二阶n次多项式自治系统的极限环的唯一性

主要利用文［１］中的变换，将下列二阶ｎ次多项式自治系统ｄｘｄｔ＝ｇ１（ｘ）＋ｈ１（ｘ）ｙｄｙｄｔ＝ｇ２（ｘ）＋ｈ２（ｘ）ｙ（＊）（其中，ｇ１（ｘ）＝∑ｎｉ＝０ａｉｘｉ，ｈ１（ｘ）＝∑ｎ－１ｉ＝０ｂｉｘｉ，ｇ２（ｘ）＝∑ｎｉ＝０ｃｉｘｉ，ｈ２（ｘ）＝∑ｎ－１ｉ＝０ｄｉｘｉ）变换成Ｌｉｅｎａｒｄ方程，再利用构造Ｄｕｌａｃ函数的方法和文［２］中的一个定理，得到了二阶ｎ次多项式自治系统（＊）的极限环唯一性的几个充分条件。     

Planetary Radiation Budgets

The energy state of a planet depends fundamentally on its radiation budget. Measurements made from space over past decades have led to significant revisions of ground-based estimates, both of the reflected fraction (the Bond albedo) of solar radiative flux and of the emitted thermal infrared radiation flux, for the Earth as well as for the other planets. After a brief survey of methods and difficulties in accurately determining planetary radiation budgets, we note contradictions in existing tabulations of global parameters, in particular Bond albedo. For the Earth, such contradictions are unjustified, considering that global and annual means as well as the seasonal cycle of Earth Radiation Budget components have now been determined with high accuracy. The Earth's Bond albedo is close to 0.3. Net storage of energy in the Earth-ocean system is close to zero, with a well-established annual cycle of amplitude close to ±12 Wm⁻². Some contradictions remain for the other terrestrial planets. For the giant planets, modern reduced values of the Bond albedo imply reduced but still significant internal energy generation.     

Latitude and solar-cycle dependence of radial IMF intensity

I describe a simple procedure for extrapolating the observed solar magnetic field into the heliosphere, which averages the asymptotic fields computed using the standard source surface and current sheet models. The resultant field is characterized by strong latitudinal gradients (maintained by volume currents outside the source surface) and by abrupt reversals in direction at the current sheets. The model yields good agreement with the observed long-term variation of the radial IMF component in the ecliptic, and is used to predict the variation of |B _r | along the latitudinal trajectory of Ulysses during 1990–1994. As found in earlier studies, the magnitude ofB _r at any latitude is determined largely by the strength and relative orientation of the Sun's dipole moment.     

挠性飞行器的脉冲调制控制

三轴稳定控制是大挠性飞行器有效和重要的姿态控制方式，喷嘴控制是实现三轴稳定控制的手段之一。本文针对伪速率调制器（ＰＳＲＭ）和脉冲调宽调频调制器（ＰＷＰＦＭ），采用非线性脉冲调制器线性化和描述函数两种方法来分析大挠性航天飞行器的姿态稳定性问题，并对某型卫星的远地点点火姿态控制系统进行了分析和仿真。     

Quasi-biennial oscillations in the cross-correlation of properties of macrospicules

Jets, whatever small (e.g. spicules) or large (e.g. macrospicules) their size, may play a key role in momentum and energy transport from photosphere to chromosphere and at least to the low corona. Here, we investigate the properties of abundant, large-scale dynamic jets observable in the solar atmosphere: the macrospicules (MS). These jets are observationally more distinct phenomena than their little, and perhaps more ubiquitous, cousins, the spicules. Investigation of long-term variation of the properties of macrospicules may help to a better understanding of their underlying physics of generation and role in coronal heating. Taking advantage of the high temporal and spatial resolution of the Solar Dynamics Observatory, a new dataset, with several hundreds of macrospicules, was constructed encompassing a period of observations over six years. Here, we analyse the measured properties and relations between these properties of macrospicules as function of time during the observed time interval. We found that cross-correlations of several of these macrospicule properties display a strong oscillatory pattern. Next, wavelet analysis is used to provide more detailed information about the temporal behaviour of the various properties of MS. For coronal hole macrospicules, a significant peak is found at around 2-year period. This peak also exists partially or is shifted to longer period, in the case of quiet Sun macrospicules. These observed findings may be rooted in the underlying mechanism generating the solar magnetic field, i.e. the global solar dynamo.     

