A model of foreground emission in UV using GALEX deep observations

Foreground emission, mainly airglow and zodiacal light, is a significant contributor in an ultraviolet observation especially from low earth orbit. Its careful estimation and removal are tedious yet unavoidable processes in the study of diffuse UV radiation and by extension interstellar dust studies. Our analysis of deep GALEX observations show that airglow is not only a function of Sun angle but also a strong function of Solar activity at the time of observation. We present here an empirical model of airglow emission, derived from GALEX deep observations, as a function of 10.7 cm Solar flux and Sun angle. We obtained the model by training machine learning models on the data using a variant of the regression algorithm that is both resilient toward outlier data and sensitive to the complexities of the provided data. Our model predictions across various observations show no loss in generalization as well as good agreement with the observed values. We find that the total airglow in an observation is the sum of a baseline part (AG_c) that depends on the Solar flux and Sun angle, and a variable part (AG_v) that depends on the Sun angle and the time of observation with respect to local midnight. We also find that the total airglow can vary between 85 – 390 photon units in FUV and 80 – 465 photon units in NUV.     

Investigations of entrainment characteristics and shear-layer vortices evolution in an axisymmetric rear variable area bypass injector

In this study,firstly,for the axisymmetric RVABI,the change-rule of adverse pressure gradient caused by radial velocity during the transition of internal flow mode in variable geometry is summarized,and a Bypass Ratio(BR) iterative algorithm based on the empirical correlation of non-equilibrium pressure is proposed.The algorithm can estimate the nonlinear relationship between area ratio and BR,with an error range falling below 6.5%.Then,we discuss the favorable effect of uniform mixing on the th...     

轴承钢等离子体基离子注碳复合改性层化学结构的研究

通过激光Ｒａｍａｎ光谱、Ｘ射线光电子谱以及电阻和显微硬度的测试，研究了ＧＣｒ１５钢及镀钛ＧＣｒ１５钢试样经乙等离子基离子注入所得表面改性层的化学结构。     

低压涡轮导向器开度对变循环发动机的影响

建立了变循环发动机整机模型并对可变几何低压涡轮特性进行修正，研究了低压涡轮导叶开度从-6°～6°时对各部件以及发动机整体性能的影响。结果表明：随低压涡轮导向器角度变大，低压涡轮进口折合流量增大，不论低压涡轮导向器开大或关小，高、低涡轮效率均下降；随导叶开度增大，高压涡轮膨胀比增大，高压轴功率增大，高压压气机（High pressure compressor,HPC）与核心机驱动风扇级（Core driven fan stage,CDFS）压比增大；双外涵模式下涡轮导叶角度为0°时单位推力最大，单外涵模式下涡轮角度为-1°时单位推力最大。     

非接触式低无源互调温箱穿仓接口技术

高低温循环状态下的无源互调（passive intermodulation, PIM）检测是全面评估航天微波产品PIM性能的必要手段，传统的温箱穿仓波导连接方式在温循PIM检测中时常出现因应力、温变等因素导致检测系统残余PIM恶化的问题，严重影响检测灵敏度和检测效率。针对此，提出一种非接触式低PIM温箱穿仓接口技术。在温箱穿仓部位利用非接触电磁屏蔽原理构建非接触式端口，避免了不良电接触，以实现温箱内外快速稳定的低PIM电连接。理论分析了其中非接触结构的PIM抑制特性，针对Ku频段应用设计研制了温箱穿仓接口并开展了实验验证，实测在长时间温循状态下系统3阶残余PIM＜-140dBm@2×100W，获得了稳定的低残余PIM特性，大幅提升了PIM检测性能和检测效率，可广泛推广于各类PIM检测系统应用中。     

航材后续备件订货周期优化研究

针对目前部队航材备件订货周期方面存在的问题以及在理论研究方面存在的不足,以故障统计数据为基础,建立了一种新型的数学模型,解决了一定保障率的情况下使得订货周期更加合理,保障经费最小的问题.     

对转涵道风扇桨叶高效设计方法

基于叶素动量理论的对转涵道风扇桨叶设计方法虽然设计速度快，但设计精度不高。为提高设计方法的设计精度，同时保留设计的快速性，通过CFD计算对基于叶素动量理论的桨叶快速设计方法进行修正，提出一种耦合CFD修正的对转涵道风扇桨叶高效设计方法。通过CFD计算与修正设计的不断迭代，可使设计结果收敛至CFD计算结果，得到满足设计要求的桨叶。结果表明：MRF方法对对转涵风扇性能的求解精度不足，需采用非定常CFD方法。而通过CFD计算结果修正桨叶的拉力占比、入流角及叶素气动力后，对转涵道风扇总拉力设计精度提高10.4%，扭矩设计精度提高18.2%。文中提出的高效设计方法只需进行少量的CFD计算修正便能较好地满足设计要求，进行加速处理后，设计效率进一步提高25%。     

Statistical analysis of the occurrence rate of geomagnetic storms during solar cycles 20–24

This study examines the occurrences rate of geomagnetic storms during the solar cycles (SCs) 20–24. It also investigates the solar sources at SCs 23 and 24. The Disturbed storm time (Dst) and Sunspot Number (SSN) data were used in the study. The study establishes that the magnitude of the rate of occurrences of geomagnetic storms is higher (lower) at the descending phases (minimum phases) of solar cycle. It as well reveals that severe and extreme geomagnetic storms (Dst < -250 nT) seldom occur at low solar activity but at very high solar activity and are mostly associated with coronal mass ejections (CMEs) when occurred. Storms caused by CME + CH-HSSW are more prominent during the descending phase than any other phase of the solar cycle. Solar minimum features more CH-HSSW- associated storms than any other phase. It was also revealed that all high intensity geomagnetic storms (strong, severe and extreme) are mostly associated with CMEs. However, CH-HSSW can occasionally generate strong storms during solar minimum. The results have proven that CMEs are the leading cause of geomagnetic storms at the ascending, maximum and the descending phases of the cycles 23 and 24 followed by CME + CH-HSSW. The results from this study indicate that the rate of occurrence of geomagnetic storms could be predicted in SC phases.     

On the time lag between solar wind dynamic parameters and solar activity UV proxies

The solar activity displays variability and periodic behaviours over a wide range of timescales, with the presence of a most prominent cycle with a mean length of 11 years. Such variability is transported within the heliosphere by solar wind, radiation and other processes, affecting the properties of the interplanetary medium. The presence of solar activity–related periodicities is well visible in different solar wind and geomagnetic indices, although their time lags with respect to the solar cycle lead to hysteresis cycles. Here, we investigate the time lag behaviour between a physical proxy of the solar activity, the Ca II K index, and two solar wind parameters (speed and dynamic pressure), studying how their pairwise relative lags vary over almost five solar cycles. We find that the lag between Ca II K index and solar wind speed is not constant over the whole time interval investigated, with values ranging from 6 years to $～$1 year (average 3.2 years). A similar behaviour is found also for the solar wind dynamic pressure. Then, by using a Lomb-Scargle periodogram analysis we obtain a 10.21-year mean periodicity for the speed and 10.30-year for the dynamic pressure. We speculate that the different periodicities of the solar wind parameters with respect to the solar 11-year cycle may be related to the overall observed temporal evolution of the time lags. Finally, by accounting for them, we obtain empirical relations that link the amplitude of the Ca II K index to the two solar wind parameters.