基于SAR的海洋内波参数的自动化检测算法与实现

为解决依靠计算机实现从SAR数据中提取内波参数的问题,从实用的角度出发建立了SAR海洋内波传播方向的自动化检测算法,该方法在多种SAR内波数据中进行了检验,证明了这种方法的有效性和实用性。     

基于核密度估计算法的飞机载荷谱统计技术

受到实际条件限制,现阶段的飞机载荷谱实测均采取小子样实测方法,小子样实测数据是取自真实母体的一个简单样本,很难保证数据的充分性、完整性.传统的均值统计法无法对数据缺陷进行弥补.为了克服小子样数据不足问题,将核密度估计技术用于载荷谱统计,取得了良好效果.介绍了核密度估计的相关理论基础,并以某型机下沉速度谱的统计为例,详细介绍了将核密度估计方法用于载荷谱统计的数学过程.结果显示:核密度估计方法对还原载荷谱原貌、补充小子样数据的不足问题具有良好作用.      

级环境下弯叶片对涡轮气动性能影响数值研究

针对某两级低压涡轮的弯扭叶片进行气动性能影响的数值研究,通过对比分析不同弯角和不同类型弯叶片的流场,认为级环境下弯叶片需根据具体载荷分布条件匹配设计.对于研究两级涡轮,第一级静叶反弯、第二级静叶正弯具有相对最优的气动绝热效率,J型弯相比对称弯改善负荷分配,降低二次流损失和激波损失,且小弯角叶片表面压力分布更均匀,流道中部熵增更小,性能高于大弯角叶片.      

一种大偏距埋入式进气道气动特性试验

对一种大偏距埋入式进气道进行了高速风洞试验研究,得到了该进气道的气动特性,结果表明:①巡航状态时,出口马赫数的变化对进气道性能影响不大,进气道具有较高的巡航性能.②在试验研究的范围内,随飞行马赫数的增加,进气道性能有所下降;攻角的增加对进气道性能有所改善,侧滑角的变化对进气道性能影响不大.③进/发匹配点时,进气道通道内气流脉动功率谱密度分布呈现白噪声特征,在大攻角或偏航条件下进气道气流脉动功率谱密度有明显的峰值.      

考虑耦合损伤的燃气轮机叶片材料高低周复合疲劳寿命研究

燃气轮机叶片在实际工作过程中,受到高低周载荷共同作用而易发生疲劳失效.针对高低周复合疲劳损伤演化和寿命预测比较复杂这一问题,考虑高低周载荷叠加形成的耦合损伤,建立了一种新的高低周复合疲劳寿命预测模型,在此基础之上,引入弱化函数描述某些低幅高周载荷对复合损伤的弱化作用,建立了具有低载强化寿命效应的高低周复合疲劳寿命预测模...     

超声速涡轮动叶设计方法研究

研究了基于2维等熵特征线理论的超声速涡轮叶栅设计方法,通过编程开发了超声速涡轮转子叶栅设计软件,该软件可根据进、出口马赫数及进口气流角设计出需要的超声速涡轮转子叶栅。在此基础上应用FLUENT详细地分析了涡轮转子叶栅流场。结果表明:该流场分布合理,未出现激波、分离等现象,且在高载荷系数下具有较高效率。     

起落架落震试验修正案的影响分析及验证思路研究

起落架是飞机的重要组成部件,起落架缓冲器的设计好坏必须经过落震试验的验证。2001年5月9日FAA颁布的N0．25-103修正案对起落架落震试验要求进行了修订。本文对该修正案提出的原因进行说明,并以修正案的内容为基础,与CCAR-25-R3版进行详细地对比和影响分析;通过对起落架动态特性的解析,提出起落架落震试验修正案的验证思路。结果表明：落震试验方法没有本质变化,但是对于试验目的提出了更为严格的要求。研究结果可为起落架落震试验的验证提供一定的技术参考。     

Energy dependence of the rigidity spectrum of Forbush decrease of galactic cosmic ray intensity

