风力机变速变桨的LQG/LTR鲁棒控制

针对变速变桨风力机实际工况下同时存在外界输入噪声及内部测量噪声的问题,采用线性二次型/回路传输恢复(Linear quadratic Gauss/loop transfer recovery,LQG/LTR)方法设计改善某风力机叶轮转速及塔架前后弯曲模态的控制器,增强风力机系统在随机干扰下的鲁棒性能。根据风力机空气动力学的圆盘理论和叶素理论,求解风力机受到的扭矩和推力。基于变速变桨风力机的线化模型,分别进行LQG和LQG/LTR控制器设计,分别仿真输出风力机的叶轮转速、塔架塔顶位移和桨距角时间变化曲线。仿真结果表明,LQG/LTR控制器在满足系统控制目标的情况下,可显著提高风力机系统的鲁棒性能及稳定性。     

基于线性模型的风电场发电量计算与分析

针对相对平坦地形,采用线性化流体方程描述流场,并根据大气边界层特性进一步简化计算方法,即利用所谓地形影响系数快速求解感兴趣点(一般为风机位置)的流动速度;针对尾流影响,采用工程上广泛使用的修正Park模型来求解,尾流线性叠加并忽略较弱的尾流影响。文中介绍了一个已建典型海滨风电场的装机规模、地表粗糙度以及测风情况,并以此风电场为算例采用不同测风数据进行发电量计算,预测结果与实际发电量较好地吻合。最后探索了算例风电场各风机发电量不均衡原因,提出地形图大小对风场模拟准确性的影响,并从工程设计角度提出具体意见。     

Modelling of Solar Wind, CME Initiation and CME Propagation

Simulations of coronal mass ejections (CMEs) evolving in the interplanetary (IP) space from the Sun up to 1 AU are performed in the framework of ideal magnetohydrodynamics (MHD) by the means of a finite-volume, explicit solver. The aim is to quantify the effect of the background solar wind and of the CME initiation parameters, such as the initial magnetic polarity, on the evolution and on the geo-effectiveness of CMEs. First, three different solar wind models are reconstructed using the same numerical grid and the same numerical scheme. Then, different CME initiation models are considered: Magnetic foot point shearing and magnetic flux emergence. For the fast CME evolution studies, a very simple CME model is considered: A high-density and high-pressure magnetized plasma blob is superposed on a background steady state solar wind model with an initial velocity and launch direction. The simulations show that the initial magnetic polarity substantially affects the IP evolution of the CMEs influencing the propagation velocity, the shape, the trajectory (and thus, the geo-effectiveness).     

Large geomagnetic storms of extreme solar event periods in solar cycle 23

During extreme solar events such as big flares or/and energetic coronal mass ejections (CMEs) high energy particles are accelerated by the shocks formed in front of fast interplanetary coronal mass ejections (ICMEs). The ICMEs (and their sheaths) also give rise to large geomagnetic storms which have significant effects on the Earth’s environment and human life. Around 14 solar cosmic ray ground level enhancement (GLE) events in solar cycle 23 we examined the cosmic ray variation, solar wind speed, ions density, interplanetary magnetic field, and geomagnetic disturbance storm time index (D_st). We found that all but one of GLEs are always followed by a geomagnetic storm with D_st  −50 nT within 1–5 days later. Most(10/14) geomagnetic storms have D_st index  −100  nT therefore generally belong to strong geomagnetic storms. This suggests that GLE event prediction of geomagnetic storms is 93% for moderate storms and 71% for large storms when geomagnetic storms preceded by GLEs. All D_st depressions are associated with cosmic ray decreases which occur nearly simultaneously with geomagnetic storms. We also investigated the interplanetary plasma features. Most geomagnetic storm correspond significant periods of southward B_z and in close to 80% of the cases that the B_z was first northward then turning southward after storm sudden commencement (SSC). Plasma flow speed, ion number density and interplanetary plasma temperature near 1 AU also have a peak at interplanetary shock arrival. Solar cause and energetic particle signatures of large geomagnetic storms and a possible prediction scheme are discussed.     

