An Overview of the Fast Auroral SnapshoT (FAST) Satellite

The FAST satellite is a highly sophisticated scientific satellite designed to carry out in situ measurements of acceleration physics and related plasma processes associated with the Earth's aurora. Initiated and conceptualized by scientists at the University of California at Berkeley, this satellite is the second of NASA's Small Explorer Satellite program designed to carry out small, highly focused, scientific investigations. FAST was launched on August 21, 1996 into a high inclination (83°) elliptical orbit with apogee and perigee altitudes of 4175 km and 350 km, respectively. The spacecraft design was tailored to take high-resolution data samples (or `snapshots') only while it crosses the auroral zones, which are latitudinally narrow sectors that encircle the polar regions of the Earth. The scientific instruments include energetic electron and ion electrostatic analyzers, an energetic ion instrument that distinguishes ion mass, and vector DC and wave electric and magnetic field instruments. A state-of-the-art flight computer (or instrument data processing unit) includes programmable processors that trigger the burst data collection when interesting physical phenomena are encountered and stores these data in a 1 Gbit solid-state memory for telemetry to the Earth at later times. The spacecraft incorporates a light, efficient, and highly innovative design, which blends proven sub-system concepts with the overall scientific instrument and mission requirements. The result is a new breed of space physics mission that gathers unprecedented fields and particles observations that are continuous and uninterrupted by spin effects. In this and other ways, the FAST mission represents a dramatic advance over previous auroral satellites. This paper describes the overall FAST mission, including a discussion of the spacecraft design parameters and philosophy, the FAST orbit, instrument and data acquisition systems, and mission operations.     

SRM 纤维缠绕壳体的蒙特卡罗随机有限元分析

采用蒙特卡罗随机有限元方法，结合复合材料壳体力学、纤维缠绕理论等知识，分析了固体火箭发动机纤维缠绕壳体在燃气内压随机变化作用下的应力响应，绘出应力分布曲线，为固体火箭发动机结构可靠性评估奠定基础。     

空载固体发动机计算与试验模态相关性分析

为了预测空载状态固体火箭发动机动态特性,对其进行了模态试验,并应用MSC.Marc进行了模态计算,然后对比两者的结果,进行了相关性分析和评估。计算得到了发动机250Hz以内的一阶弯曲模态和五阶呼吸模态。试验测得了发动机的三阶呼吸模态和一阶弯曲模态。比较试验测试模态和与之对应的计算模态:固有频率相对误差均在5%以内;振型相关图上的点大都分布在斜率为1(或 1)的直线周围;MAC(模态置信判据)值在0 9左右。说明计算与试验模态有较好的相关性,有限元计算模型比较准确的反映了实际情况。     

金属水反应水冲压发动机系统性能估算

使用金属／水反应燃料是推进水下超高速航行器的最佳途径，分析了单次注水和二次注水的铝／水反应燃料水冲压发动机系统，得出了燃料质量配比、燃烧室温度、燃烧室压强、系统有效推力、效率等关键技术性能指标。指出了二次注水系统的优越性并提出了一种二次注水系统的实施方案。分析结论与实际系统性能指标相吻合，证明了分析的正确性，可以为系统研究提供参考。     

一次火箭参数对RBCC引射模态性能的影响

应用经过校验的三维湍流有限体积数值算法，对引射模态下RBCC模型不同一次引射火箭结构和工作参数条件下的多种工作状态进行了模拟。结果发现：提高一次火箭燃烧室工作压强，二次流量增加，系统推力增加，混合效果增强；一次火箭喷管形状直接影响引射掺混效果，但在保证足够一次流量的前提下，方形管道中可以使用锥形一次喷管，不会带来性能上的较大差异；一次火箭喷管数目增加，掺混质量提高；一次喷管扩张半角的改变不会影响二次引入流量，但会影响掺混效果和一次火箭自身推力；一次喷管面积膨胀比的变化，不会影响二次引入流量．但会改变混合效果。     

