Soft gamma repeaters

The observational properties of the soft gamma repeaters are reviewed briefly, starting with the time histories and energy spectra of their bursts. The short bursts and giant flares are compared. Their quiescent emission is presented, and the context of the magnetar model is discussed.     

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.     

Partition method for improvement of piecewise linear model with full envelope covered

Since ambient conditions vary in a wide range within the full flight envelope, the existing piecewise linear model (PLM), which is based on sea-level static condition with use of corrected parameters for other points in the flight envelope, cannot meet the accuracy for replacing the nonlinear model. To obtain more accurate linear models, a method of partitioning the flight envelope over a grid of Mach number and altitude boxes was suggested. Then, a set of linear models for a given operating condition was selected by picking the nearest (Mach number, altitude) box in the flight envelope. Through the selected set of linear models, interpolating for power level based on a weighted sum of corrected rotor speeds can obtain a linear model with acceptable accuracy. Simulation results of different points within the full flight envelope showed that the maximum error between nonlinear model and the existing PLM was more than 50%, while the maximum error between nonlinear model and the improved PLM was within 8%. It is concluded that the improved PLM performs accurately, especially under the non-standard conditions. In addition, the improved PLM can satisfy the real-time requirement better than the existing PLM.      

民用飞机阵风载荷及减缓技术的研究

由于民用飞机机翼具有大展弦比的特点,因此阵风载荷经常成为民用飞机飞行载荷的严重情况,是各国适航标准重点考察的飞行情况。而且,阵风干扰还会因飞机机体的自身弹性引起结构弹性振动,使飞机结构刚度降低,造成机体疲劳损伤,甚至引起颤振。因此,在民用飞机载荷设计过程中对阵风载荷及其减缓技术进行研究具有非常重要的意义。介绍了民用飞机阵风载荷的原理及相关技术,以及阵风载荷减缓技术中用直接升力控制方法来实现机翼的阵风载荷减缓。     

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.     

某机载短波干扰飞机控制系统机理研究

文中以系统级电磁干扰测试试验为基础,利用HFSS软件对短波发射时飞机典型位置场强分布、短波馈线电流分布等进行数值仿真。最终定义了机载短波干扰飞机控制系统的机理,并为后续的解决措施的提出及验证提供了理论支持。这种分析电磁干扰机理的方法对实际工程有很大的参考价值。     

Determination of Sulfur Abundance in the Solar Wind

Solar chemical abundances are determined by comparing solar photospheric spectra with synthetic ones obtained for different sets of abundances and physical conditions. Although such inferred results are reliable, they are model dependent. Therefore, one compares them with the values for the local interstellar medium (LISM). The argument is that they must be similar, but even for LISM abundance determinations models play a fundamental role (i.e., temperature fluctuations, clumpiness, photon leaks). There are still two possible comparisons—one with the meteoritic values and the second with solar wind abundances. In this work we derive a first estimation of the solar wind element ratios of sulfur relative to calcium and magnesium, two neighboring low-FIP elements, using 10 years of CELIAS/MTOF data. We compare the sulfur abundance with the abundance determined from spectroscopic observations and from solar energetic particles. Sulfur is a moderately volatile element, hence, meteoritic sulfur may be depleted relative to non-volatile elements, if compared to its original solar system value.     

某离心式喷嘴雾化特性及优化设计研究

喷嘴结构参数、喷油压降和燃油物性对喷嘴雾化特性具有重要影响。采用数值计算和试验手段研究某离心式喷嘴航空煤油和0#柴油雾化特性及差异性,并讨论喷嘴内部流动和喷嘴结构参数对雾化特性的影响。结果表明:数值计算与试验值存在差异,但雾化锥角、流量系数等随压力变化的趋势一致,验证了流体体积函数(VOF)追踪油气两相界面的正确性;喷嘴内部气、液相的涡是内部流动不稳定和气液面波动的原因;几何结构参数对喷嘴雾化特性影响明显;优化后的喷嘴结构,流量系数和雾化锥角分别增大了0.15和0.16倍,而喷嘴出口液膜厚度减小了0.53倍,明显改善了该喷嘴的雾化质量。     

高超侧压式进气道参数分析及试验研究

分析了高超侧压式进气过第一、二溢流窗的溢流角随后掠角的变化规律，分析了溢流窗气流与主流相互作用而形成一道脱体曲面激波的原因，设计了侧压角为６°，后掠角３０°的直前缘及圆弧前缘两套高超侧压式进气道，在Ｍ５．３风洞中利用风洞壁面自然发展的附面层进行非均匀来流下进气道起动性能及总体性能试验，试验发现大量附面层吸入不仅对起动性能有重大影响，而且对总压恢复影响也极大。     

Galactic Evolution of D and 3He

The most recent chemical evolution models for D and 3He are reviewed and their results compared with the available data.Models in agreement with the major galactic observational constraints predict deuterium depletion from the Big Bang to the present epoch smaller than a factor of 3 and therefore do not allow for D/H primordial abundances larger than 5 × 10-5. Models predicting higher D consumption do not seem to be able to reproduce other observed features of our galaxy (e.g. SFR, abundances, abundance ratios and/or gradients of heavier elements, metallicity distribution of G-dwarfs).Observational and theoretical 3He abundances can be reconciled with each other if the majority of low mass stars experience in the red giant phase a deep mixing allowing the consumption of most of the 3He produced during core-hydrogen burning.