The Solar Wind and the Sun in the Past

Exposure to the solar wind can have significant long term consequences for planetary atmospheres, especially for planets such as Mars that are not protected by global magnetospheres. Estimating the effects of solar wind exposure requires knowledge of the history of the solar wind. Much of what we know about the Sun’s past behavior is based on inferences from observations of young solar-like stars. Stellar analogs of the weak solar wind cannot be detected directly, but the interaction regions between these winds and the interstellar medium have been detected and used to estimate wind properties. I here review these observations, with emphasis on what they suggest about the history of the solar wind.     

On the Radial Evolution of Alfvénic Turbulence in the Solar Wind

The observations at different solar distances and latitudes, collected in the past three decades, and the results obtained from more and more sophisticated numerical simulations allowed us to reach a good understanding on many aspects of the complex phenomenon of solar wind turbulence. Moreover, new interesting insights in the theory of turbulence have been obtained, in the past decade, from the point of view that considers a turbulent flow as a complex system, where chaotic behavior and well-established scaling laws coexist. This review aims to provide a quick overview on the state of art in this research field with particular focus on local generation mechanisms.     

Nickel Isotopic Composition and Nickel/Iron Ratio in the Solar Wind: Results from SOHO/CELIAS/MTOF

Using the Mass Time-of-Flight Spectrometer (MTOF)—part of the Charge, Elements, Isotope Analysis System (CELIAS)—onboard the Solar Heliospheric Observatory (SOHO) spacecraft, we derive the nickel isotopic composition for the isotopes with mass 58, 60 and 62 in the solar wind. In addition we measure the elemental abundance ratio of nickel to iron. We use data accumulated during ten years of SOHO operation to get sufficiently high counting statistics and compare periods of different solar wind velocities. We compare our values with the meteoritic ratios, which are believed to be a reliable reference for the solar system and also for the solar outer convective zone, since neither element is volatile and no isotopic fractionation is expected in meteorites. Meteoritic isotopic abundances agree with the terrestrial values and can thus be considered to be a reliable reference for the solar isotopic composition. The measurements show that the solar wind elemental Ni/Fe-ratio and the isotopic composition of solar wind nickel are consistent with the meteoritic values. This supports the concept that low-FIP elements are fed without relative fractionation into the solar wind. Our result also confirms the absence of substantial isotopic fractionation processes for medium and heavy ions acting in the solar wind.     

On the Differences in Composition between Solar Energetic Particles and Solar Wind

Although the average composition of solar energetic particles (SEPs) and the bulk solar wind are similar in a number of ways, there are key differences which imply that solar wind is not the principal seed population for SEPs accelerated by coronal mass ejection (CME) driven shocks. This paper reviews these composition differences and considers the composition of other possible seed populations, including coronal material, impulsive flare material, and interplanetary CME material.     

VHE Gamma-ray supernova remnants

Increasing observational evidence gathered especially in X-rays and γ-rays during the course of the last few years support the notion that Supernova remnants (SNRs) are Galactic particle accelerators up to energies close to the “knee” in the energy spectrum of Cosmic rays. This review summarises the current status of γ-ray observations of SNRs. Shell-type as well as plerionic type SNRs are addressed and prospect for observations of these two source classes with the upcoming GLAST satellite in the energy regime above 100 MeV are given.     

三维平壁进气道的特性研究

介绍三维进气道和超声速燃烧冲压式喷气发动机 (SCRAMJET)模型一项实验研究的结果。Scramjet模型由进气道和燃烧室组成 ,此模型组件的设计是为了研究流动结构以获得进气道的特性 ,以及研究燃烧室和进气道、燃料 (氢及碳氢燃料 )点火和燃烧的相互影响。这些试验是在下吹式风洞(M =2 ～ 6,Reunit=( 8～ 54) × 1 0 6)和热射式风洞 (M =6及 7 2 ,Reunit =( 1 0 ～ 32 )× 1 0 6,Tt =1 50 0 ～ 2 50 0K)中进行的。