平板式预膜喷嘴初次雾化特性试验

为深入了解平板式预膜喷嘴初次雾化特性,试验研究不同进口条件对平板式预膜喷嘴初次雾化特性的影响规律。试验采用了背光照明和片状激光照明相结合的高频拍摄手段分别获得液膜俯视和侧视破碎形态,同时运用本征正交分解(POD)法和液膜边缘定位等分析方法进行光学图像结果后处理,获得表征平板式预膜喷嘴初次雾化特性三个物理量:液膜波动频率、破碎距离和横向不稳定波长。试验结果表明:①通过分析侧视和俯视破碎形态,平板式预膜喷嘴液膜破碎形态可分为三类:末端破碎、波浪脱落和表面剥离,进口韦伯数对预膜喷嘴破碎形态的影响占主导地位;②把POD法和液膜边缘定位方法等相结合方法应用到高频非接触光学喷嘴雾化图像的后处理分析中,是一种非常有效的数据后处理方法;③液膜初次雾化特性主要受到进口韦伯数和气液动量比的影响,破碎距离和横向不稳定波长都随进口韦伯数的增加而降低,液膜表面不稳定波动频率随进口韦伯数的增加而增加,所获得的经验关系式与试验数据吻合较好。所获得的进口参数对液膜破碎形态和雾化特性的影响规律为喷嘴后续优化设计提供了依据。     

某型装备轴承件无失效时的可靠性参数估计

针对寿命服从威布尔分布的某型装备轴承件在无失效数据时的可靠性参数估计问题,首先,以失效概率为待估参数,取其先验分布为Beta分布,在2个超参数的先验密度函数为2种不同情形下,建立了失效概率的2种EBayes估计模型,分析了稳健性、渐近性和单调性;然后,对威布尔分布参数进行了加权最小二乘估计,进而建立了可靠度的2种E-Bayes估计模型,分析了稳健性和单调性;最后,结合实例数据进行了可靠性参数估计与分析,指出第2种估计模型更加合理有效。     

汽车双横臂独立悬架参数优化与仿真研究

针对国内某轿车双横臂独立悬架系统，运用ADMAS／View模块建立了双横臂式悬架模型，利用ADMAS／Insight模块对建立的双横臂式独立悬架进行了优化分析。优化结果分析表明：通过悬架参数优化设计，使前悬架性能有了较大的提高。     

基于ATML标准的ATS软件建模技术

论述了国外ATML标准体系结构和构成ATML标准所有子模型的描述方法,提出了在现有ATS软件平台基础上,实现兼容ATML标准所需的建模流程设计、模型识别及模型运行流程设计等技术途径,为实现ATS软件平台的通用性、开放性及武器装备各种维护级别的测试资源的共享奠定了技术基础。     

CLVD 法制备C/C复合材料工艺探索研究

研究了采用化学液气相沉积法制备C／C复合材料的工艺过程，分析了不同预制件、温度、浸泡时间等工艺参数对致密速度、效果的影响，并总结出了一套快速高效的致密方法。     

Halo White Dwarfs and Baryonic Dark Matter

We describe the formation of hot intergalactic gas along with baryonic remnants in galaxy halos. In this scenario, the mass and metallicity of the hot intracluster and intragroup gas relates directly to the production of baryonic remnants during the collapse of galactic halos. We construct a schematic but self-consistent model in which early bursts of star formation lead to a large remnant population in the halo, and to the outflow of stellar ejecta into the halo and ultimately the Local Group. We consider local as well as high redshift constraints on this scenario. This study suggests that the microlensing objects in the Galactic halo may predominantly be 0.5M white dwarfs, assuming that the initial mass function for early star formation favored the formation of intermediate mass stars with m 1M. However, the bulk of the baryonic dark matter in this scenario is associated with the ejecta of the white dwarf progenitors, and resides in the hot intergalactic medium.     

运动基航天飞行模拟器信号缩比策略

对于大幅值的输入信号,三阶多项式缩比法易产生信号畸变且参数配置复杂;而Hermite缩比函数法的触发速度较慢.提出两种改进的缩比方法:基于三阶多项式缩比法的最优参数配置法和加入线性缩比的非线性缩比法.前一种方法通过参数的优化配置最大化稳定区,以防止信号的畸变;后一种方法则利用线性缩比的特性将缩比度限制在稳定区内.仿真结果表明:线性缩比的加入可以防止三阶多项式缩比法信号的畸变;最优配置参数法应用方便且整体效果较好.为航天飞行模拟提供了更有效的缩比策略.     

Antideuteron based dark matter search with GAPS: Current progress and future prospects

The General Antiparticle Spectrometer (GAPS) is a new approach to the indirect detection of dark matter. It relies on searching for primary antideuterons produced in the annihilation of dark matter in the galactic halo. Low energy antideuterons produced through Standard Model processes, such as collisions of cosmic-rays with interstellar baryons, are greatly suppressed compared to primary antideuterons. Thus a low energy antideuteron search provides a clean signature of dark matter. In GAPS antiparticles are slowed down and captured in target atoms. The resultant exotic atom deexcites with the emission of X-rays and annihilation pions, protons and other particles. A tracking geometry allows for the detection of the X-rays and particles, providing a unique signature to identify the mass of the antiparticle. A prototype detector was successfully tested at the KEK accelerator in 2005, and a prototype GAPS balloon flight is scheduled for 2011. This will be followed by a full scale experiment on a long duration balloon from Antarctica in 2014. We discuss the status and future plans for GAPS.     

Current status and future plans for the general antiparticle spectrometer (GAPS)

We discuss current progress and future plans for the general antiparticle spectrometer experiment (GAPS). GAPS detects antideuterons through the X-rays and pions emitted during the deexcitation of exotic atoms formed when the antideuterons are slowed down and stopped in targets. GAPS provides an exceptionally sensitive means to detect cosmic-ray antideuterons. Cosmic-ray antideuterons can provide indirect evidence for the existence of dark matter in such form as neutralinos or Kaluza–Klein particles. We describe results of accelerator testing of GAPS prototypes, tentative design concepts for a flight GAPS detector, and near-term plans for flying a GAPS prototype on a balloon.     

Mathematical description of the NaK model for MASTER-2005

The release of NaK droplets has been modeled for the new version of the European Meteoroid and Space Debris Terrestrial Environment Reference model MASTER-2005. Previously published versions of the model have been revised. The parameters of the model are introduced and discussed. NaK droplets consist of eutectic sodium–potassium alloy and have been released during RORSAT reactor core ejections. They contributed to the space debris environment in the centimeter and millimeter size regime. Sixteen nuclear powered RORSATs launched between 1980 and 1988 activated a reactor core ejection system in Sufficiently High Orbits (SHO), mostly between 900 and 950 km altitude. The core ejection caused an opening of the primary coolant circuit. The liquid coolant has been released into space during these core ejections. The outflow is considered as a discrete event for each of the sixteen core ejections in total. The NaK coolant has been forming droplets up to a diameter of 5.5 cm. NaK releases are restricted to a very narrow region near 65° inclination. This paper gives the parameters of the NaK release model as it is implemented in MASTER-2005. The quantitative values of all model parameters including characteristic diameter and uniformity parameter are presented. The ratio of the characteristic droplet size to the orifice diameter is discussed. It is estimated that altogether 128 kg of NaK-78 (8 kg per RORSAT) was released on orbit. Simulation runs show that there are still 45,000 droplets with a total mass of 97 kg in orbit at the reference epoch 1 May 2005, whereas the smallest droplet has a diameter of 5 mm. Results of orbit propagation simulation runs are presented in terms of spatial density.