A new parameter to define interplanetary coronal mass ejections

The interplanetary manifestations of coronal mass ejections, ICMEs, have many signatures in the solar wind but none of these signatures in the velocity, density, temperature, magnetic field, plasma composition or energetic particles uniquely and unambiguously identifies the occurrence of an ICME. Different investigators identify different events when confronted with the same data. Herein, we present a single physical parameter that combines information from multiple plasma components and that holds the promise of defining a beginning and an end of the region of influence ICME and an indication of the location of the encounter with the ICME relative to its central meridian. This parameter is the total plasma pressure perpendicular to the magnetic field, consisting of the sum of the magnetic pressure and plasma kinetic or thermal pressure. It provides a vehicle for classifying the nature of the ICME encounter and, in many cases, provides an unambiguous start and stop time of the event. However, it does not provide a start and stop time for any embedded flux rope. This identification depends on examination of the magnetic field.     

Orbital phase spectroscopy of X-ray pulsars to study the stellar wind of the companion

High Mass X-ray Binary Pulsars (HMXBP), in which the companion star is a source of supersonic stellar wind, provide a laboratory to probe the velocity and density profile of such winds. Here, we have measured the variation of the absorption column density along with other spectral parameters over the binary orbit for two HMXBP in elliptical orbits, as observed with the Rossi X-ray Timing Explorer (RXTE) and the BeppoSAX satellites. A spherically symmetric wind profile was used as a model to compare the observed column density variations. In 4U 1538-52, we find the model corroborating the observations; whereas in GX 301-2, the stellar wind appears to be very clumpy and a smooth symmetric wind model seems to be inadequate in explaining the variation in column density.     

Prediction of geosynchronous electron fluxes using an artificial neural network driven by solar wind parameters

There are hundreds of satellites operating at the geosynchronous (GEO) orbit where relativistic electrons can cause severe damage. Thus, predicting relativistic electron fluxes is significant for spacecraft safety. In this study, using GOES satellite data during 2011–2020, we propose two neural network models with two hidden layers to predict geosynchronous relativistic electron fluxes at two energy channels (>0.8 MeV and > 2 MeV). The number of input neurons of the two channels (>0.8 MeV and > 2 MeV) are determined to be 36 and 44, respectively. The > 0.8 MeV model has 22 and 9 neurons in the hidden layers, while the > 2 MeV model has 25 and 15 neurons in the hidden layers. The input parameters include the north–south component of the interplanetary magnetic field, solar wind speed, solar wind dynamic pressure and solar wind proton density. Through the analysis of different time delays, we determine that the optimal time delays of two energy channels (>0.8 MeV and > 2 MeV) are 8 days and 10 days, respectively. The training set and validation set (Jan 2011-Dec 2018) are divided by the 10-fold cross-validation method, and the remaining data (Jan 2019-Feb 2020) is used to analyze the model performance as a test set. The prediction results of both energy channels show good agreement with satellite observations indicated by low RMSE (～0.3 cm^-2sr^-1s^?1), high PE (～0.8) and CC (～0.9). These results suggest that only using solar wind parameters is capable of obtaining reasonable predictions of geosynchronous relativistic electron fluxes.     

基于改进SSD的风机叶片表面缺陷检测方法

针对无人机对风机叶片表面缺陷检测中出现的多尺度目标问题,本文提出一种基于改进SSD的风机叶片缺陷检测方法。以具有多尺度结构框架的目标检测模型SSD为基础,引入残差网络ResNet50作为其特征提取网络,用以获取更深层次的细节特征信息,从而提升缺陷检测模型的整体效果。在建立的风机叶片表面缺陷图像数据集下进行模型验证,结果表明,该方法的平均精确度mAP@.5为84.29%,与YOLOv3和RetainNet相比,对各类型缺陷的平均精确度分别提高了2.92%和8.69%,同时较传统SSD算法平均精确度提升了2.21%。     

风螺旋线精确算法在程序转弯模板中的应用

程序转弯是航空器进场阶段使用的一种反向飞行程序,程序转弯模板是用来量化转弯区范围的一种复杂图形,模板的主体由风螺旋线构成.传统模板绘制是基于手工做图的方法来实现,步骤复杂,不利于计算机的自动化处理.通过引入风螺旋线精确算法,可以准确实现程序转弯模板中的风螺旋线绘制、公切线计算,以及风螺旋线的趋势分析,使飞行程序模板的计算过程得到较大的简化,为计算机的自动化处理提供理论参考.     