We show that rigidity spectrum of Forbush decrease (Fd) of galactic cosmic ray (GCR) intensity in September 9–23, 2005 clearly depends on energy. We calculated rigidity spectrum of the Fd based on the neutron monitors and Nagoya muon telescope channels’ data divided in three groups according to their cut off rigidities. We found that temporal changes of rigidity spectrum exponent γ are approximately similar for all cut off rigidity groups, but γ values are the larger the higher are cut off rigidities. We conclude that rigidity spectrum of Fd is hard for lower energy range and is soft for the higher energy range. We believe that an energy dependence of the power law rigidity spectrum of Fd is observed owing to the preferential convection–diffusion mechanism during Fd in September 9–23, 2005. It is a reflection of an influence of the temporal changes of the structure of the interplanetary magnetic field (IMF) turbulence in different range of frequency f during Fd. Particularly, a decisive role in formation of the character of the rigidity spectrum belongs to the changes of the exponent ν of the power spectral density (PSD) of the IMF turbulence (PSD ∝ f^−ν). The exponent ν is greater for high frequency region of the IMF turbulence (responsible for scattering of low rigidity particles of GCR), than for low frequency region of the IMF turbulence (being responsible for scattering of higher rigidity particles). Also, we challenge to estimate an existence of slab/2D structure of solar wind turbulence during the Fd in September 9–23, 2005 based on the distribution of average turbulence energy among the IMF’s components.     

Particle acceleration and gamma rays in solar flares: Recent observations and new modeling

Experiments on SMM, GAMMA, Yohkoh, GRANAT, Compton GRO, INTEGRAL, RHESSI and CORONAS-F satellites over the past three decades have provided copious data for fundamental research relating to particle acceleration, transport and energetics of flares and to the ambient abundance of the solar corona, chromosphere and photosphere. We summarize main results of solar gamma-astronomy (including some results of several joint Russian–Chinese projects) and try to appraise critically a real contribution of those results into modern understanding of solar flares, particle acceleration at the Sun and some properties of the solar atmosphere. Recent findings based on the RHESSI, INTEGRAL and CORONAS-F measurements (source locations, spectrum peculiarities, ³He abundance etc.) are especially discussed. Some unusual features of extreme solar events (e.g., 28 October 2003 and 20 January 2005) have been found in gamma-ray production and generation of relativistic particles (solar cosmic rays, or SCR). A number of different plausible assumptions are considered concerning the details of underlying physical processes during large flares: (1) existence of a steeper distribution of surrounding medium density as compared to a standard astrophysical model (HSRA) for the solar atmosphere; (2) enhanced content of the ³He isotope; (3) formation of magnetic trap with specific properties; (4) prevailing non-uniform (e.g., fan-like) velocity (angular) distributions of secondary neutrons, etc. It is emphasized that real progress in this field may be achieved only by combination of gamma-ray data in different energy ranges with multi-wave and energetic particle observations during the same event. We especially note several promising lines for the further studies: (1) resonant acceleration of the ³He ions in the corona; (2) timing of the flare evolution by gamma-ray fluxes in energy range above 90 MeV; (3) separation of gamma-ray fluxes from different sources at/near the Sun (e.g., different acceleration sources/episodes during the same flare, contribution of energetic particles accelerated by the CME-driven shocks etc.); (4) asymmetric magnetic geometry and new magnetic topology models of the near-limb flares; (5) modeling of self-consistent time scenario of the event.     

单模光纤耦合器的传输光谱温度特性

在温变条件下,对光纤光源发出光波经单模光纤耦合器传输后的输出光谱进行了测试.借助测试结果,仿真计算了耦合器的透射光波和耦合光波分别进入Sagnac干涉仪后干涉仪输出信号的误差随温度的变化情况.结果表明:当环境温度发生变化时,耦合器透射光波和耦合光波的平均波长和功率都会发生变化,且透射光波的平均波长和功率的温度稳定性远远高于耦合光波的稳定性;当透射光波作为干涉仪输入光波时,由温变引起的干涉仪输出误差比耦合光波作为输入光波时的误差小一个数量级.