时滞系统内模控制器参数整定方法研究

针对内模原理对时滞系统控制的局限性,利用一阶泰勒级数逼近模型的时 滞部分, 推导了工业上常见的一阶时滞和二阶时滞模型的内模控制参数表达式, 结合 ITAE 指标和系统鲁棒性设计了新的目标函数, 通过对目标函数的寻优实现了内模控制 器参数的整定。仿真结果表明,该方法具有较好的动态跟踪性能、较强的抗干扰性和鲁 棒性,具有一定的工程应用价值。     

一种定量建立主题数据库的算法

本文利用企业模型中的企业活动与实体之间的关系给出了实体组之间的相关系数定义，在此基础上，给出了实体组的分组算法，从而应可以根据主要数据库分划标准把实体划分成实体大组，形成主题数据库。     

混合动力学中一种综合控制指标

本文从环境流体力学角度，结合混合动力学机理，导出了一种新混合综合控制指标。     

Comparison of observed ionospheric vertical TEC over the sea in Indian region with IRI-2016 model

The vertical ionospheric TEC values obtained from GAGAN grid based ionospheric delay correction values over the sea in the Indian equatorial region have been compared with the corresponding values derived from the International Reference Ionosphere model, IRI-2016. The objective of this work is to study the deviation of the vertical TEC derived from the IRI model from ground truths over the sea for different conditions. This will serve the basic intention of assessing the candidature of the IRI model as an alternative ionospheric correction model in navigation receivers in terms of accuracy. We have chosen different solar activity periods, seasons, geomagnetic conditions, locations etc. for our comparison and analysis. The TEC values by the IRI-2016 were compared with the actual measured values for the given conditions and errors were obtained. The measured vertical TEC values at the ionospheric grid points were derived from the GAGAN broadcast ionospheric delay data and used as reference. The IRI model with standard internal functions was used in estimating the TEC at the same ionospheric grid points. The errors in the model derived values are statistically analysed. Broadly, the results show that, for the Indian sector over the sea, the IRI model performs better on quiet days in off equatorial regions, particularly in the northern region. The overall performance degrades for other conditions with the model generally underestimating the true TEC values and most severely in the equatorial region. The performance is worst in this region for the disturbed days of the equinoctial period. The comparison study is also done with the TEC data measured directly by dual frequency GPS receivers. The results were found to be in general agreement with those obtained by comparing the model with GAGAN broadcast data as reference. This study will be useful in considering the IRI-2016 model for real time estimates of TEC as an alternative to the current parametric model in a satellite navigation receiver in absence of other options.     

电动式磁悬浮动量球电磁场耦合分析

本文针对电动式磁悬浮动量球(Electrodynamic suspension reaction sphere, EDSRS)的电磁场耦合进行分析，采用定子绕组的感应电动势评判耦合强度，提出了耦合强度评判指标，作为EDSRS的结构设计约束，以降低电磁场耦合的影响。首先，结合EDSRS的具体结构特点，对多定子之间的电磁场耦合问题进行分析，采用定子电磁场在另一个定子绕组中产生的感应电动势评判耦合强度。然后，对感应电动势产生规律进行分析，提出了耦合强度评判指标，并基于所提评判指标，建立了耦合约束验证流程，作为EDSRS的结构设计约束，最后，通过有限元仿真和实验验证了上述电磁场耦合分析。     

Non-stationarity and cross-correlation effects in the MHD solar activity

The analysis of turbulent processes in sunspots and pores which are self-organizing long-lived magnetic structures is a complicated and not yet solved problem. The present work focuses on studying such magneto-hydrodynamic (MHD) formations on the basis of flicker-noise spectroscopy using a new method of multi-parametric analysis. The non-stationarity and cross-correlation effects taking place in solar activity dynamics are considered. The calculated maximum values of non-stationarity factor may become precursors of significant restructuring in solar magnetic activity. The introduced cross-correlation functions enable us to judge synchronization effects between the signals of various solar activity indicators registered simultaneously.     

