地面效应下的不同翼型亚声速气动特性分析

采用数值方法研究了亚声速地面效应条件下不同翼型的气动特性,进一步以Ma=0.5来流工况为例,研究了翼型参数和飞行高度对气动特性的影响。计算结果表明在Ma为0.5、迎角为6°的地效情况下,翼型弯度减小,更容易在翼型前缘产生激波阻力;翼型下翼面后缘弯度增大使得后缘压力更高,升力系数和低头力矩相应增大;随着飞行高度的减小,地效作用加强,翼型下翼面压力增大,下翼面的升力增量大于上翼面吸力损失,机翼升力系数和升阻比增加越来越显著。     

Comparative anatomy of the day- and night-time radar echoes from the 130–170 km region of the low latitude ionosphere

Recent observations of daytime 150 km echoes made from Gadanki have revealed ‘descending layer type’ echoing pattern, which are remarkably different from their well known ‘necklace’ pattern. These descending layer type echoing pattern have close resemblance to those of the nighttime valley region echoes that are presumably linked with the intermediate layer formed by the meridional wind shear associated with the semidiurnal/terdiurnal tidal winds. The observed close resemblance between the two echoing patterns reminds the plausible role of the semidiurnal/terdiurnal tidal wind and metallic ions in the governing physical processes. We present a comparative anatomy of these two echoing phenomena by making a close examination of the radar observations from Gadanki. Importantly, we bring out the similarities and dissimilarities in their characteristics and discuss the results in the light of currently available theoretical frameworks in an effort to further our understanding on the origin of these echoing phenomena, which have been addressed so far in isolation.     

一种应用Partial Hausdorff 距离的多尺度图像配准方法

基于图像边缘特征提取的PartialHausdorff距离的配准方法,可以有效抑制由于多传感器的成像特性差异、边缘特征提取等原因对配准的影响。本文对基于PartialHausdorff距离的图像配准方法作了改进,采用多尺度的配准方法,避免了PartialHausdorff距离准则引起的无值和多值性问题,而且显著减少了计算量,实现了PartialHausdorff距离准则对于图像配准的优点。     

小型部分进气亚声速涡轮流动损失研究及优化

为拓展某小型部分进气亚声速涡轮的应用能力,要求进一步提高其气动性能。使用Numeca商用计算流体力学软件建立了原型部分进气涡轮流道的全环域网格,进行了流场的粘性数值仿真,通过与相同叶型全周进气式涡轮的流场对比分析,揭示了部分进气式涡轮的流动机理和流动损失分布规律。在流场结构研究的基础上,对原型涡轮的动叶进行了改型优化,将动叶叶型由原来的纯冲击式叶型改为略带反力度的叶型,流场仿真结果表明涡轮效率提高了5个百分点。通过对改型前后2种部分进气式涡轮气动参数分布情况的对比分析,表明略带反力度的动叶叶型能有效减小部分进气式涡轮非进气扇区动叶通道内的回流损失,对提高涡轮性能有利,可为同类涡轮的气动设计提供参考。     

部分模糊度固定方法在GNSS/INS紧组合中的应用研究

针对动态环境下GNSS/INS导航定位模糊度固定难的问题,提出了一种基于部分模糊度固定的GNSS/INS紧组合导航定位算法,通过选择模糊度的最优子集进行固定,并利用实测车载实验进行了算法验证.实验结果表明:在开阔环境下,基于部分模糊度固定的GNSS/INS紧组合与基于全模糊度固定的GNSS/INS紧组合算法的定位精度相...     

Sea fog detection based on unsupervised domain adaptation

Sea fog detection with remote sensing images is a challenging task. Driven by the different image characteristics between fog and other types of clouds, such as textures and colors, it can be achieved by using image processing methods. Currently, most of the available methods are datadriven and relying on manual annotations. However, because few meteorological observations and buoys over the sea can be realized, obtaining visibility information to help the annotations is difficult. Considering t...     

Boundary of nighttime ozone chemical equilibrium in the mesopause region: Improved criterion of determining the boundary from satellite data

A modified derivation of the criterion of nighttime ozone chemical equilibrium (NOCE) in the mesopause region is presented. According to 3D model calculations, the improved criterion reproduces the lower boundary of the equilibrium much better than its earlier version. Processing of the SABER/TIMED data of 2021 has shown that the modified criterion elevates the NOCE boundary by ～ 0.1–1.7 km, depending on latitude and season. The proposed method of determining the condition of chemical equilibrium can be used to analyse the equilibrium of many trace gases in the stratosphere and troposphere important for different practical applications.     

