End-to-End Modeling of the Solar Terrestrial System

Traditionally modeling for space science has concentrated on developing simulations for individual components of the solar terrestrial system. In reality these regions are coupled together. This coupling can be as simple as the driving of the magnetosphere – ionosphere – thermosphere system by the solar wind or as a complicated as the feedback of the ionospheric conductivity and currents on the magnetosphere. As part of the CISM project we are beginning a concentrated effort to compressively model the entire system. This approach includes chains of models. In the first chain physics based numerical models are utilized while in the second chain empirical models are coupled together. The first half of this paper discusses the numerical modeling approach by highlighting the coupling of pairs of regions within the system. In the second section we present results from empirical models which are combined to make long term forecasts of conditions in the geospace environment. It is expected that a validated and reliable forecast model for space weather can be obtained by combining the strongest elements of each chain.     

Grid-Adaptive Computations of Magnetized Jets

We present grid-adaptive numerical simulations of magnetized plasma jets, modeled by means of the compressible magnetohydrodynamic equations. The Adaptive Mesh Refinement strategy makes it possible to investigate long-term jet dynamics where both large-scale and small-scale effects are at play. We extend recent findings for uniformly magnetized, periodic shear layers to planar and fully 3D extended jet segments. The jet lengths cover multiple, typically 10, axial wavelengths of the fastest growing Kelvin–Helmholtz (KH) like modes. The dominant linear MHD instabilities of the jet flows are quantified by means of MHD spectroscopic analysis. In cases characterized by sonic Mach numbers about unity and large plasma beta values, both single and double shear layers (planar jets) manifest self-organizing trends to large scales, e.g. by continuous pairing/merging between co-rotating vortices, simultaneously with the introduction of small-scale features by magnetic reconnection events. The vortices form as a result of KH unstable shear-flow layers, and their coalescence arises from the growth of subharmonic modes at multiple wavelengths of the fastest growing KH instability. In extended two-dimensional jet segments, we investigate how varying jet width alters this coalescence process occurring at both edges, e.g. by introducing Batchelor-like coupling between counter-rotating vortices formed at opposing weakly magnetized, close shear layers. Finally, periodic segments of supersonic magnetized jets are simulated in two- and three-dimensional cases, which are characterized by violent shock-dominated transients.     

A Class of TVD Type Combined Numerical Scheme for MHD Equations With a Survey About Numerical Methods in Solar Wind Simulations

It has been believed that three-dimensional, numerical, magnetohydrodynamic (MHD) modelling must play a crucial role in a seamless forecasting system. This system refers to space weather originating on the sun; propagation of disturbances through the solar wind and interplanetary magnetic field (IMF), and thence, transmission into the magnetosphere, ionosphere, and thermosphere. This role comes as no surprise to numerical modelers that participate in the numerical modelling of atmospheric environments as well as the meteorological conditions at Earth. Space scientists have paid great attention to operational numerical space weather prediction models. To this purpose practical progress has been made in the past years. Here first is reviewed the progress of the numerical methods in solar wind modelling. Then, based on our discussion, a new numerical scheme of total variation diminishing (TVD) type for magnetohydrodynamic equations in spherical coordinates is proposed by taking into account convergence, stability and resolution. This new MHD model is established by solving the fluid equations of MHD system with a modified Lax-Friedrichs scheme and the magnetic induction equations with MacCormack II scheme for the purpose of developing a combined scheme of quick convergence as well as of TVD property. To verify the validation of the scheme, the propagation of one-dimensional MHD fast and slow shock problem is discussed with the numerical results conforming to the existing results obtained by the piece-wise parabolic method (PPM). Finally, some conclusions are made. This revised version was published online in August 2006 with corrections to the Cover Date.     

低马赫数流动数值模拟方法的研究

在文献[1，2]提出的一种低马赫数流动数值模拟新方法的基础上，本文作者进一步优化了算法，确定了该方法适用的马赫数范围，讨论了参数σ对计算的影响。大量的定常／非定常、低雷诺数流动的计算结果表明这种方法具有计算精度高、收敛速度快以及计算花销小的特点。     

CAM后置处理研究

分析了数控加工后置处理技术的特征、面临的问题和当前的发展趋势,介绍了应用通用后置处理器开发定制专用后置处理器的实践。     

一种求解核函数方程的新方法—辅助核法

本文提出了求解核函数方程的辅助核法。此法克服了偶极子栅格法对网格分布的限制,具有更大的适用范围。数值计算表明,此法对求解绕翼型的跨声速激波流动是很有利的。     

微型脉冲推力器点火启动过程计算与点火药量选择

建立了微型脉冲推力器点火启动模型,模型中考虑了两相流动和颗粒对推进剂表面的冲击传热。根据数值计算结果,给出了不同产物颗粒含量下的点火药量选择参考范围。该参考范围对于产物颗粒含量小于50%的点火药是适用的;由于过多的颗粒含量将对装药表面产生强烈的热力冲蚀破坏作用,产物颗粒含量超过50%的点火药不适合微型火箭发动机。     

驻涡燃烧室前钝体燃料喷射性能数值分析

为研究驻涡燃烧室在前钝体燃料喷射状况下的燃烧性能,采用3维数值仿真模拟方法,对驻涡燃烧室前钝体燃料喷射 状况下的燃烧效率及燃烧室性能与无前钝体燃料喷射状况下的燃烧性能进行了对比分析,并对驻涡燃烧室的冷流以及燃烧状态 下的燃烧室性能进行了系统研究。燃烧室温度分布表明：前钝体顶部燃料喷射在0.2~0.7的喷射系数范围内,缩短了燃烧室火焰 长度,提高了燃烧室在相同轴向长度下的燃烧效率,使燃烧室更加紧凑;驻涡燃烧室前钝体顶部燃料喷射孔的孔径在一定范围内 的变化对燃烧室的燃烧效率、出口温度分布系数以及总压损失影响较小。     

三维弹塑性接触问题的边界元法

将边界元法发展用于解决三维弹塑性接触问题,推导了无摩擦的三维弹塑性接触问题的积分方程,讨论了其数值解技术。数值结果与有限无法的数值结果对比表明,所发展的方法是成功的。