Latitudinal distribution of solar coronal active regions

We studied the cyclic evolution of the latitudinal distribution of solar coronal active regions based on daily images from SOHO EIT for the period 1995–2017. Fully automated software was used, which included the following steps: initial preparation of images in the data series, normalization of histograms and correction of limb brightening, segmentation of images using threshold intensity values obtained from their histograms, scanning of segmented images in heliographic coordinates and obtaining profiles of latitudinal distribution of coronal active regions for each image of the data series. From the output data, we obtained a temporary change in the latitudinal distribution profiles and the migration of activity centers on the solar disk. From the period of minimum activity to the next minimum in both hemispheres, activity centers begin to migrate from high latitudes towards the equator. At the same time, the general center of activity repeatedly changes the direction of migration. The latitudinal distribution of the so-called presence factor of coronal active regions closely resembles the magnetic butterfly diagram, which proves their direct causal relationships. Variations in the presence factor of coronal active regions are correlated with cyclic variations in the sunspot daily numbers.     

失效概率矩独立全局灵敏度分析的高效算法

失效概率矩独立全局灵敏度分析对指导可靠性优化至关重要，本文从乘法降维及Edgeworth级数展开的角度提出一种失效概率矩独立全局灵敏度指标分析的高效算法。所提算法通过Edgeworth级数展开将失效概率矩独立全局灵敏度指标的求解转化为输出无条件及条件前四阶整数矩的求解。对于输出的无条件及条件四阶矩的计算，基于乘法降维的思想，本文推导了重复利用计算输出的无条件矩的输入输出样本来计算条件矩以及外层关于输入变量一维积分的计算公式，使得仅需重复利用输出无条件前四阶矩求解产生的积分网格内的数据即可同时求得输出的前四阶条件矩以及外层关于输入变量的一维积分。所提算法大大提高了失效概率矩独立全局灵敏度的分析效率。航空发动机涡轮盘以及汽车前轴的分析结果验证了所提算法的高效性及准确性。     

How do interplanetary shock impact angles control the size of the geoeffective magnetosphere?

In this paper, we investigate temporal and spatial magnetosphere response to the impact of interplanetary (IP) shocks with different inclinations and speeds on the Earth’s magnetosphere. A data set with more than 500 IP shocks is used to identify positive sudden impulse (SI⁺) events as expressed by the SuperMAG partial ring current index. The SI⁺ rise time (RT), defined as the time interval between compression onset and maximum SI⁺ signature, is obtained for each event. We use RT and a model suggested by Takeuchi et al. (2002) to calculate the geoeffective magnetospheric distance (GMD) in the shock propagation direction as a function of shock impact angle and speed for each event. GMD is a generalization of the geoeffective magnetosphere length (GML) suggested by Takeuchi et al. (2002), defined from the subsolar point along the X line toward the tail. We estimate statistical GMD and GML values which are then reported for the first time. We also show that, similarly to well-known results for RT, the highest correlation coefficient for the GMD and impact angle is found for shocks with high speeds and small impact angles, and the faster and more frontal the shock, the smaller the GMD. This result indicates that the magnetospheric response depends heavily on shock impact angle. With these results, we argue that the prediction and forecasting of space weather events, such as those caused by coronal mass ejections, will not be accurately accomplished if the disturbances’ angles of impact are not considered as an important parameter within model and observation scheme capabilities.     

L-band nighttime scintillations at the northern edge of the EIA along 95°E during the ascending half of the solar cycle 24

The characteristics of nighttime ionospheric scintillations measured at the L-band frequency of 1.575 GHz over Dibrugarh (27.5°N, 95°E, MLAT ～ 17°N, 43° dip) during the ascending half of the solar cycle 24 from 2010 to 2014 have been investigated and the results are presented in this paper. The measurement location is within or outside the zone of influence of the equatorial ionization anomaly depending on solar and geomagnetic activity. Maximum scintillation is observed in the equinoxes irrespective of solar activity with clear asymmetry between March and September. The occurrence frequency in the solstices shifts from minimum in the June solstice in low solar activity to a minimum in the December solstice in high solar activity years. A significant positive correlation of occurrence of scintillations in the June solstice with solar activity has been observed. However, earlier reports from the Indian zone (～75°E) indicate negative or no correlation of scintillation in June solstice with solar activity. Scintillations activity/occurrence in solstices indicates a clear positive correlation with Es recorded simultaneously by a collocated Ionosonde. In equinoxes, maximum scintillations occur in the pre-midnight hours while in solstices the occurrence frequency peaks just after sunset. The incidence of strong scintillations (S₄ ≥ 0.4) increases with increase in solar activity. Strong (S₄ ≥ 0.4) ionospheric scintillations accompanied by TEC depletions in the pre-midnight period is attributed to equatorial irregularities whereas the dusk period scintillations are related to the sporadic-E activity. Present results thus indicate that the current location at the northern edge of the EIA behaves as low as well as mid-latitude location.