一种脉宽数字快速电磁阀驱动电路的设计

采用强激颤振电流、维持颤振电流及占空比的控制方法,设计了一种驱动电路,使电磁阀在开占空比时强激吸合后迅速降低驱动电流,降低了电磁阀的发热量,提高了电磁阀的响应速度,从而达到电磁阀对燃油流量的精确控制.在脉宽数字快速电磁阀电路设计中使用了为数不多的贴片元器件,实现了电磁阀小型化和高可靠性驱动的控制.     

A fast arc fault detection method for AC solid state power controllers in MEA

Arc fault detection is desperately required in Solid State Power Controllers (SSPC) in addition to their fundamental functions because arcs will provoke growing harm and threat to aircraft safety. Experimental study has been done to obtain the faulted current data. In order to improve the detection speed and accuracy, two fast arc fault detection methods have been proposed in this paper with the analysis of only half cycle data. Both Fast Fourier Transform (FFT) and Wavelet Packets Decomposition (WPD) have been adopted to distinguish arc fault currents from normal operation currents. Analysis results show that Alternating Current (AC) arcs can be effectively and accurately detected with the proposed half cycle data based methods. Moreover, experimental verification results have also been provided.     

基于CPLD的循环冗余校验码的实现

本文介绍了利用VHDL语言，在MAXPLUSⅡ平台上，使用CPLD实现串行、并行两种信源方式的CRC码的设计及其模型验证结果。无论是串行，还是并行的信源要想实现CRC码设计必须建立校验、纠错两个模块，完成数据传输中的差错控制。同时在用硬件实现CRC码传输的过程中，比较了串、并两种方式的优缺点。     

Segmentation of extreme ultraviolet solar images via multichannel fuzzy clustering

The study of the variability of the solar corona and the monitoring of its traditional regions (Coronal Holes, Quiet Sun and Active Regions) are of great importance in astrophysics as well as in view of the Space Weather and Space Climate applications. Here we propose a multichannel unsupervised spatially constrained fuzzy clustering algorithm that automatically segments EUV solar images into Coronal Holes, Quiet Sun and Active Regions. Fuzzy logic allows to manage the various noises present in the images and the imprecision in the definition of the above regions. The process is fast and automatic. It is applied to SoHO–EIT images taken from February 1997 till May 2005, i.e. along almost a full solar cycle. Results in terms of areas and intensity estimations are consistent with previous knowledge. The method reveal the rotational and other mid-term periodicities in the extracted time series across solar cycle 23. Further, such an approach paves the way to bridging observations between spatially resolved data from imaging telescopes and time series from radiometers. Time series resulting form the segmentation of EUV coronal images can indeed provide an essential component in the process of reconstructing the solar spectrum.     

Even–odd cycle parity in complexity of hemispheric sunspot activity

We have used the Lempel–Ziv measure to describe the complexity in sunspot activity during the solar cycles 18–23. In particular, we examined the time series of daily sunspot numbers in the northern and southern hemispheres in each of the six cycles and calculated the Lempel–Ziv complexity (LZC) value for each time series. Our results indicate that in the even cycles, the LZC values of the sunspot numbers in the two hemispheres are very close to each other, whereas in the odd cycles they differ significantly between the two hemispheres. We also find that within each hemisphere the LZC varies from cycle to cycle. This even–odd cycle parity reflects the variations in inter-hemispheric strengths of the solar magnetic field leading to different temporal distributions of sunspots in the two hemispheres. The degree of complexity may influence the predictability of sunspot activity in the two hemispheres during the various cycles. Although the physical implication of the results is not clear, these results may stimulate new ideas into modeling the complex dynamics of the solar dynamo.