Influence of the Interplanetary Magnetic Field on the Solar Wind Flow about Planetary Obstacles

The main effects caused by the interplanetary magnetic field (IMF) are analyzed in cases of supersonic solar wind flow around magnetized planets (like Earth) and nonmagnetized (like Venus) planets. The IMF has a relatively weak strength in the solar wind but it is enhanced considerably in the so-called plasma depletion layer or magnetic barrier in the vicinity of the streamlined obstacle (magnetopause of a magnetized planet, or ionopause of a nonmagnetized planet). For magnetized planets, the magnetic barrier is a source of free magnetic energy for magnetic reconnection in cases of large magnetic shear at the magnetopause. For nonmagnetized planets, mass loading of the ionospheric particles is very important. The new created ions are accelerated by the electric field related to the IMF, and thus they gain energy from the solar wind plasma. These ions form the boundary layer within the magnetic barrier. This mass loading process affects considerably the profiles of the magnetic field and plasma parameters in the flow region.     

Comparison of magnetic flux tube and cosmic string behavior in Kerr metric

Cosmic strings are topological defects which were generated at a transition phase of the very early Universe and are probably responsible for large-scale structure forming. However, they may pull through all history and exist in the recent epoch. Thus, they can have influence for the recent Universe interacting with different objects. We consider the cosmic string behavior in the vicinity of a spinning black hole by means of a numerical simulation. Here we present preliminary results of this work via a comparison of cosmic string and magnetic flux tube behavior in the Kerr metric. Such an approach follows from the similarity of the equations which describe these objects. Therefore, many aspects of this behavior may be comparable.     

Challenges in X-ray binary timing: current and future

Millisecond X-ray time variability studies of accreting low-magnetic-field neutron stars and stellar-mass black holes in X-ray binaries probe the motion of matter in regions of strong gravity. In these regions, general relativity (GR) is no longer a small correction to the classical laws of motion, but instead dominates the dynamics: we are studying motion in strongly curved spacetime. Such millisecond X-ray variability studies can therefore provide unique tests of GR in the strong-field regime. The same studies also constrain neutron-star parameters such as stellar mass and radius, and thereby the equation of state (EOS) of ultradense matter. I briefly review the status, and discuss the prospects for mapping out space-time near accreting stellar-mass compact objects, and measuring the EOS of dense matter, through millisecond timing, particularly with an eye towards future missions. The overwhelming consideration for timing sensitivity is collecting area: contrary to most applications, the signal-to-noise ratio for the aperiodic timing phenomena produced by accretion flows increases proportionally with count rate rather than as the square root of it. A 10 times larger instrument turns 1σ effects into 10σ effects (or does as well in 1% of the time). With the Rossi X-ray Timing Explorer (RXTE), using 0.6 m² collecting area, we have found several timing diagnostics from the accretion flow in the strong field region around neutron stars and black holes, as well as signals from neutron star surface hot spots. Combined work between RXTE and the new sensitive X-ray spectrographs onboard Chandra and XMM can already begin to clinch the geometry and physical mechanisms underlying these signals. Future instruments, larger in area by an order of magnitude and in some cases with enhanced spectral capabilities, are expected to turn these diagnostics of GR into true tests of GR. They are also expected to put strong constraints on neutron-star structure, and thereby on the EOS of supranuclear density matter.     

Turbulent boundary layer separation control using plasma actuator at Reynolds number 2000000

An experimental investigation was conducted to evaluate the effect of symmetrical plasma actuators on turbulent boundary layer separation control at high Reynolds number. Compared with the traditional control method of plasma actuator, the whole test model was made of aluminum and acted as a covered electrode of the symmetrical plasma actuator. The experimental study of plasma actuators' effect on surrounding air, a canonical zero-pressure gradient turbulent boundary, was carried out using particle image velocimetry(PIV) and laser Doppler velocimetry(LDV) in the 0.75 m × 0.75 m low speed wind tunnel to reveal the symmetrical plasma actuator characterization in an external flow. A half model of wing-body configuration was experimentally investigated in the  3.2 m low speed wind tunnel with a six-component strain gauge balance and PIV. The results show that the turbulent boundary layer separation of wing can be obviously suppressed and the maximum lift coefficient is improved at high Reynolds number with the symmetrical plasma actuator. It turns out that the maximum lift coefficient increased by approximately 8.98% and the stall angle of attack was delayed by approximately 2° at Reynolds number2 ×10~6. The effective mechanism for the turbulent separation control by the symmetrical plasma actuators is to induce the vortex near the wing surface which could create the relatively largescale disturbance and promote momentum mixing between low speed flow and main flow regions.     

