Magnetospheric Models and Trajectory Computations

The calculation of particle trajectories in the Earth's magnetic field has been a subject of interest since the time of Störmer. The fundamental problem is that the trajectory-tracing process involves using mathematical equations that have `no solution in closed form'. This difficulty has forced researchers to use the `brute force' technique of numerical integration of many individual trajectories to ascertain the behavior of trajectory families or groups. As the power of computers has improved over the decades, the numerical integration procedure has grown more tractable and while the problem is still formidable, thousands of trajectories can be computed without the expenditure of excessive resources. As particle trajectories are computed and the characteristics analyzed we can determine the cutoff rigidity of a specific location and viewing direction and direction and deduce the direction in space of various cosmic ray anisotropies. Unfortunately, cutoff rigidities are not simple parameters due to the chaotic behavior of the cosmic-ray trajectories in the cosmic ray penumbral region. As the computational problem becomes more manageable, there is still the issue of the accuracy of the magnetic field models. Over the decades, magnetic field models of increasing complexity have been developed and utilized. The accuracy of trajectory calculations employing contemporary magnetic field models is sufficient that cosmic ray experiments can be designed on the basis of trajectory calculations. However, the Earth's magnetosphere is dynamic and the most widely used magnetospheric models currently available are static. This means that the greatest uncertainly in the application of charged particle trajectories occurs at low energies.     

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.      

Can Surface Flux Transport Account for the Weak Polar Field in Cycle 23?

To reproduce the weak magnetic field on the polar caps of the Sun observed during the declining phase of cycle 23 poses a challenge to surface flux transport models since this cycle has not been particularly weak. We use a well-calibrated model to evaluate the parameter changes required to obtain simulated polar fields and open flux that are consistent with the observations. We find that the low polar field of cycle 23 could be reproduced by an increase of the meridional flow by 55% in the last cycle. Alternatively, a decrease of the mean tilt angle of sunspot groups by 28% would also lead to a similarly low polar field, but cause a delay of the polar field reversals by 1.5 years in comparison to the observations.     

An overview of infrared thermography techniques used in large wind tunnels

Infrared thermography (IRT) is used at Onera in large facilities for boundary layer visualization and for heat flux assessment. Modern IR cameras and insulating paints enable efficient visualization of the laminar/turbulent transition region. This technique is now applied in large transonic test facilities. Heat flux assessment is one of the main purposes of hypersonic tests. It is done mainly with IRT and dedicated softwares, while sensors as thermocouples are used to check the reliability of IRT. A 1D data reduction method has been developed to provide the heat flux through temperature measurements. It takes into account thickness and curvature effects. The method has been recently improved to be used with steel models covered with an insulating paint, which provides a high emissivity. The temperature film is converted into a heat flux film, which is be used to extract the useful information. This requires image processing tools that relate every pixel to a point on the model. A new application of IRT is going on in the Onera's high enthalpy hypersonic wind tunnel F4. The camera is used in single-line scan mode because of the short duration of the run. The main difficulty comes from the flow, which is not transparent. The first trial to cope with this kind of optical pollution is encouraging.     

Solar Variability of Possible Relevance for Planetary Climates

The global variability of the Sun of relevance for planetary climates has been directly measured for the past few decades. For longer stretches of time models are required. Semi-empirical models can now accurately reproduce the measured records of solar total and spectral irradiance, as well as of the magnetic flux. They can also provide reconstructions of these quantities on longer time scales. Here a summary is given of some of the modelling efforts and of the results achieved so far.     

Signature of the 11-Year Cycle in the Upper Atmosphere

In the last 45 years I have studied the thermal structure of the atmosphere from the thermosphere down to the stratosphere, and found evidence of its variability in relationship with the change of solar irradiation during the 11-year solar cycle. I would review, in the light of recent model results, the measurements which I had made since the 1960s and which, for some of them, did not find any explanation at the time of their publication. The data were obtained by two different techniques, rockets and lidars and correspond to different regions of the atmosphere from the upper thermosphere to the stratosphere. The expectation was until recently that the atmosphere should be warmed by an increase of solar flux in the course of the solar cycle due to the increase of UV flux. It has been shown to be the case in the tropical stratosphere and at all latitudes in the upper thermosphere. But, at high and mid latitudes and at other altitudes, the reverse situation was found to exist and, until recently, this cooling observed in parts of the atmosphere with increasing solar flux had never been simulated by models. In addition to reviewing our own data, the paper will present recent results using other dataset which support our observations. It is only recently that we succeeded with a model able to tune the forcing by planetary waves at the tropopause level and thus reproduce such behaviour.     