Study of UV Ne II line shapes in the cathode sheath of an abnormal glow discharge

We report results of an experimental and theoretical study of complex UV line shapes of Ne II 369.421 nm, Ne II 370.962 nm, Ne II 371.308 nm, and.Ne II 372.711 nm lines in the cathode sheath (CS) region of an abnormal DC glow discharge in pure neon. Two sets of experimental profiles and electric field distributions, one for discharge with tungsten and the other with titanium cathode, were obtained by means of the optical emission spectroscopy (OES) and theoretically studied by the iterative CS kinetic model. It is shown that our theoretical model enables the determination of the most important CS parameters (e.g. the thickness of the CS region, and the theoretical distributions of electric field and gas temperature) and thereupon based accurate theoretical predictions of the experimentally observed profiles of the studied lines.     

Where is the base of the Transition Region? Evidence from TRACE,SDO, IRIS and ALMA observations

Classic solar atmospheric models put the Chromosphere-Corona Transition Region (CCTR) at $～2$ Mm above the ${\tau }_{5000}=1$ level, whereas radiative MHD (rMHD) models place the CCTR in a wider range of heights. However, observational verification is scarce. In this work we review and discuss recent results from various instruments and spectral domains. In SDO and TRACE images spicules appear in emission in the 1600, 1700 and 304 Å bands and in absorption in the EUV bands; the latter is due to photo-ionization of H i and He i, which increases with wavelength. At the shortest available AIA wavelength and taking into account that the photospheric limb is $～0.34$ Mm above the ${\tau }_{5000}=1$ level, we found that CCTR emission starts at $～3.7$ Mm; extrapolating to $\lambda =0$, where there is no chromospheric absorption, we deduced a height of $3.0\pm 0.5$ Mm, which is above the value of 2.14 Mm of the Avrett and Loeser model. Another indicator of the extent of the chromosphere is the height of the network structures. Height differences produce a limbward shift of features with respect to the position of their counterparts in magnetograms. Using this approach, we measured heights of $0.14\pm 0.04$ Mm (at 1700 Å), $0.31\pm 0.09$ Mm (at 1600 Å) and $3.31\pm 0.18$ Mm (at 304 Å) for the center of the solar disk. A previously reported possible solar cycle variation is not confirmed. A third indicator is the position of the limb in the UV, where IRIS observations of the Mg ii triplet lines show that they extend up to $～2.1$ Mm above the 2832 Å limb, while AIA/SDO images give a limb height of $1.4\pm 0.2$ Mm (1600 Å) and $5.7\pm 0.2$ Mm (304 Å). Finally, ALMA mm-$\lambda$ full-disk images provide useful diagnostics, though not very accurate, due to their relatively low resolution; values of $2.4\pm 0.7$ Mm at 1.26 mm and $4.2\pm 2.5$ Mm at 3 mm were obtained. Putting everything together, we conclude that the average chromosphere extends higher than homogeneous models predict, but within the range of rMHD models..     

Shocks and instabilities in the partially ionised solar atmosphere

The low solar atmosphere is composed of mostly neutral particles, but the importance of the magnetic field for understanding observed dynamics means that interactions between charged and neutral particles play a very important role in controlling the macroscopic fluid motions. As the exchange of momentum between fluids, essential for the neutral fluid to effectively feel the Lorentz force, is through collisional interactions, the relative timescale of these interactions to the dynamic timescale determines whether a single-fluid model or, when the dynamic frequency is higher, the more detailed two-fluid model is the more appropriate. However, as many MHD phenomena fundamentally contain multi-time-scale processes, even large-scale, long-timescale motions can have an important physical contribution from two-fluid processes. In this review we will focus on two-fluid models, looking in detail at two areas where the multi-time-scale nature of the solar atmosphere means that two-fluid physics can easily develop: shock-waves and instabilities. We then connect these ideas to observations attempting to diagnose two-fluid behaviour in the solar atmosphere, suggesting some ways forward to bring observations and simulations closer together.