Aerodynamic performance enhancement of a flying wing using nanosecond pulsed DBD plasma actuator

Experimental investigation of aerodynamic control on a 35 swept flying wing by means of nanosecond dielectric barrier discharge(NS-DBD) plasma was carried out at subsonic flow speed of 20–40 m/s, corresponding to Reynolds number of 3.1 · 105–6.2 · 105. In control condition, the plasma actuator was installed symmetrically on the leading edge of the wing. Lift coefficient, drag coefficient, lift-to-drag ratio and pitching moment coefficient were tested with and without control for a range of angles of attack. The tested results indicate that an increase of 14.5% in maximum lift coefficient, a decrease of 34.2% in drag coefficient, an increase of 22.4% in maximum lift-to-drag ratio and an increase of 2 at stall angle of attack could be achieved compared with the baseline case. The effects of pulsed frequency, amplitude and chord Reynolds number were also investigated.And the results revealed that control efficiency demonstrated strong dependence on pulsed frequency. Moreover, the results of pitching moment coefficient indicated that the breakdown of leading edge vortices could be delayed by plasma actuator at low pulsed frequencies.     

热障涂层界面脱粘缺陷的脉冲红外热成像检测

针对热障涂层界面脱粘缺陷的无损检测问题,首先制备了一种导热过程更加接近真实缺陷,且尺寸可控的人工模拟脱粘缺陷试样;在此基础上,采用脉冲红外热成像检测技术对人工脱粘缺陷进行检测,分析了涂层界面脱粘区和非脱粘区的表面温度瞬态响应过程;以图像标准差（SD）和归一化对比度（NC）作为评价标准,定量对比了脉冲相位法、主成分分析和表面热信号重构3种典型的热图重构方法在脱粘缺陷识别中的作用。结果表明,对400 μm厚的YSZ热障涂层,原始热图中可识别最小直径为4 mm的脱粘缺陷,而3种重构热图中均可识别最小直径为2 mm的界面脱粘缺陷,3种重构算法均显著提高了界面脱粘缺陷的识别能力,其中以表面热信号重构算法对图像的噪声抑制能力最强。     

小型回流燃烧室燃烧特性数值研究

某科研样机采用蒸发管回流燃烧室,其燃烧室结构复杂,燃烧机理和气流流动情况尚不清楚。在实验过程中发现,蒸发管及附近的火焰筒壁面上出现了较严重的积碳现象,影响燃烧室的性能。为了探究该型燃烧室的工作过程、分析积碳现象的原因,采用k-ε湍流模型、旋涡耗散概念燃烧模型(EDC)以及颗粒随机轨道模型对该燃烧室工作流场进行流固热耦合数值计算。结果表明,燃烧室性能参数计算值与台架试车数据较吻合,各项参数相对误差均小于1.7%。计算得到了燃烧室工作时流动和燃烧情况,同时分析出了各气孔流动情况及发挥的作用,并得出了产生积碳现象的原因,为该型燃烧室优化设计提供依据。     

C/SiC复合材料在高能HAN发动机上应用研究

针对高能硝酸羟胺(HAN)发动机特点,联合国防科技大学与贵研铂业股份有限公司研发了新型C/SiC复合材料身部,并进行地面试验。试验结果表明,C/SiC复合材料身部结构完好,表面HfO_2基环障涂层较完整,未出现显著开裂、剥落,涂层效果明显,保证了HAN单元发动机工作寿命。本研究为C/SiC身部在HAN单元发动机上工程化应用提供参考。     

炭／陶复合材料电热性能的研究

通过在陶瓷基体原料(高岭土)中添加炭系导电原料(石墨、炭黑),经球磨混合、模压成形和烧结工艺制得炭/陶复合材料.采用X射线衍射(XRD)、扫描电镜(SEM)、数字测温仪等分析和测试了所研制试样的相组成、显微结构以及电热性能.结果表明,本实验的烧结条件下,炭系导电原料不会和陶瓷基体发生反应,其导电性不会受到影响.单一石墨和炭黑含量超过30和25wt%或石墨加炭黑混合(m石墨: m炭黑=1: 1)导电原料含量超过30wt%时,可在炭/陶复合材料内部形成良好的连续导电通道,且该材料具有优良的电发热性能.     

波音757客改货中的9G隔框组件区域改装

简要介绍了9G隔框组件区域改装的主要工作内容以及改装的技术特点和创新点,讨论了如何合理协调安排9G隔框组件区域改装,以便各个专业和各个区域更为合理地在不同时间安排人力,在保证改装质量的前提下能够更高效地完成客改货项目。