Study of the magnetospheres of active regions on the sun by radio astronomy techniques

In the 1990s, based on detailed studies of the structure of active regions (AR), the concept of the magnetosphere of the active region was proposed. This includes almost all known structures presented in the active region, ranging from the radio granulation up to noise storms, the radiation of which manifests on the radio waves. The magnetosphere concept, which, from a common point of view, considers the manifestations of the radio emission of the active region as a single active complex, allows one to shed light on the relation between stable and active processes and their interrelations. It is especially important to identify the basic ways of transforming nonthermal energy into thermal energy. A dominant role in all processes is attributed to the magnetic field, the measurement of which on the coronal levels can be performed by radio-astronomical techniques. The extension of the wavelength range and the introduction of new tools and advanced modeling capabilities makes it possible to analyze the physical properties of plasma structures in the AR magnetosphere and to evaluate the coronal magnetic fields at the levels of the chromosphere–corona transition zone and the lower corona. The features and characteristics of the transition region from the S component to the B component have been estimated.     

Interplanetary scintillations of the radio source ensemble at the maximum of cycle 24 of solar activity

The results of the interplanetary scintillation observations performed in the period of the maximum of solar activity from April 2013 to April 2014 on the BSA LPI radio telescope at the frequency 111MHz are presented. Fluctuations of the radio emission flux were recorded round the clock for all sources with a scintillating flux of more than 0.2 Jy falling in a strip of sky with a width of 50° over declinations corresponding to a 96-beam directional pattern of the radio telescope. The total number of sources observed during the day reaches 5000. The processing of the observational data was carried out on the assumption that a set of scintillating sources represents a homogeneous statistical ensemble. Daily two-dimensional maps of the distribution of the level of scintillations, whose analysis shows the strong nonstationarity and large-scale irregularity of the spatial distribution of solar wind parameters, were constructed. According to maps of the distribution of the level of scintillations averaged over monthly intervals, the global structure of the distribution of the solar wind was investigated in the period of the maximum of solar activity, which was found to be on the average close to spherically symmetric. The data show that on a spherically symmetric background an east–west asymmetry is observed, which indicates the presence of a large-scale structure of a spiral type in the solar wind.     

A general calculation method to specify center-of-buoyancy for the stratospheric airship with multiple gas cells

As the lighter-than-air (LTA) flight vehicle, the stratospheric airship is a desirable platform to provide communication and surveillance services. During the ascent from sea-level to the mission altitude, the volume of the lifting gas may change significantly, which will result in the change of the center-of-buoyancy (CB). A general calculation method is developed to specify CB for the stratospheric airship with a double-ellipsoid hull and an arbitrary number of the gas cells. The cross-section-integral (CSI) method is used as a basic calculation scenario to specify CB. Considering the complexity in determining the boundary between the helium and air in the gas cell, a searching algorithm is put forward and the specification of CB can be conducted by the iterative calculation. As an important application, the stable condition of the pitch angle is analyzed when the change of CB is involved. Under different initial configurations, the stable pitch angle of the stratospheric airship during the ascent is specified and compared, which shows the advantages of the multi-gas-cell configuration. The results of this paper may provide an important reference for the engineering application of the stratospheric airship.     

Determination of Gas-Generator Fuel Capacity for Hybrid Aerial Underwater Vehicles with Airfoil Cavity-Forming System

We determine the behavior of onboard gas-generator flowrate for generating the cavitation flow around a hybrid aerial underwater vehicle by using an annular wing on the underwater trajectory section.     

基于调平回路的LESO抗干扰方法研究

针对平台台体转位过程中方位角速度对水平通道调平回路的干扰问题,提出了惯导平台调平回路抗干扰方法.将线性扩张状态观测器(LESO)应用于调平回路中,对干扰进行估计并实时补偿.基于调平回路模型,对LESO进行设计及仿真分析.仿真结果表明,LESO能准确估计干扰且动态补偿效果好,较原系统具有更强的抑制干扰能力.     

空间压力容器可靠性定量设计方法研究

针对空间压力容器常规设计方法难以满足航天技术快速发展对轻质量、低成本、高可靠的需求,基于可靠性理论中应力-强度干涉模型,建立空间压力容器可靠性设计数学模型。结合某型号钛合金球形气瓶随机变量统计数据,开展了气瓶可靠性定量设计。计算结果表明,可靠性定量设计方法能够给出产品可靠度定量指标,并在一定程度上降低空间压力容器结构重量。     

PSO-LSSVM在民机气动性能数学建模上的应用

目前风洞试验仅为民用飞机飞行性能提供有限数据.全飞行包线的技术支持对于民机飞行试验十分重要,需要采用数学建模和参数辨识的方法.选择合适的机器学习算法是参数辨识中最为关键的一步.支持向量机(SVM)采用结构风险最小化原理,尤其适用于小样本情形.根据A320非巡航起降阶段的几组真实数据,以及全机气动力估算的结果,使用最小二乘支持向量机建立预测模型.随后采用粒子群算法优化模型参数从而提升泛化能力.由此实现民机飞行包线的气动性能整体建模与辨识.与Ma=0.78时的实验数据相比较,PSO-LSSVM模型的预测结果吻合,是一种有效的气动数学建模方法.     

一种修正的Osher通量在高阶WCNS中的特性

将一种基于多维修正的Osher通量运用于高阶加权紧致非线性格式(WCNS)中,该修正通量主要在垂直于激波面的界面上增加耗散,能够改善Osher通量的激波捕捉稳定性,同时对边界层和接触间断的分辨率影响非常小。对修正的Osher通量在高阶WCNS中的特性进行研究,通过数值模拟测试了基于Osher通量的WCNS的激波稳定性、热流预测精度、边界层模拟能力、激波边界层干扰模拟能力,并与Steger-Warming通量和Roe通量进行了对比。结果表明修正后的Osher通量比Harten修正的Roe通量具有更好的激波捕捉鲁棒性,而边界层、驻点热流值和激波边界层干扰的模拟则明显优于Steger-Warming通量。上述结果说明了基于修正的Osher通量的高阶WCNS具有较好的激波捕捉特性、热流预测精度和边界层计算能力。     

Numerical scheme of the second order of accuracy for vortex methods for incompressible flow simulation around airfoils

A high-accuracy numerical scheme is proposed for vortex methods of flow simulation around airfoils of arbitrary shape including airfoils with sharp edges, because it does not require the solution continuity on the airfoil.