可调桨距冲压空气涡轮气动特性实验与数值分析

冲压空气涡轮风洞实验主要目的是采用相似准则,模拟空中加油工作状态,测量涡轮输出功率,分析涡轮气动特性。实验分别使用励磁发电机和加油泵作为测功器,通过调桨变距并测量最大输出功率。气动特性实验表明在风洞气流速度比加油机最小飞行速度低16%的条件下,冲压涡轮输出功率即可满足加油需要。论文还采用高数值稳定性代数Baldwin-Lomax湍流模型模拟冲压涡轮全三维混合型流场,分析流场主要气动特性,讨论桨叶表面载荷的分布。数值模拟结果显示在冲压空气涡轮桨叶近轮毂区域需要进一步优化。      

On the Coronal Magnetic Field Configuration and Solar Flare/CME Process

The coronal magnetic field configuration is important for understanding the energy storage and release processes that account for flares and/or CMEs. Here we present a model which is based on the work for potential magnetic field problems that only applies the condition at infinity with the boundary condition on the solar surface specified. We also discuss some recent progress on general force-free field models. For some event analyses, we have employed MDI/SOHO longitudinal magnetogram insected into the synoptic magnetogram to obtain whole boundary condition over the solar surface. Globally, the extrapolated global magnetic field structures effectively demonstrate the case for the disk signature of the radio CMEs and the evolution of the radio sources during the CME/flare processes.     

典型城市街道内汽车排放污染物扩散规律的模拟研究

采用自主开发的街道峡谷内污染物扩散模式,对城市中几种典型的街道峡谷内流场和污染物的浓度场进行了模拟研究。模拟结果表明:在一定气象条件下,街道中机动车排放污染物的扩散受街道宽高比、街道两侧建筑物对称性、街道两侧建筑物高度分布及街道两侧的建筑物形状等因素的影响;街道峡谷宽高比接近1时、递升型峡谷以及宽阔街道有利于污染物的扩散。     

端弯叶片通道出口二次流的研究

实验并且采用考虑粘性的涡传输方程计算端弯压气机叶片通道出口二次流。给出了３种端弯叶片及对应的原始直叶片通道出口气流偏转角的实验值和计算预测值。研究表明：采用上述方程能比较准确地预测出口气流偏转角；叶片后缘减弯可减小流向二次涡强度。     

Mathematical modeling of plasma drifts over equatorial low latitude regions

This paper presents a mathematical model to simulate ionospheric plasma drifts at equatorial low latitude regions by coupling of E- and F-regions. The governing non-linear differential equations (of elliptic and parabolic nature) are solved numerically through finite-difference schemes and obtained neutral winds and electric fields. The temperature and electron density profiles are generated utilizing MSIS-86 atmospheric model. The continuity equation is employed to obtain night-time E-region density profile using measured ionograms at Trivandrum (India). The computed vertical and zonal plasma drifts are comparable with measured Jacamarca plasma drifts with little variations during noon and evening times. The plasma drifts at Trivandrum (8.5° N, 76.5° E, dip 0.5° N) are compared with those of Jicamarca (12° S, 76.9° W, dip 2° N). Neutral wind simulations of present model agree well with those of horizontal wind model (HWM-93). The post-sunset enhancement and its reversal are also discussed.     

左、右手媒质间电磁传输特性的对比分析

文章通过重新表述折射率，对比分析了左、右手媒质不同组合情况下，电磁波在媒质界面上的折射特性。通过引入色散关系的时域有限差分法对无限大左手介质板以及线源置于左手媒质覆层内两种模型进行了模拟，模拟结果与分析相符合。分析表明，负折射现象出现在界面两侧媒质类型（LHM／RHM或RHM／LHM）不同的情况下。对于同种类型媒质的情况，左手媒质并不能引起反常的折射现象。LHM引起的反常现象通过与RHM的对比才能得以有效考察。     

A heuristic derivation of an improved analytical theory for perpendicular diffusion of charged particles

A heuristic derivation of an improved nonlinear guiding center theory for perpendicular diffusion of charged particles is presented. This new derivation complements previous work which is based on an indirect solution of the Fokker–Planck equation. The new derivation confirms the improved theory for diffusion of charged particles and makes the validity of the theory plausible.     

Viewing radiation signatures of solar energetic particles in interplanetary space

A current serious limitation on the studies of solar energetic particle (SEP) events is that their properties in the inner heliosphere are studied only through in situ spacecraft observations. Our understanding of spatial distributions and temporal variations of SEP events has come through statistical studies of many such events over several solar cycles. In contrast, flare SEPs in the solar corona can be imaged through their radiative and collisional interactions with solar fields and particles. We suggest that the heliospheric SEPs may also interact with heliospheric particles and fields to produce signatures which can be remotely observed and imaged. A challenge with any such candidate signature is to separate it from that of flare SEPs. The optimum case for imaging high-energy (E > 100 MeV) heliospheric protons may be the emission of π⁰-decay γ-rays following proton collisions with solar wind (SW) ions. In the case of E > 1 MeV electrons, gyrosynchrotron radio emission may be the most readily detectible remote signal. In both cases we may already have observed one or two such events. Another radiative signature from nonthermal particles may be resonant transition radiation, which has likely already been observed from solar flare electrons. We discuss energetic neutrons as another possible remote signature, but we rule out γ-ray line and 0.511 MeV positron annihilation emission as observable signatures of heliospheric energetic ions. We are already acquiring global signatures of large inner-heliospheric SW density features and of heliosheath interactions between the SW and interstellar neutral ions. By finding an appropriate observable signature of remote heliospheric SEPs, we could supplement the in situ observations with global maps of energetic SEP events to provide a comprehensive view of SEP events.     

扇面波导中馈电探针输入电阻数值计算

推导出扇面波导中激励探针的等效输入电阻表达式，探针是伸入波导中的同轴线的内导体，在Ｘ波段，计算了输入电阻值随着探针伸入波导中不同长度的变化。     

Physical processes in the strong magnetic fields of accreting neutron stars

The key radiative processes are discussed, numerical methods of magnetized radiative transfer are presented, and these are considered in their application to X-ray pulsar models.