扰;最后,利用数据集训练一个FCN,以实现对火星表面地貌的分割预测。仿真结果表明:网络测试准确率达到83.03%,地形分割预测结果可靠,验证了方法的可行性。     

Aero-engine fault diagnosis applying new fast support vector algorithm

A new fast learning algorithm was presented to solve the large-scale support vector machine ( SVM ) training problem of aero-engine fault diagnosis.The relative boundary vectors ( RBVs ) instead of all the original training samples were used for the training of the binary SVM fault classifiers.This pruning strategy decreased the number of final training sample significantly and can keep classification accuracy almost invariable.Accordingly , the training time was shortened to 1 / 20compared with basic SVM classifier.Meanwhile , owing to the reduction of support vector number , the classification time was also reduced.When sample aliasing existed , the aliasing sample points which were not of the same class were eliminated before the relative boundary vectors were computed.Besides , the samples near the relative boundary vectors were selected for SVM training in order to prevent the loss of some key sample points resulted from aliasing.This can improve classification accuracy effectively.A simulation example to classify 5classes of combination fault of aero-engine gas path components was finished and the total fault classification accuracy reached 96.1%.Simulation results show that this fast learning algorithm is effective , reliable and easy to be implemented for engineering application.     

航天器天文导航模糊自适应卡尔曼滤波研究

星光折射间接敏感地平的自主天文导航方法能够获得很高的导航精度,但由于大气密度模型时空分辨率不高,这种方法所敏感的地平有可能出现较大的瞬时误差,从而导致导航滤波器精度降低,有时甚至发散.为了解决这一问题,提出将模糊推理系统应用于自主天文导航,研究基于Unscented卡尔曼滤波的模糊自适应算法,使导航滤波器在观测值异常时具有一定的自适应能力.计算机仿真结果验证了该方法的有效性.      

直流磁控溅射ZnO:Al薄膜的光电和红外发射特性

以锌、铝合金(ω(Al)=3%)为靶材,利用直流反应磁控溅射法制备了系列掺铝氧化锌ZnO:Al(ZAO)薄膜样品,通过X射线衍射(XRD)、扫描电子显微镜(SEM)、分光光度计、霍耳效应及红外发射率测量仪等测试仪器或方法表征了样品的结构、形貌、光学、电学及红外发射特性.测得样品最低电阻率达到1.8×10^-6(Ω·m),最大禁带宽度为3.47?eV,可见光区平均透过率达到90%,8~14?μm波段平均红外发射率在0.26~0.9之间.上述特性均随衬底温度和溅射功率的变化有着规律的变化.当方块电阻小于45?Ω时,薄膜在8~14?μm波段平均红外发射率与方块电阻遵循二阶函数变化规律.     

Understanding high-density matter through analysis of surface spectral lines and burst oscillations from accreting neutron stars

We discuss millisecond period brightness oscillations and surface atomic spectral lines observed during type I X-ray bursts from a neutron star in a low mass X-ray binary system. We show that modeling of these phenomena can constrain models of the dense cold matter at the cores of neutron stars. We demonstrate that, even for a broad and asymmetric spectral line, the stellar radius-to-mass ratio can be inferred to better than 5%. We also fit our theoretical models to the burst oscillation data of the low mass X-ray binary XTE J1814-338, and find that the 90% confidence lower limit of the neutron star’s dimensionless radius-to-mass ratio is 4.2.     

Clusters of Galaxies: Setting the Stage

Clusters of galaxies are self-gravitating systems of mass ∼10¹⁴–10¹⁵ h ⁻¹ M_⊙ and size ∼1–3h ⁻¹ Mpc. Their mass budget consists of dark matter (∼80%, on average), hot diffuse intracluster plasma (≲20%) and a small fraction of stars, dust, and cold gas, mostly locked in galaxies. In most clusters, scaling relations between their properties, like mass, galaxy velocity dispersion, X-ray luminosity and temperature, testify that the cluster components are in approximate dynamical equilibrium within the cluster gravitational potential well. However, spatially inhomogeneous thermal and non-thermal emission of the intracluster medium (ICM), observed in some clusters in the X-ray and radio bands, and the kinematic and morphological segregation of galaxies are a signature of non-gravitational processes, ongoing cluster merging and interactions. Both the fraction of clusters with these features, and the correlation between the dynamical and morphological properties of irregular clusters and the surrounding large-scale structure increase with redshift. In the current bottom-up scenario for the formation of cosmic structure, where tiny fluctuations of the otherwise homogeneous primordial density field are amplified by gravity, clusters are the most massive nodes of the filamentary large-scale structure of the cosmic web and form by anisotropic and episodic accretion of mass, in agreement with most of the observational evidence. In this model of the universe dominated by cold dark matter, at the present time most baryons are expected to be in a diffuse component rather than in stars and galaxies; moreover, ∼50% of this diffuse component has temperature ∼0.01–1 keV and permeates the filamentary distribution of the dark matter. The temperature of this Warm-Hot Intergalactic Medium (WHIM) increases with the local density and its search in the outer regions of clusters and lower density regions has been the quest of much recent observational effort. Over the last thirty years, an impressive coherent picture of the formation and evolution of cosmic structures has emerged from the intense interplay between observations, theory and numerical experiments. Future efforts will continue to test whether this picture keeps being valid, needs corrections or suffers dramatic failures in its predictive power.     

Cosmological Shock Waves

Large-scale structure formation, accretion and merging processes, AGN activity produce cosmological gas shocks. The shocks convert a fraction of the energy of gravitationally accelerated flows to internal energy of the gas. Being the main gas-heating agent, cosmological shocks could amplify magnetic fields and accelerate energetic particles via the multi-fluid plasma relaxation processes. We first discuss the basic properties of standard single-fluid shocks. Cosmological plasma shocks are expected to be collisionless. We then review the plasma processes responsible for the microscopic structure of collisionless shocks. A tiny fraction of the particles crossing the shock is injected into the non-thermal energetic component that could get a substantial part of the ram pressure power dissipated at the shock. The energetic particles penetrate deep into the shock upstream producing an extended shock precursor. Scaling relations for postshock ion temperature and entropy as functions of shock velocity in strong collisionless multi-fluid shocks are discussed. We show that the multi-fluid nature of collisionless shocks results in excessive gas compression, energetic particle acceleration, precursor gas heating, magnetic field amplification and non-thermal emission. Multi-fluid shocks provide a reduced gas entropy production and could also modify the observable thermodynamic scaling relations for clusters of galaxies.     

Evaluation of the contribution of different types of galaxies to the cosmic diffuse background based on γ-ray observations

The relative contribution to the γ-ray background of different types of sources, namely Seyfert Galaxies, Quasars, BL Lac objects, radio galaxies and field galaxies is estimated under the hypothesis that the cosmic diffuse flux is the result of a superposition of many unresolved galaxies. The γ-ray data indicate that the Seyfert volume emissivity matches that of the diffuse background at few hundred keV and exceeds it at higher energies by as much as a factor of about 4. Whilst normal galaxies contribute less than 0.1%, BL Lac objects, Quasars and Radio Galaxies may contribute as much as 5–10% each, even without significant evolution. In this paper we explore different ways of reconciling the observational data on active galaxies with the measured diffuse background level.     

Future Instrumentation for the Study of the Warm-Hot Intergalactic Medium

We briefly review capabilities and requirements for future instrumentation in UV- and X-ray astronomy that can contribute to advancing our understanding of the diffuse, highly ionised intergalactic medium.