Chaotic Temporal Variability of Magnetospheric Radio Emissions

Nonthermal magnetospheric radio emissions provide the radio signatures of solar-terrestrial connection and may be used for space weather forecasting. A three-wave model of auroral radio emissions at the fundamental plasma frequency was proposed by Chian et al. (1994) involving resonant interactions of Langmuir, whistler and Alfvén waves. Chaos can appear in the nonlinear evolution of this three-wave process in the magnetosphere. We discuss two types of intermittency in radio signals driven by temporal chaos: the type-I Pomeau-Manneville intermittency and the interior crisis-induced intermittency. Examples of time series for both types of intermittency are presented. This revised version was published online in August 2006 with corrections to the Cover Date.     

High-energy solar-particle events

Conclusion Recent high-energy solar-particle events have been illustrated and described individually. The manner in which the observations have been used to develop and test concepts of the hydromagnetic behaviour of the solar plasma in space has been outlined. Some of the events have been analyzed in more detail than hitherto. The results seem to support the concept that the magnetic field of a sunspot tends to erupt, or to balloon, into space in the form of a great tongue or sack attached to the sun near the sunspot. Supersonic shock processes also must be involved in the propagation of disturbances in planetary space, and the fluxes of galactic and of solar particles may change in the vicinity of such shocks, but alone shocks do not appear to be capable of explaining all the observed effects.     

The laminar-turbulent transition zone in the boundary layer

The flow during transition from the laminar to a turbulent state in a boundary layer is best described through the distribution of the intermittency. In constant-pressure, two-dimensional flow, turbulent spots appear to propagate linearly; the hypothesis of concentrated breakdown, together with Emmons's theory, leads to an adequate model for the intermittency distribution over flow regimes ranging all the way from low subsonic to hypersonic speeds. However, when the pressure gradient is not zero, or when the flow is not two-dimensional, spot propagation characteristics are more complicated. The resulting intermittency distributions often show peculiarities that may be best viewed as ‘subtransitions’. Previous experimental results in such situations are reviewed and recent results and models are discussed. The problem of predicting the onset of transition remains difficult, but is outside the scope of the present article.Although this paper is intended to be chiefly a survey, several new results in various stages of publication are also included.     

A New Morphology of Solar Activity and Recurrent Geomagnetic Disturbances: The Late-Declining Phase of the Sunspot Cycle

Certain aspects of the Sun and resulting geomagnetic disturbances can be studied better on the source surface, an imaginary spherical surface of 3.5 solar radii, than on the photospheric surface. This paper presents evidence that the Sun exhibits one of the most fundamental aspects of activities most clearly during the late-declining phase of the sunspot cycle. It is the period when 27-day average values of the solar wind speed and of geomagnetic disturbances tend to be highest during the sunspot cycle. Important findings of this study on the late-declining phase of the sunspot cycle are the following:

1. By introducing a new coordinate system, modifying the Carrington coordinates, it is shown that various solar activity phenomena, solar flares, the brightest coronal regions, and also the lowest solar wind speed region, tend to concentrate in two quadrants, one around 90^° in longitude in the northern hemisphere (NE) and the other around 270^° in longitude in the southern hemisphere (SW). For this reason, the new coordinate system is referred to as the NESW coordinate system.
2. It is shown that the above results are closely related to the fact that the neutral line exhibits a single wave (sinusoidal or rectangular) in both the Carrington coordinates and the NESW coordinate system during the late-declining phase. The shift of the neutral line configuration during successive solar rotations during the late-declining phase causes longitudinal scatter of the location of solar flares with respect to the neutral line in a statistical study. The NESW coordinate system is designed to suppress the shift, so that the single wave location is fixed and thus a ‘nest’ of solar flares emerges in the NE and SW quadrants.
3. It is also shown that the single wave is the source of the double peak of the solar wind speed and two series of recurrent geomagnetic disturbances in each solar rotation, making the 27-day average solar wind and geomagnetic disturbances highest during the sunspot cycle. The double peak is a basic feature during the late-declining phase, but is obscured by several complexities which we identified in this paper; see item 8.
4. The single wave of the neutral line configuration can be approximated by three dipole fields, one which can be represented by a central dipole (parallel or anti-parallel to the rotation axis) and two hypothetical dipoles on the photosphere. This configuration is referred to as the triple dipole model.
5. The location of the two hypothetical photospheric dipoles coincide with the two active regions (solar flares, the brightest coronal region) and also the lowest solar wind speed region in the NESW coordinate system; the lowest solar wind regions are the cause of the valleys of the double peak of the solar wind speed.
6. The two hypothetical dipole fields actually do exist at the location of the two active regions in a coarse magnetic map (5 × 5^°). The two dipoles follow the Hale–Nicholson polarity law. Thus, they are real physical entities.
7. The apparent meridional rotation of the dipolar field on the source surface during the sunspot cycle results from combined changes of both the central dipole field and of the two photospheric dipoles, although the central dipole remains axially parallel or anti-parallel. Thus, the Sun has a general field that can be represented by an axially aligned dipole located at the center of the Sun throughout the sunspot cycle, except for the sunspot maximum period when the polarization reversal occurs.
8. The complexity of recurrent geomagnetic disturbances can also be understood by having the NESW coordinate system for various solar phenomena and the relative location of the earth with respect to the solar equatorial plane.
9. As the intensity of the two dipoles decreases toward the end of the sunspot cycle, the amplitude of the single wave decreases, and the neutral line tends to align with the heliographic equator.
10. The neutral line shows a double wave structure during certain epochs of the sunspot cycle. In such a situation, it can be considered that two NESW coordinate systems are present in one Carrington coordinate, resulting in four active regions.
11. The so-called classical “sector boundary” arises when the peaks (top and bottom) of the single wave reached 90^° in latitude in both hemispheres.
12. In summary: A study of the late-declining period of the sunspot cycle is very important compared with the sunspot maximum period. In the late-declining period, the Sun shows its activities in the simplest form. It is suggested that some of the basic features of solar activities and recurrent geomagnetic disturbances that have been studied by many researchers in the past can be synthesized in a simplest way by introducing the NESW coordinate system and the triple dipole model. There is a possibility that the basic results we learned during the late phase of the sunspot cycle can be applicable to the rest of the sunspot cycle.