Deconvolution of Energetic Neutral Atom Images of the Earth's Magnetosphere

A method for deconvolving equatorial pitch angle distributions of energetic neutral atoms from images from the ENA instruments on the IMAGE satellite is described and illustrated using simulated data obtained from calculated models of ring current flux. The unknown flux is expanded in terms of cubic B-splines and Legendre polynomials. The expansion coefficients are obtained from the solution of a linear set of equations that select the smoothest solution that fits the data. In this way, all the information that is contained in the data is extracted but no more.     

永磁同步电机有限控制集模型预测转矩控制系统研究

建立了基于定子磁链xy坐标系的永磁同步电机(PMSM)有限控制集模型预测转矩控制(FCSMPTC)系统,仿真验证了系统的有效性和可行性。针对磁链和转矩预测模型较为复杂的问题,提出了磁链和转矩的简化预测模型。理论分析、仿真和试验结果验证了FCSMPTC的简化模型与常规模型控制效果相当,可明显减小计算负担,提高系统实时性能。将电压矢量幅值和角度作为FCSMPTC的控制变量,设计了变幅值变角度的备选电压矢量集合。仿真结果表明该备选电压矢量集合可有效减小稳态转矩脉动,但动态性能不及传统备选电压矢量集合。基于不同备选电压矢量的特点,提出了根据系统状态自适应动态变化的备选电压矢量策略。仿真结果表明,该控制策略在静动态下均可取得良好的控制性能。     

Algebraic turbulent energy flux models for hypersonic shear flows

Algebraic truncation models were derived for the turbulent energy flux for high-speed shear flows with and without thermal and mechanical non-equilibrium effects. To facilitate closure, fluctuating dilatation moments were modeled via conservation of mass truncations and the inhomogeneous terms were neglected. The resulting energy flux model provided significant improvements, up to 20%, in the temperature predictions over the gradient diffusion model for equilibrium flows over a Mach number range of 0.02–11.8. Our experiments showed that vibrational relaxation significantly altered the basic decay rate of grid turbulence. Also, our models indicated that compressibility introduces an explicit pressure gradient dependency. Analyses of a governing parameter indicated that these terms are negligibly small for low speeds, but may be important, or even dominant, for high-speed flows.     

模型燃烧室紊流燃烧的大涡模拟

采用了两种不同的亚网格尺度燃烧模型对带 V型稳定器的模型燃烧室紊流化学反应流动进行了大涡模拟 ,用 k-ε方程亚网格尺度模型确定亚网格紊流粘性 ,为了考虑热辐射对燃烧室壁温和气流温度的影响 ,运用热流法辐射模型估算热辐射通量 ,用 SIMPLE算法和混合差分求解大涡模拟各守恒方程 ,通过对两种不同亚网格尺度燃烧模型数值模拟结果与实验值的比较表明 ,两种燃烧模型都与实验值较吻合 ,但 G方程小火焰模型要比亚网格 EBU燃烧模型符合得更好些      

高超声速气动热辨识技术实验研究

为估计高超声速飞行中的气动热流,采用热流辨识技术研究了平板表面的气动热流。首先采用仿真数据对辨识方法进行验证,结果表明,在测量噪声较低时热流辨识结果误差较小。此后,开展了平板的高超声速气动热风洞实验,通过内埋热电偶测量平板内部温度,采用热流辨识法获得平板表面的气动热流,采用辅助测点对比验证了内埋测点辨识结果的可信度。最后将辨识结果与平板边界层热流理论估算结果进行对比,分析了两者产生误差的原因。本文的研究为热流辨识技术的实际应用奠定了基础。     