高超声速风洞压敏漆试验技术

提出了适用于高超声速风洞开展压敏漆(PSP)试验研究的关键技术及解决办法。采用自主设计的PSP校准系统及测试系统,考核了代号为EC-PSP的压力敏感涂料在高超声速条件下的适用性、图像处理软件功能以及高温条件影响下数据处理方法的可行性。以压缩拐角模型为例开展了马赫数为5的高超声速PSP技术验证性风洞试验研究,辅以红外测温方法获得模型表面连续温度分布。试验结果表明在高超声速风洞开展的PSP试验技术研究清晰地捕获了基于压力变化的压缩拐角模型表面流动特征,实现了连续压力分布的测量。     

Modeling of the outer heliosphere with the realistic solar cycle

Time-dependent kinetic-continuum model of the solar wind interaction with the two-component local interstellar cloud (LIC) has been developed recently [Izmodenov, V., Malama, Y.G., Ruderman, M.S. Solar cycle influence on the interaction of the solar wind with local interstellar cloud. Astron. Astrophys. 429, 1069–1080, 2005a.]. Here, we adopted this model to the realistic solar cycle, when the solar wind parameters at the Earth’s orbit are taken from space data. This paper focuses on the results related to the termination shock (TS) excursion with the solar cycle that may help to understand Voyager 1 data obtained at and after the crossing of the termination shock and to predict the time of the TS crossing by Voyager 2.     

一种翼身融合飞行器的失速特性研究

翼身融合（BWB）布局飞行器作为下一代商用飞机的主要构型之一，越来越受到重视。对于翼身融合飞行器的研究主要针对其巡航状态的特性，而对其失速特性的研究较少。对一种翼身融合客机构型进行风洞试验研究，采用测力试验方法对其无增升装置的构型，以及具有翼梢小翼、前缘缝翼和机身上部双吊舱的组合部件构型下的纵向特性进行研究，特别是对其失速特性的分析，并通过二维粒子图像测试技术以及油流试验对其失速过程的流动机理进行研究。结果表明，无增升装置的基本构型下，翼身融合飞行器可以保持低速飞行，而各组合构型都具有提高最大升力系数的作用。对失速过程的分析表明，随着迎角的增大，飞机表面流场分离区域从翼梢开始逐渐向翼根以及机身发展，当外翼段完全处于分离区域时，飞机并不会马上失速，因为中心体同样具有提供升力的作用，且中心体的流动分离较外翼的流动分离更晚，所以当外翼在失速迎角出现升力损失时可以通过中心体的升力进行补偿，维持其低速飞行状态，真正的失速发生在中心体出现流动分离之后。     

A polytropic model for the solar wind

The solar wind fills the heliosphere and is the background medium in which coronal mass ejections propagate. A realistic modelling of the solar wind is therefore essential for space weather research and for reliable predictions. Although the solar wind is highly anisotropic, magnetohydrodynamic (MHD) models are able to reproduce the global, average solar wind characteristics rather well. The modern computer power makes it possible to perform full three dimensional (3D) simulations in domains extending beyond the Earth’s orbit, to include observationally driven boundary conditions, and to implement even more realistic physics in the equations. In general, MHD models for the solar wind often make use of additional source and sink terms in order to mimic the observed solar wind parameters and/or they hide the not-explicitly modelled physical processes in a reduced or variable adiabatic index. Even the models that try to take as much as possible physics into account, still need additional source terms and fine tuning of the parameters in order to produce realistic results. In this paper we present a new and simple polytropic model for the solar wind, incorporating data from the ACE spacecraft to set the model parameters. This approach allows to reproduce the different types of solar wind, where the simulated plasma variables are in good correspondence with the observed solar wind plasma near 1 AU.