Alfvén waves as a driving mechanism in stellar winds

Alfvén waves have been invoked as an important mechanism of particle acceleration in stellar winds of cool stars. After their identification in the solar wind they started to be studied in winds of stars located in different regions of the HR diagram. We discuss here some characteristics of these waves and we present a direct application in the acceleration of late-type stellar winds.     

O5+ in High Speed Solar Wind Streams: SWICS/Ulysses Results

Recent observations with UVCS on SOHO of high outflow velocities of O⁵⁺ at low coronal heights have spurred much discussion about the dynamics of solar wind acceleration. On the other hand, O⁶⁺ is the most abundant oxygen charge state in the solar wind, but is not observed by UVCS or by SUMER because this helium-like ion has no emission lines falling in the wave lengths observable by these instruments. Therefore, there is considerable interest in observing O⁵⁺ in situ in order to understand the relative importance of O⁵⁺ with respect to the much more abundant O⁶⁺. High speed streams are the prime candidates for the search for O⁵⁺ because all elements exhibit lower freezing-in temperatures in high speed streams than in the slow solar wind. The Ulysses spacecraft was exposed to long time periods of high speed streams during its passage over the polar regions of the Sun. The Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses is capable of resolving this rare oxygen charge state. We present the first measurement of O⁵⁺ in the solar wind and compare these data with those of the more abundant oxygen species O⁶⁺ and O⁷⁺. We find that our observations of the oxygen charge states can be fitted with a single coronal electron temperature in the range of 1.0 to 1.2 MK assuming collisional ionization/recombination equilibrium with an ambient Maxwellian electron gas. This revised version was published online in June 2006 with corrections to the Cover Date.     

Modeling PSBL high speed ion beams observed by Cluster and Double Star

On October 8, 2004, the Cluster and Double Star spacecraft crossed the near-Earth (12–19 R_E) magnetotail neutral sheet during the recovery phase of a small, isolated substorm. Although they were separated in distance by ∼7 R_E and in time by ∼30 min, both Cluster and Double Star observed steady, but highly structured Earthward moving >1000 km/s high speed H⁺ beams in the PSBL. This paper utilizes a global magnetohydrodynamic (MHD) simulation driven by Wind spacecraft solar wind input to model the large-scale structure of the PSBL and large-scale kinetic (LSK) particle tracing calculations to investigate the similarities and differences in the properties of the observed beams. This study finds that the large-scale shape of the PSBL is determined by the MHD configuration. On smaller scales, the LSK calculations, in good qualitative agreement with both Cluster and Double Star observations, demonstrated that the PSBL is highly structured in both time and space, on time intervals of less than 2 min, and spatial distances of the order of 0.2–0.5 R_E. This picture of the PSBL is different from the ordered and structured region previously reported in observations.     

涡扇发动机装机状态自然低温试验

为完成涡扇发动机状态鉴定，在北方场站开展了发动机装机状态下的自然环境低温试验。通过地面试验完成了自然低 温试验环境的量化分析，研究了不同气源起动模式、不同使用方法对装机状态自然低温条件下发动机起动性能的影响，分析了发 动机样本量对试验鉴定结果的影响。结果表明：APU供气是低温冷浸透起动的首选起动方式；冷运转可以有效改善发动机低温起 动性能，使相对起动时间缩短0.125～0.250；增加发动机样本量可以获得更加科学的鉴定结果，在低温起动过程中，发动机可能出 现失速等不稳定现象，甚至造成起动失败。开展了飞行试验，研究了空中低温环境对发动机工作参数及加减速特性的影响。结果 表明：在相同高度和速度下发动机加速时间随进气温度的降低而延长，当空中进气温度相差约30 ℃时，加速时间延长最多约为 18%；减速时间随进气温度的变化不大。     

Furthering our understanding of electrostatic solitary waves through Cluster multispacecraft observations and theory

