稀土对电沉积镍基复合镀层高温抗氧化性的影响

研究了稀土加入三种电沉积镍基复合镀层Ni—B_4C、Ni—TiC、Ni—ZrO_2前后,在850℃时的氧化行为。通过金相观察、ESCA(光电子能谱)分析及X射线衍射等方法研究表明:镀层中不同的复合颗粒和稀土两者对镀层的抗氧化能力均有影响。其小不同种类的颗粒对镀层抗氧化能力所产生影响的差别很明显;而稀土对镀层抗氧化能力影响的差别较小,且影响的程度比较接近。另外,两者影响的机理也不同。颗粒是通过分解、扩散等过程改变表面膜的组成来影响的,而稀土则是从提高膜的致密度和膜与基体的粘附性来影响的。作者认为,它们的影响既互相独立,而又互相补充。     

粒子流量可调的喷管烧蚀试验方法

发展了一种保持燃气参数不变的情况下能实现粒子流量可调的喷管烧蚀试验方法,并研制了试验装置。该试验方法是将两相流燃气中的一部分粒子收集起来,以减少流经喷管的粒子流量,通过改变收集孔和收敛角的大小来调节粒子流量。采用该方法开展了变粒子流量的喷管烧蚀试验,试验结果验证了该方法是有效的,试验条件下喷管喉部平均线烧蚀率随粒子流量减小而降低。     

Cluster observations showing the indication of the formation of a modified-two-stream instability in the geomagnetic tail

This study presents several observations of the Cluster spacecraft on September 24, 2003 around 15:10 UT, which show necessary prerequisites and consequences for the formation of the so-called modified-two-stream instability (MTSI). Theoretical studies suggest that the plasma is MTSI unstable if (1) a relative drift of electrons and ions is present, which exceeds the Alfvèn speed, and (2) this relative drift or current is in the cross-field direction. As consequences of the formation of a MTSI one expects to observe (1) a field-aligned electron beam, (2) heating of the plasma, and (3) an enhancement in the B-wave spectrum at frequencies in the range of the lower-hybrid-frequency (LHF). In this study we use prime parameter data of the CIS and PEACE instruments onboard the Cluster spacecraft to verify the drift velocities of ions and electrons, FGM data to calculate the expected LHF and Alfvèn velocity, and the direction of the current. The B-wave spectrum is recorded by the STAFF instrument of Cluster. Finally, a field aligned beam of electrons is observed by 3D measurements of the IES instrument of the RAPID unit. Observations are verified using a theoretical model showing the build-up of a MTSI under the given circumstances.     

The hydroxyl radical as an indicator of SEP fluxes in the high-latitude terrestrial atmosphere

The low background values at nighttime of the mesospheric hydroxyl (OH) radical make it easier to single out the atmospheric response to the external solar forcing in Polar Regions. Because of the short lifetime of HO_x, it is possible to follow the trails of Solar Energetic Particle (SEP) events in the terrestrial atmosphere, as shown by Storini and Damiani (2008). The sensitivity of this indicator makes discernible not only extreme particle events with a flux peak of several thousand pfu [1 pfu = 1 particle/(cm² s sr)] at energies >10 MeV, but also those with lower flux up to about 300 pfu. Using data from the Microwave Limb Sounder (MLS) on board the EOS AURA satellite, we examined the correlation of OH abundance vs. solar proton flux for almost all the identified SEP events spanning from November 2004 to December 2006 (later on no more SEP events occurred during Solar Cycle no. 23). The channels at energies greater than 5 MeV and 10 MeV showed the best correlation values (r ∼ 0.90–0.95) at altitudes around 65–75 km whereas, as expected, the most energetic channels were most highly correlated at lower altitudes. Therefore, it is reasonably possible to estimate the solar proton flux from values of mesospheric OH (and viceversa) and it could be useful in studying periods with gaps in the records of solar particles.     

固体火箭喷管排气中的粒子分布

1.前言 现代的固体火箭发动机为提高推进剂的能量特性及抑制不稳定燃烧，常常在推进剂中添加金属粉末，最常见的是加金属铝粉。在发动机工作时，铝粉燃烧形成凝聚相的氧化铝粒子。这些粒子在喷管中的流动过程中，温度、速度等方面的变化滞后于燃·气本身的变     

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.     

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.     

小型回流燃烧室多工况碳黑分布预测

为了研究小型回流燃烧室不同条件下的工作状态,并分析其产生积碳现象的原因,采用k-ε湍流模型、EDC湍流燃烧等模型对该燃烧室多个工况进行数值计算。结果表明,燃烧室性能参数计算值与台架数据较吻合,各个状态下参数相对误差均小于1.37%。根据各工况的温度分布的变化,发现燃烧室火焰随工况降低逐渐向火焰筒头部收缩。计算了各工况蒸发管内的燃油蒸发率,发现蒸发率在低工况时明显降低。根据出口温度分布情况,计算出口温度分布系数OTDF为0.35。分析碳黑粒子的分布,发现积碳现象主要在火焰筒头部,其原因主要是燃烧不充分和冷却气膜的缺失。     

超声速PIV示踪粒子布撒技术研究

介绍了上海交通大学高超声速创新技术研究实验室为发展超声速PIV流场测试系统而开发的示踪粒子布撒技术。研究中设计了一套超声速风洞PIV示踪粒子布撒装置,提出了利用发生器罐体内的真空度吸入示踪粒子的加注方式,选定了测试流程时序并得到了较好的粒子布撒效果。通过比较不同的发生器罐注入压力对粒子布撒浓度的影响,得到了效果良好的测试方案。     

高能合成煤油GN-1性能研究 --“液体火箭推进”专刊

结合火箭发动机工程应用环境,研究了GN-1煤油高温高压热物性、安全特性、传热结焦性能以及点火延迟性能,并和现役火箭煤油作了对比分析。采用商业仪器对GN-1煤油在最高200℃、最高压力25MPa范围内的密度、黏度、定压比热容、导热系数、表面张力进行了实验测量。在实验数据的基础上,依据基团贡献法、基于比容平移法则的P-R方程、摩擦理论、广义对应态原理分别对GN-1煤油在最高350℃、最高压力60MPa范围内的密度、黏度、定压比热容、导热系数、表面张力进行了理论计算,建立了GN-1煤油的密度方程、黏度方程、导热系数方程,并将方程的计算值与实验值进行了对比,计算偏差较小。对GN-1煤油和火箭煤油的安全性能进行对比研究,GN-1煤油的闪点为40℃,自燃温度为305℃,高于火箭煤油(225℃);燃点为47℃,低于火箭煤油(82℃),GN-1煤油的爆炸极限范围为0.44%-2.9%（40℃）。GN-1煤油和火箭煤油的急性经口毒性LD50＞5000mg/kg,均属于第五级化合物（实际无毒）。在入口压力10 MPa,流速10 m·s-1,内壁温480℃条件下,GN-1煤油的传热系数比火箭煤油提高14.4%,建立了传热准则方程。GN-1煤油出口油温220℃时试验段平均结焦速率是出口油温150℃时的4.43倍,GN-1煤油不锈钢材质管路中试验段平均结焦为高合管材质管路中的22.3%。在970K-1105K温度范围内,GN-1煤油的点火延迟时间为320μs-471μs,是火箭煤油的55.6%-69.3%。相关研究可对发动机可靠设计及应用提供重要参考。