武器分离及舱门开启过程数值模拟研究

基于非结构重叠网格技术,发展了一套能较好模拟空腔流动和武器分离问题的数值计算方法.通过模拟典型空腔流动和WPFS模型分离轨迹,并与试验结果比较,说明本文方法可较好模拟空腔复杂流动和武器分离轨迹.采用发展的数值方法对某内埋弹舱舱门开启过程和内埋武器分离轨迹进行了数值模拟,研究了舱门运动的非定常效应对舱门气动特性的影响.研究表明:一定条件下,舱门运动产生的非定常效应对舱门气动特性影响较大,舱门和舱门控制系统设计时必须考虑;在本文给定条件下,弹舱内的内、外侧导弹均能安全分离.通过研究,为内埋弹舱的舱门设计和内埋武器分离安全评估提供了技术手段和依据.     

红外成像设备输出图像十字线毛刺或扭曲故障问题技术归零研究

针对某型直升机红外成像设备输出图像十字线毛刺或扭曲问题,在视频处理电路原理分析的基础上,结合不同技术状态的电路板对比分析试验,进行故障排查定位,揭示了故障隐含于锁相电路和电路点像素时钟被干扰的真实原因,给出了消除毛刺或扭曲的解决办法和措施。     

The Crab pulsar seen with AquEYE at Asiago Cima Ekar observatory

We are developing fast photon-counter instruments to study the rapid variability of astrophysical sources by time tagging photon arrival times with unprecedented accuracy, making use of a Rubidium clock and GPS receiver. The first realization of such optical photon-counters, dubbed AquEYE (the Asiago Quantum Eye), was mounted in 2008 at the 182 cm Copernicus Observatory in Asiago. AquEYE observed the Crab pulsar several times and collected data of extraordinary quality that allowed us to perform accurate optical timing of the Crab pulsar and to study the pulse shape stability on a timescale from days to years with an excellent definition. Our results reinforce the evidence for decadal stability of the inclination angle between the spin and magnetic axis of the Crab pulsar. Future realizations of our instrument will make use of the Galileo Global Navigation Satellite System (GNSS) time signal.     

基于三阶累积量的转子振动信号降噪方法研究

本文根据信号分离理论研究了发动机转子系统振动信号的降噪问题。当转子系统发生轻微碰摩时 ,由于振动信号中含有瞬时突变的微弱高频信息 ,这可能与高频随机噪声的频带互相叠加 ,所以利用传统的滤波方法不能有效地去噪 ,为碰摩故障诊断带来了困难。本文利用基于高阶累积量的盲信号分离方法 ,设计了相应算法 ,成功地从被噪声污染的信号中恢复源振动信号 ,从而可确保碰摩故障的检测和诊断能顺利进行     

Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.     

非结构动网格技术及其在超声速飞行器头罩分离模拟中的应用

针对激波诱导物体运动的二维动力学模型,比较了采用流动定常、结合非定常弹道方程的所谓"准定常"计算方法和非结构动网格计算方法,通过流场和运动特性分析,指出发展有相对运动的非定常流动模拟方法的重要性;另外采用修正弹簧近似和局部重构的非结构动网格技术,耦合求解Euler方程及6DOF弹道方程,数值模拟高度H=25km、飞行马赫数Ma=6.0、迎角α=0°状态下火箭抛罩的动力学过程.研究表明,稠密大气层内头罩受到的气动力比惯性力大几个数量级,导致头罩的运动特性完全由气动力控制.分离过程中,头罩和火箭头部之间的气动干扰在时间和空间上都表现出强烈的非线性特征,头罩姿态变化剧烈.本文还对分离过程中部分位置上的流场进行定常模拟,比较了定常和非定常的气动力,所得结论对于分析地面风洞可控轨迹系统(CTS)试验具有指导意义.     

Elemental Abundances of the Bulk Solar Wind: Analyses from Genesis and ACE

Analysis of the Genesis samples is underway. Preliminary elemental abundances based on Genesis sample analyses are in good agreement with in situ-measured elemental abundances made by ACE/SWICS during the Genesis collection period. Comparison of these abundances with those of earlier solar cycles indicates that the solar wind composition is relatively stable between cycles for a given type of flow. ACE/SWICS measurements for the Genesis collection period also show a continuum in compositional variation as a function of velocity for the quasi-stationary flow that defies the simple binning of samples into their sources of coronal hole (CH) and interstream (IS).     

D/H and Nearby Interstellar Cloud Structures

Analysis of UV spectra obtained with the HST, FUSE and other satellites provides a new understanding of the deuterium abundance in the local region of the galactic disk. The wide range of gas-phase D/H measurements obtained outside of the Local Bubble can now be explained as due to different amounts of deuterium depletion on carbonaceous grains. The total D/H ratio including deuterium in the gas and dust phases is at least 23 parts per million of hydrogen, which is providing a challenge to models of galactic chemical evolution. Analysis of HST and ground-based spectra of many lines of sight to stars within the Local Bubble have identified interstellar velocity components that are consistent with more than 15 velocity vectors. We have identified the structures of 15 nearby warm interstellar clouds on the basis of these velocity vectors and common temperatures and depletions. We estimate the distances and masses of these clouds and compare their locations with cold interstellar clouds.     

Fe/O Ratios in Interplanetary Shock Accelerated Particles

It is widely accepted that diffusive shock acceleration is an important process in the heliosphere, in particular in producing the energetic particles associated with interplanetary shocks driven by coronal mass ejections. In its simplest formulation shock acceleration is expected to accelerate ions with higher mass to charge ratios less efficiently than those with lower mass to charge. Thus it is anticipated that the Fe/O ratio in shock-accelerated ion populations will decrease with increasing energy above some energy. We examine the circumstances of five interplanetary shocks that have been reported to have associated populations in which Fe/O increases with increasing energy. In each event, the situation is complex, with particle contributions from other sources in addition to the shock. Furthermore, we show that the Fe/O ratio in shock-accelerated ions can decrease even when the shock is traveling through an Fe-rich ambient ion population. Thus, although shock acceleration of an Fe-rich suprathermal population has been proposed to explain large Fe-rich solar particle events, we find no support for this proposal in these observations.     

Galactic Wind: Mass Fractionation and Cosmic Ray Acceleration

The dynamical and chemical effects of the Galactic Wind are discussed. This wind is primarily driven by the pressure gradient of the Cosmic Rays. Assuming the latter to be accelerated in the Supernova Remnants of the disk which at the same time produce the Hot Interstellar Medium, it is argued that the gas removed by the wind is enriched in the nucleosynthesis products of Supernova explosions. Therefore the moderate mass loss through this wind should still be able to remove a substantial amount of metals, opening the way for stars to produce more metals than observed in the disk, by e.g. assuming a Salpeter-type stellar initial mass function beyond a few Solar masses. The wind also allows a global, physically appealing interpretation of Cosmic Ray propagation and escape from the Galaxy. In addition the spiral structure of the disk induces periodic pressure waves in the expanding wind that become a sawtooth shock wave train at large distances which can re-accelerate “knee” particles coming from the disk sources. This new Galactic Cosmic Ray component can reach energies of a few×10¹⁸ eV and may contribute to the juncture between the particles of Galactic and extragalactic origin in the observed overall Cosmic Ray spectrum.