Energy release in stellar magnetospheres

The interaction of a stellar magnetosphere with a thin accretion disk is considered. Specifically, I consider a model in which (1) the accretion disk is magnetically linked to the star over a large range of radii and (2) the magnetic diffusivity of the disk is sufficiently small that there is little slippage of field lines within the disk on the rotation time scale. In this case the magnetic energy built up as a result of differential rotation between the star and the disk is released in quasi-periodic reconnection events occuring in the magnetosphere (Aly and Kuijpers 1990). The radial transport of magnetic flux in such an accretion disk is considered. It is show that the magnetic flux distribution is stationary on the accretion time scale, provided the time average of the radial component of the field just above the disk vanishes. A simple model of the time-dependent structure of the magnetosphere is presented. It is shown that energy release in the magnetosphere must take place for (differential) rotation angles less than about 3 radians. The magnetic flux distribution in the disk depends on the precise value of the rotation angle.     

对偶网络拓扑法在场问题计算中的应用

网络拓扑法已被实践证明为一种有效实用的数值计算方法。它以数学分析简单、物理概念明确、单元剖分灵活、适用性强等优点,已被越来越多的场计算专家所采用,成为一种较优秀的数值分析方法。本文在普通网络拓扑法的基础上,以温度场计算为例,通过建立其能量泛函并求其极值,导出一种高精度的网络拓扑法——对偶网络拓扑法。在给定的求解精度条件下,由于两组网络计算时产生误差之间的补偿作用,使用该方法能有效地减少计算存贮空间、缩短计算用时。这对用微机求解复杂场问题是很有意义的。本文最后的实例虽然是针对温度场分析的,但对其他场问题完全适用,故具有普遍性。     

四种风洞收缩段流场特性对比

基于西北工业大学高亚声速平面叶栅风洞,测量了维氏收缩段的出口流场,发现其方向场品质较差,相比速度场和总压场,核心区沿周向减小了15%。对四种收缩段进行数值模拟后,对比了收缩段的出口核心区、均匀性及分离特性,发现维氏曲线在前部收缩,进口收缩过急引起旋涡,但出口稳流段较长,因此出口均匀性更好。双三次曲线在后部收缩,主流区顺压梯度更大,因此附面层更薄,气流偏角更小,分离特性更好,但出口过冲更大。现有维氏收缩段的三维结构在拓宽核心区同时对气流扰动较大,恶化速度场与方向场,气流偏角增加最大达43%。进口管径对双三次收缩段的流场特性影响不大。     

基于IDDES方法和γ-Re_θ转捩模型的粗糙颗粒诱导高速边界层强制转捩模拟

采用γ-Re_θ转捩模型与IDDES (Improved Delayed Detached Eddy Simulation)相结合的方法对BAM6QT (Boeing/AFOSR Mach-6 Quiet Tunnel)中的马赫6来流条件下粗糙颗粒诱导转捩情况进行了数值模拟研究,通过与试验测量的压力脉动均方根值、脉动主频和边界层内的皮托压分布的定量对比及与文献中DNS (Direct Numerical Simulation)流场结构的定性对比,表明该方法可以捕捉粗糙单元诱导出的流向涡,能够模拟颗粒前缘分离激波和弓形激波之间的震荡现象,能够模拟流向涡向下游的发展失稳过程及其脉动发展过程。计算结果表明流向涡结构在粗糙颗粒下游40倍颗粒直径位置开始破碎,非定常扰动能也在该点附近增长达到最大值。粗糙单元诱导出了明显的条带涡结构,其中低速条带处于边界层上层,在向下游发展的过程中逐渐扩散至边界层外缘并耗散掉。高速条带位于边界层底部,在向下游发展的同时往展向两侧拓展,最终展向上多条高速条带接触并互相耦合,导致最后条带涡结构的破碎和尾迹区边界层的转捩。     

地磁导航技术研究进展

地磁场是地球的固有资源,利用地磁场匹配进行导航是一种新型导航技术.与传统的惯性导航和卫星导航比较,地磁导航具有无积累误差、抗干扰、隐蔽性好、导航信息丰富等优势.文章介绍了地磁导航的3个基本要素,即磁场测量技术、地磁模型以及定位与导航技术.分析了弱磁场磁力仪在地磁导航中的应用及其优缺点,讨论了地磁场模型和地磁匹配算法,展望了地磁导航技术的应用前景.     