     

空间交会对接中太阳光照窗口的研究

在空间交会对接过程中，光学测量装置对目标航天器的观测将直接受太阳光照反射强度的影响，空间交会对接必须在满足太阳光照条件的前提下进行，从正常交会对接和异常交会对接两个方面，详细分析了满足目标航天器光照条件的光照弧段和光照窗口问题，并且简要地讨论了地影区对光照弧段和光照窗口的影响，最后通过一个仿真算例，具体说明了光照条件及地影区对交会对接的约束。     

Particle measurements on an ESRO satellite (Neutral-1) in a highly eccentric Polar orbit

Conclusion A satellite such as Neutral-1 should be instrumented with magnetometers, plasma detectors, and detectors of energetic particles, and flown to an altitude of some 26 R _E in a high-inclination orbit. It can thus probe regions of the magnetosphere of particular importance but as yet unexplored. It also is in an orbit that offers the optimum variety of phenomena to be explored, with the additional advantage that the characteristics of each phenomenon can be compared one with the other and the interrelation of these phenomena deduced. Such a satellite offers unique opportunities to investigate a multitude of unknown phenomena, such as the origin and energization of the particles that cause auroras and constitute Van Allen radiation. It can also potentially yield data to help solve long-lived problems, viz.: do the particles that cause auroras come from the sun, and how does a ripple in the solar corona ultimately feed energy into the magnetosphere at an average rate of 10¹⁷-10¹⁸ ergs/sec? Someone should fly such a satellite at the earliest opportunity and certainly by sunspot maximum (1969) since the existing satellite and instrumental technology is adequate.     

Evolution of the Sunspot Number and Solar Wind $$ Time Series

The past two decades have witnessed significant changes in our knowledge of long-term solar and solar wind activity. The sunspot number time series (1700-present) developed by Rudolf Wolf during the second half of the 19th century was revised and extended by the group sunspot number series (1610–1995) of Hoyt and Schatten during the 1990s. The group sunspot number is significantly lower than the Wolf series before ～1885. An effort from 2011–2015 to understand and remove differences between these two series via a series of workshops had the unintended consequence of prompting several alternative constructions of the sunspot number. Thus it has been necessary to expand and extend the sunspot number reconciliation process. On the solar wind side, after a decade of controversy, an ISSI International Team used geomagnetic and sunspot data to obtain a high-confidence time series of the solar wind magnetic field strength (\(B\)) from 1750-present that can be compared with two independent long-term (> ～600 year) series of annual \(B\)-values based on cosmogenic nuclides. In this paper, we trace the twists and turns leading to our current understanding of long-term solar and solar wind activity.     

Nanoflares and current sheet dissipation

Energy must be continually supplied to the solar corona to maintain both its average temperature and its high energy manifestations. The energy is supplied by photospheric motions and the magnetic field acts both to transmit this energy to the corona and as the furnace in which the energy is stored. The means by which the energy is dissipated and transformed into the actual forms we observe is the activation of current sheets. We conjecture here the properties of such current sheets as derived by both energetical arguments and numerical evidence of the self-organization of a system of currents in a highly turbulent medium. The consequences of the appearance of spatial and temporal intermittency on the different aspects of solar acitvity are also discussed.     