涡轮叶片表面气膜冷却效率的实验研究

采用放大的叶片模型，利用大尺寸低速线性叶栅风洞进行实验，测量了涡轮导向叶片表面不同位置单排气膜孔的气膜冷却效率，研究了孔排位置、吹风比及来流雷诺数的影响。风洞实验段由3个叶片组成，其中中间的叶片为试验叶片，由优质木材制成。试验叶片表面上开有15排气膜孔，其中吸力面3排，前缘区6排，压力面6排。实验的参数变化范围是：基于叶片弦长的来流雷诺数250000-450000，吹风比0．5-2．5。结果表明，由于气膜孔排位置的不同，其下游冷却效率受来流雷诺数及吹风比影响的变化趋势也有所不同。     

Langmuir Turbulence and Solar Radio Bursts

Langmuir waves and turbulence resulting from an electron beam-plasma instability play a fundamental role in the generation of solar radio bursts. We report recent theoretical advances in nonlinear dynamics of Langmuir waves. First, starting from the generalized Zakharov equations, we study the parametric excitation of solar radio bursts at the fundamental plasma frequency driven by a pair of oppositely propagating Langmuir waves with different wave amplitudes. Next, we briefly discuss the emergence of chaos in the Zakharov equations. We point out that chaos can lead to turbulence in the source regions of solar radio emissions. This revised version was published online in August 2006 with corrections to the Cover Date.     

六喷管超音速引射器性能的理论分析和实验研究

对某一定尺寸的六喷管超音速引射器进行气动性能的实验研究。结果表明：随着主次流压比Ｐ＊ｐ／Ｐ＊ｓ增加，引射系数及修正引射系数下降；当引射系数增加时，混合管动量修正系数Ｋｍ下降，但主喷管流量系数μ变化不大。对上述工况进行理论计算的结果与实验数据符合良好。     

Steady magnetospheric convection: A review of recent results

Theoretical pressure balance arguments have implied that steady convection is hardly possible in the terrestrial magnetotail and that steady energy input necessarily generates a cyclic loading-unloading sequence, i.e., repetitive substorms. However, observations have revealed that enhanced solar wind energy input to the magnetospheric system may either lead to substorm activity or enhanced but steady convection. This topic is reviewed with emphasis on several recent case studies of the Steady Magnetospheric Convection (SMC) events. In these cases extensive data sets from both satellite and ground-based instruments from various magnetospheric and ionospheric regions were available.Accurate distinction of the spatial and temporal scales of the magnetospheric processes is vital for correct interpretation of the observations during SMC periods. We show that on the large scale, the magnetospheric configuration and plasma convection are stable during SMC events, but that both reveal considerable differences from their quiet-time assemblies. On a shorter time scale, there are numerous transient activations which are similar to those found during substorms, but which presumably originate from a more distant tail reconnection process, and map to the poleward boundary of the auroral oval. The available observations and the unresolved questions are summarized here.The tail magnetic field during SMC events resembles both substorm growth and recovery phases in the neartail and midtail, respectively, but this configuration may remain stable for up to ten hours. Based on observations and model results we discuss how the magnetospheric system avoids pressure balance problems when the plasma convects earthward.Finally, the importance of further coordinated studies of SMC events is emphasized. Such studies may shed more light on the substorm dynamics and help to verify quantitatively the theoretical models of the convecting magnetosphere.     

Radial and meridional trends in solar wind thermal electron temperature and anisotropy: Ulysses

Ulysses plasma measurement from 1.15 to 5.31 AU and from S6.4° to S48.3° solar latitude are used to assess the trends in the solar wind thermal electron temperature and anisotropy. Improved spacecraft potential corrections and data products have been incorporated. The radial temperature gradient is steeper than in previous determinations, but flatter than adiabatic. When normalized to 1 AU, temperature decrease with increasing latitude. Little change in the average thermal anisotropy has been seen during the mission.