基于未加权区域采样的直线反走样算法

直线作为组成图形的基本元素,其生成方法一直是计算机图形学研究的基础内容之一.针对非垂直且非水平直线在光栅图形显示器存在的走样现象,结合经典的Bresenham算法和未加权区域采样思想,提出一种新的反走样直线生成算法.相比于传统的未加权区域采样以及Wu算法,该算法主要利用整数加减运算完成直线的反走样,计算简单,利于FPGA(Field Programmable Gate Array)硬件实现.仿真结果表明:新算法的仿真速度约为传统未加权区域采样的3倍,与Wu算法仿真速度相当;利用Wu算法生成的直线平滑性较好,但是沿着直线方向的某些相邻像素灰度值相差较大,而新算法生成的直线不但平滑效果好,而且沿直线方向相邻像素灰度值相差不大,因此,相比于Wu算法,新算法反走样效果更佳.     

载人航天器密封舱内生物剂量三维仿真技术

对载人航天器密封舱内航天员遭受的生物剂量进行研究分析,可为乘员辐射防护设计和工程实施提供依据。文章将基于一维深度-剂量计算、结合扇区射线法的三维辐射仿真技术运用于载人航天器总体设计中,以某中期驻留载人航天器为例,构建生物剂量仿真分析模型。计算实例分析表明,三维剂量仿真结果可有效指导乘员辐射防护优化设计,对后续长期载人飞行中的航天员辐射安全设计具有较强的实用性。     

超音速喷管收缩扩张段匹配问题研究

超音速喷管由收缩和扩张两段组成,是高速风洞中获得超音速流动的重要部件。对于超音速喷管收缩段设计方法的研究较多,但尚未见到喷管收缩段的几种设计型面曲线如何与扩张段合理匹配问题的研究。针对以上的问题,利用CFD数值模拟方法对几种收缩曲线与扩张段匹配问题进行了计算。通过对计算结果进行对比分析,发现不同收缩曲线对超音速喷管内流有一定的影响,分析了流场特征,展示了马赫数在喷管内部的分布。     

Using GPS-TEC data to calibrate VTEC computed with the IRI model over Nigeria

This paper presents the development of a Total Electron Content (TEC) map for the Nigerian ionosphere. In this work, TEC measurements obtained from the AFRL-SCINDA GPS (Air Force Research Laboratory-Scintillation Network Decision Aid, Global Positioning System) equipment installed at Nsukka (6.87°N, 7.38°E) are used to adapt the International Reference Ionosphere (IRI) model for the Nigerian Ionosphere. The map is being developed as a computer program (implemented in the MATLAB programming language) that shows spatial and temporal representations of TEC for the Nigerian ionosphere. The method is aimed at showing how the IRI model can be used to estimate VTEC over wide areas by incorporating GPS measurements. This method is validated by using GPS VTEC data collected from a station in Ilorin (8.50°N, 4.55°E).     

Heavy ion contributions to organ dose equivalent for the 1977 galactic cosmic ray spectrum

Estimates of organ dose equivalents for the skin, eye lens, blood forming organs, central nervous system, and heart of female astronauts from exposures to the 1977 solar minimum galactic cosmic radiation spectrum for various shielding geometries involving simple spheres and locations within the Space Transportation System (space shuttle) and the International Space Station (ISS) are made using the HZETRN 2010 space radiation transport code. The dose equivalent contributions are broken down by charge groups in order to better understand the sources of the exposures to these organs. For thin shields, contributions from ions heavier than alpha particles comprise at least half of the organ dose equivalent. For thick shields, such as the ISS locations, heavy ions contribute less than 30% and in some cases less than 10% of the organ dose equivalent. Secondary neutron production contributions in thick shields also tend to be as large, or larger, than the heavy ion contributions to the organ dose equivalents.