皮卫星姿态估计及粗太阳敏感器标定算法研究

粗太阳敏感器是一种由多个光电池片配置组成的模拟式太阳敏感器,它结构简单、资源要求少,在皮卫星平台应用较为广泛。光电池光伏输出特性是粗太阳敏感器测量的基础,使用余弦关系近似等效会引入很大的误差。通过实际测试和深入分析,建立了更高精度的粗太阳敏感器输出特性等效数值模型,并以此为基础,推导了卫星姿态估计及粗太阳敏感器标定的联合在轨实时算法。算法采用多级耦合结构,由1个扩展卡尔曼滤波器(EKF)和6个卡尔曼滤波器组成,同时估计卫星姿态、卫星角速度以及卫星6个面共30个标定参数。仿真表明,和常规的EKF姿态估计算法相比,联合算法的运算量只增加了一半,而估计精度却提高了一个量级。     

基于混沌变量的航空发动机模糊神经网络控制

针对模糊神经网络控制器中模糊规则的设计和神经网络权值的确定存在困难这个问题,提出了混沌优化控制方案,将混沌优化算法应用到航空发动机模糊神经网络控制中,利用混沌优化算法对模糊神经网络的参数进行优化。仿真结果表明,设计的模糊神经网络控制器具有良好的性能。      

拟合带间歇性的人工风速序列

研究生成既满足给定的工程谱特性，又具有间歇性结构的风速序列作为结构气动计算的输入。生成大气边界层紊流的人工风速序列是做结构风振计算的重要步骤，目前的方法都是生成高斯序列；实际的大气边界层紊流具有多尺度多层次的非高斯结构，集中体现在所谓“间歇性”上。利用余振苏与Leveque提出的对数泊松律模型产生各尺度的小波系数，可以在拟合目标风速谱的同时引入湍流间歇性，通过小波逆变换生成单条风速序列，再用拟合周期图的思路扩展为多重相关序列。     

基于S-A湍流模型和间歇因子输运方程的转捩流数值模拟

考虑到γ-Re_θt转捩模型中间隙因子输运方程并不依赖于具体的湍流模型,因而提出了耦合S-A湍流模型和间歇因子输运方程的转捩流模拟方法.其主要思想是构造与间歇因子相关的两个耦合函数,分别作用到S-A模型的生成项和耗散项用以控制湍流的产生与发展,从而实现层流到湍流的数值转捩.结果表明:该方法中模型方程具有完全当地性的特点,易于实施,可直接用以求解三维转捩流动.4个典型算例表明该方法模拟结果与γ-Re_θt模型准确度相当,但少求解了两个输运方程,计算耗时减少了15%.      

Thermo-mechanical design aspects for primary composite structures of large transport aircraft

Thermo-mechanical design aspects for primary carbon fibre reinforced plastics (CFRP) components, especially wings, of future large transport aircraft are discussed. Numerical simulations of the heating of a wing under intensive sun irradiation and of cooling during taxiing and take-off result in the recommendation of an appropriate design temperature. The study of flat stringer-stiffened panels reveals the influence of imperfections and boundary conditions on the buckling load under simultaneous thermal and mechanical loading.     

高超声速飞行器-进气道一体化热流数值计算

采用CFD(计算流体动力学)技术, 开展了飞行器前体/发动机一体化气动热环境分析.对层流区、转捩区和湍流区分别采用计算模型, 在湍流区利用压缩性修正的SSGZ-Jk-ε湍流模型, 在转捩区引入代数型转捩因子模型描述边界层由层流逐渐过渡为完全湍流的流动过程.计算了前体和内通道的表面热流, 并与实验结果进行了对比.结果表明所采用的计算方法可以较好地预测前体及发动机内通道热流率, 流动状态、几何结构及激波入射对热流值影响较大.      

On deterministic chaos,stationarity, periodicity and intermittency in coronal bursts and flares

Solar and stellar flares are highly structured in space and in time, as is indicated for example by their radio signatures: the narrowband spikes, type III, type II and IV, and pulsation events. Structured in time are also the not flare related type I events (noise storms). The nature of this observationally manifest fragmentation is still not clear. Either, it can be due to stochastic boundary or initial conditions of the respective processes, such as inhomogeneities in the coronal plasma. Or else, a deterministic non-linear process is able to cause complicated patterns of these kinds.We investigate the nature of the fragmentation in time. The properties of processes we enquire are stationarity, periodicity, intermittency, and, with dimension estimating methods, we try to discriminate between stochastic and low-dimensional deterministic processes. Since the measured time series are rather short, the dimension estimate methods have to be used with care: we have developed an extended dimension estimate procedure consisting of five steps. Among others, it comprises again the questions of stationarity and intermittency, but also the more technical problems of temporal correlations, judging scaling and convergence, and limited number of data points (statistical limits).We investigate 3 events of narrowband spikes, 13 type III groups, 10 type I storms, 3 type II bursts and 1 type IV event of solar origin, and 3 pulsation-like events of stellar origin. They have in common that all of them have stationary phases, periodicities are rather seldom, and intermittency is quite abundant. However, the burst types turn out to have different characteristics. None of the investigated time series reveals a low-dimensional behaviour. This implies that they originate from complex processes having dimensions (degrees of freedom) larger than about 4 to 6, which includes infinity,i. e. stochasticity. The lower limit of the degrees of freedom is inferred from numerical experiments with known chaotic systems, using time series of similar lengths, and it depends slightly on the burst types.     