Nonlinear isolated electrostatic solitary waves (ESWs) are observed routinely at many of Earth’s major boundaries by the Wideband Data (WBD) plasma wave receivers that are mounted on the four Cluster satellites. The current study discusses two aspects of ESWs: their characteristics in the magnetosheath, and their propagation in the magnetosheath and in the auroral acceleration (upward current) region. The characteristics (amplitude and time duration) of ESWs detected in the magnetosheath are presented for one case in which special mutual impedance tests were conducted allowing for the determination of the density and temperature of the hot and cold electrons. These electron parameters, together with those from the ion experiment, were used as inputs to an electron acoustic soliton model as a consideration for the generation of the observed ESWs. The results from this model showed that negative potential ESWs of a few Debye lengths (10–50 m) could be generated in this plasma. Other models of ESW generation are discussed, including beam instabilities and spontaneous generation out of turbulence. The results of two types of ESW propagation (in situ and remote sensing) studies are also presented. The first involves the propagation of bipolar type ESWs from one Cluster spacecraft to another in the magnetosheath, thus obtaining the velocity and size of the solitary structures. The structures were found to be very flat, with large scale perpendicular to the magnetic field (>40 km) and small scale parallel to the field (<1 km). These results were then discussed in terms of various models which predict such flat structures to be generated. The second type of propagation study uses striated Auroral Kilometric Radiation (SAKR) bursts, observed on multiple Cluster satellites, as tracers of ion solitary waves in the upward current region. The results of all studies discussed here (pulse characteristics and ESW velocity, lifetime, and size) are compared to in situ measurements previously made on one spacecraft and to theoretical predictions for these quantities, where available. The primary conclusion drawn from the propagation studies is that the multiple spacecraft technique allows us to better assess the stability (lifetime) of ESWs, which can be as large as a few seconds, than can be achieved with single satellites.     

运输类飞机典型货舱地板下部结构冲击吸能特性

为了研究运输类飞机货舱地板下部结构在冲击载荷作用下的吸能特性，选取三框两段典型货舱地板下部结构试验件开展落重冲击试验，即质量为478.5 kg的落重以3.95 m/s的速度垂直冲击倒置并固定在测力平台上的试验件，分析试验件失效模式及动态响应，同时建立有限元模型进行仿真与试验结果相关性分析及吸能特性研究。结果显示，在此种工况的冲击载荷作用下，中间支撑件发生由32框面向34框面方向的弯曲，并带动机身框发生同向弯曲和扭转，从而导致C型支撑件发生与中间支撑件相反方向的弯曲变形，并最终在机身框与C型支撑件的连接处形成两处塑性铰；紧固件失效以位于中间支撑件附近区域的长桁和剪切角片连接处的22个扁圆头铆钉发生剪切失效为主；试验初始加速度峰值和初始撞击力峰值分别为25.1g和173 kN。仿真与试验获得的结构变形模式吻合较好，仿真获得的最大压缩量与试验结果24.3 mm相差3.7%，仿真获得的压板上初始加速度峰值与试验结果25.1g相差4%。通过仿真分析发现机身框和中间支撑件是主要的吸能部件，吸能贡献分别占总吸能的32.1%和30.4%。     

高过载条件下固体火箭发动机绝热层失效研究

根据化学反应／两相流耦合,建立了铝粒子燃烧模型,通过化学反应速率模型的模化湍流燃烧,对含铝推进剂固体火箭发动机在高过载条件下的内流场进行数值研究。结果表明,过载条件下燃烧室局部异常铝滴积聚及剧烈的化学放热反应是导致绝热层异常烧蚀的主要原因。     

引力场中运动物体加速度的各向异性

在引力或任何其它力的作用下 ,运动物体的加速度是各向异性的。即在同样大小力的作用下 ,力与速度方向垂直时的加速度要大于力与速度方向一致时的加速度。将这种横向额外加速度理论应用在天体力学方面 ,正确地计算了行星近日点的“多余”进动角和光线在经过太阳表面时由引力引起的偏转角。并且定性地解释了最近发现的所谓航天器的“奇异”加速度。因此 ,行星、航天器和光子等等完全不同的物体在引力场中的运动轨道可以用完全相同的物理机制——“加速度各向异性”理论扩展了的牛顿理论加以描述。     

基于修改加速控制规律的航空发动机寿命延长控制

针对发动机加速过程,以涡轮导向叶片热机械疲劳寿命为例,通过在原加速控制规律后半段增加转子加速度限制,综合考虑加速性能与寿命延长指标,利用遗传算法对加速规律进行优化.仿真结果表明修改后的加速控制规律能够明显地延长涡轮导向叶片的寿命,而发动机加速过程上升时间基本保持不变.      

只测视线角速度的目标可观性判据

在二维平面内,把已有的只测视线角的目标可观判据扩展到只测视线角速度的情况.针对N阶机动目标,在直角坐标系中,通过分析导弹与目标相对运动方程,给出了只有视线角速度量测值情况下目标不可观的充分必要条件(目标不可观判据).目标不可观判据分为两种简单的表达形式:一种是对弹目相对距离的约束;另一种是对视线角的约束.在修正极坐标系中,通过分析系统的Fisher信息阵,得到了在只有视线角速度量测值情况下常加速度目标可观的充分必要条件.结果表明:目标不可观判据与在修正极坐标系中得到的充分必要条件是一致的,与只测视线角的目标可观判据不冲突;推理简单,不要求分析可观性矩阵和非线性微分方程,因此简单易用.