粗糙壁热交换实验研究

 本文介绍了来流马赫数5的条件下,典型球锥模型的粗糙壁热交换实验结果。模型头部半径R为27.4毫米,底部直径D为60毫米,对五个不同粗糙度的模型进行了实验。模型表面粗糙颗粒直径d分别为0、0.3、0.5、0.7、0.9毫米。风洞前室总压P_t为10～45公斤/厘米。,相应的来流雷诺数R_eD为（O.8～3.6）×10⁶。 实验结果表明:光滑壁模型表面是层流加热,驻点热流与层流理论计算值较一致。粗糙度的影响,在低总压条件下（10公斤/厘米）主要在于促使边界层的转捩和发展。随着风洞总压的提高,物面静压和局部雷诺数的相应增大,粗糙度对热流的影响才明显增强,而严重的区域在端头。在实验最大粗糙度和最大总压条件下（d=O.9毫米、p_t=45公斤/厘米。）,除驻点值外,热流与光滑壁层流驻点值相比(q_i/q_so)的峰值在音点区域且接近4,而在驻点,此模型有别于其它模型,较为特殊,比热流最大值接近6,看来这可能与驻点局部外形变化有关。     

Reassessment of the wall functions approach for RANS computations

To assert the validity of the wall law approach in a RANS code, the results obtained with this approach are compared with those obtained from computations with fine meshes for which the turbulence models, including wall damping functions, are integrated down to the wall. It is shown that a very simple representation of the velocity profile in the wall region gives good results for transonic flows over airfoils with shock wave/boundary layer interaction leading to separation. Moreover, it is also shown that the heat flux can be correctly predicted in separated regions. The case of the infinite swept wing near separation is also considered and gives excellent results.Four popular turbulence models, k–ε, k–ω, k–l and Spalart Allmaras, have been used for the study, but the approach can be extended to other models.     

An Introduction to Theory and Models of CMEs, Shocks, and Solar Energetic Particles

We present a brief introduction to the essential physics of coronal mass ejections as well as a review of theory and models of CME initiation, solar energetic particle (SEP) acceleration, and shock propagation. A brief review of the history of CME models demonstrates steady progress toward an understanding of CME initiation, but it is clear that the question of what initiates CMEs has still not been solved. For illustration, we focus on the flux cancellation model and the breakout model. We contrast the similarities and differences between these models, and we examine how their essential features compare with observations. We review the generation of shocks by CMEs. We also outline the theoretical ideas behind the origin of a gradual SEP event at the evolving CME-driven coronal/interplanetary shock and the origin of “impulsive” SEP events at flare sites of magnetic reconnection below CMEs. We argue that future developments in models require focused study of “campaign events” to best utilize the wealth of available CME and SEP observations.     

基于不同定子槽模型的分段磁路分析

结合等效磁场实现转子内磁场强度至转子轭表面的转换,分别建立了开口、半开(闭)口定子槽模型,采用分段磁路法分析各段磁路长度变化情况,给出了不同定子槽模型下齿槽转矩的解析式。分析定子冲片选用不同牌号的硅钢片材料对齿槽转矩的影响。经研究表明:分段磁路法能够提高槽间磁路近似精度,且经分析优选的定子硅钢片材料可较为有效地削弱齿槽转矩。     

Cosmic ray Implications for Human Health

There appears to be concern among some people about the possible effects of cosmic radiation on everyday life. The amount of cosmic radiation that reaches the Earth and its environment is a function of solar cycle, altitude and latitude. The possible effect of naturally occurring cosmic radiation on airplane crews and space flight personal is a subject of current study. This paper discusses the variables controlling the cosmic ray flux in the atmosphere and describes models and software that have been developed that provide quantitative information about the cosmic radiation exposure at flight altitudes. The discussion is extended to include the cosmic radiation exposure to manned spacecraft. This revised version was published online in August 2006 with corrections to the Cover Date.     

The Solar Dynamo

It is generally accepted that the strong toroidal magnetic fields that emerge through the solar surface in sunspots and active regions are formed by the action of differential rotation on a poloidal field, and then stored in or near the tachocline at the base of the Sun’s convection zone. The problem is how to explain the generation of a reversed poloidal field from this toroidal flux—a process that can be parametrised in terms of an α-effect related to some form of turbulent helicity. Here we first outline the principal patterns that have to be explained: the 11-year activity cycle, the 22-year magnetic cycle and the longer term modulation of cyclic activity, associated with grand maxima and minima. Then we summarise what has been learnt from helioseismology about the Sun’s internal structure and rotation that may be relevant to our subject. The ingredients of mean-field dynamo models are differential rotation, meridional circulation, turbulent diffusion, flux pumping and the α-effect: in various combinations they can reproduce the principal features that are observed. To proceed further, it is necessary to rely on large-scale computation and we summarise the current state of play.