Towards Synthesis of Solar Wind and Geomagnetic Scaling Exponents: A Fractional Lévy Motion Model

Mandelbrot introduced the concept of fractals to describe the non-Euclidean shape of many aspects of the natural world. In the time series context, he proposed the use of fractional Brownian motion (fBm) to model non-negligible temporal persistence, the ‘Joseph Effect’; and Lévy flights to quantify large discontinuities, the ‘Noah Effect’. In space physics, both effects are manifested in the intermittency and long-range correlation which are by now well-established features of geomagnetic indices and their solar wind drivers. In order to capture and quantify the Noah and Joseph effects in one compact model, we propose the application of the ‘bridging’ fractional Lévy motion (fLm) to space physics. We perform an initial evaluation of some previous scaling results in this paradigm, and show how fLm can model the previously observed exponents. We suggest some new directions for the future.     

用子波系数概率密度函数研究湍流多尺度结构的间歇性

用热线风速仪在充分发展平板湍流边界层中测量流向速度信号的时间序列并进行湍流多尺度结构统计特性的实验研究。用热线风速仪以高于对应最小湍流时间尺度的分辨率精细测量风洞中平板湍流边界层不同法向位置的流向速度分量的时间序列信号,用子波分析对湍流脉动速度信号进行多尺度分解,将推广的自相似性(ESS)应用于子波分析。用子波系数的概率密度函数验证了多尺度相干结构对间歇性的影响,并证明与距壁面距离有关。对比研究了提取湍流边界层多尺度相干结构前后湍流多尺度结构函数间歇性的变化规律及概率密度函数的变化规律,验证了多尺度相干结构是湍流边界层产生奇异标度律的原因。当这些相干结构被分离出后,由子波系数计算的ESS标度律就回到K olm ogorov线性标度律,这一现象在整个湍流边界层都是很明显的。      

THE SIGNAL OF THE 11-YEAR SUNSPOT CYCLE IN THE UPPER TROPOSPHERE-LOWER STRATOSPHERE

The paper summarizes work by the authors over the past ten years on an apparent signal of the 11-year sunspot cycle in the lower stratosphere-upper troposphere. The signal appears as a basic, consistent pattern in correlations between heights of stratospheric constant-pressure levels, at least as high as 25 km, and the solar cycle in which the highest correlations are in the subtropics.The variation of the stratospheric heights in phase with the sunspot cycle are – in the areas of high correlations between the two – associated with temperature variations on the same time scale in the middle and upper troposphere. The spatial distribution of the correlations suggests that the year-to-year changes in tropical and subtropical vertical motions contain a component on the time scale of the solar cycle.In January and February the correlations with the sunspot cycle are smallest. The smallness of the correlations is owing to the fact that they are different in the east and west years of the quasi-biennial oscillation in the equatorial stratospheric winds. The correlation pattern in the east years is the same as in the other seasons and is statistically significant. In the west years the correlations are insignificant outside the arctic, and the positive correlation in the arctic in these years is related to the fact that major midwinter breakdowns of the cyclonic vortex in the west years so far have happened only at maxima in the solar cycle.Until recently reliable continuous series of analyses of the stratosphere were not available for the southern hemisphere. The U.S. National Centers for Environmental Prediction and the National Center for Atmospheric Research have now, however, issued a 23-year series of re-analyzed global data which has made it possible to detect the solar signal on the southern hemisphere. It turns out to be almost the same as that on the northern hemisphere.The correlations between total column ozone and the sunspot cycle are lowest in the equatorial regions, where ozone is produced, and in the subpolar regions, where the largest amounts are found. In the annual mean the largest correlations lie between 5° lat. and 30° lat. We suggest that this distribution of correlations is due to the fact that the subtropical heights of the constant-pressure surfaces in the ozone layer are higher in maximum than in minimum years of the sunspot cycle, and that the higher subtropical heights in the solar maxima depress the poleward transport of ozone through the subtropics and thus create an abundance of ozone.