外并联式TBCC发动机模态转换性能模拟与分析

针对Ma7一级外并联式TBCC发动机,发展了组合进气道模态转换性能简化计算模型和高马赫数涡轮发动机风车性能计算模型,实现了TBCC发动机由涡轮模态至冲压模态完整转换过程的动态性能模拟。将模态转换过程划分为冲压发动机冷通流打开和涡轮发动机关闭加力、降转、风车关闭等四个典型阶段,基于推力连续准则提出了模态转换策略。计算结果表明:模态转换期间,TBCC发动机的推力转换主要发生在涡轮发动机由全加力状态变化至不加力状态过程中;模态转换前期处于冷通流状态的冲压发动机以及后期处于风车状态的涡轮发动机产生负推力,最大值分别为模态转换后总推力的5.3%和13.7%;当涡轮发动机进入风车状态时,风扇和压气机的工作点均位于其特性图的低转速大流量区域,此后随着涡轮发动机空气流量的减小,风扇压比和压气机压比均趋向于1.0,与相关试验结果基本一致。     

串联式TBCC发动机模态转换模拟

为开展涡轮基组合循环(TBCC)发动机模态转换过程研究,基于某小型涡喷发动机,应用串联式TBCC发动机总体性能数值计算程序进行性能计算。根据沿飞行轨道TBCC发动机冲压涵道与涡轮发动机涵道气流混合过程中的参数变化规律,开展模态转换过程模拟。分析了不同等动压头、加力/冲压燃烧室进口马赫数、出口温度等主要参数对发动机性能的影响。根据小型串联式TBCC发动机模态转换过程和沿飞行轨道的发动机稳态特性模拟,确定了较为合理的模态转换区间,并得到了推力、耗油率等发动机性能参数。研究表明:不同动压头对应不同的模态转换马赫数,加力/冲压燃烧室进口马赫数和出口总温对模态转换马赫数并无影响。     

Ma4一级内并联式TBCC发动机模态转换性能分析

涡轮基组合循环(TBCC)发动机是未来远程高速飞行器和可重复使用双级入轨(TSTO)飞行器第一级运载器的理想动力,而模态转换是实现TBCC发动机工程实用所必须解决的关键技术之一。针对Ma4一级内并联式TBCC发动机,分析了其工作原理,发展了相应的总体性能计算模型,该模型考虑了进气道与发动机的流量匹配关系,改进了发动机模型的迭代求解方法。通过对比涡轮模态与冲压模态的净推力、单位燃油消耗率沿飞行轨迹的变化规律,确定模态转换马赫数为3.0。根据模态转换期间发动机推力、空气流量连续变化的基本要求,提出了一种根据涡轮发动机工作状态分三阶段进行的模态转换策略,确定了模态转换过程的参数调节规律。模态转换动态性能模拟结果表明,基本实现了涡轮模态至冲压模态的平稳转换,但在涡轮发动机加力关闭时,为保证发动机空气流量连续变化,发动机总推力将出现短暂的下降,降幅约为12.5%。     

国外并联式涡轮基组合循环发动机技术发展途径浅析

为借鉴国外并联式涡轮基组合循环(TBCC)发动机技术研究经验,从飞行器使用需求出发,分析了并联式TBCC发动机面临的技术挑战,并从高速涡轮基技术、冲压发动机技术和组合技术三个方面,梳理了美国典型并联式TBCC发动机的研发计划。在此基础上,分析并提出了并联式TBCC发动机技术发展途径:拓展涡轮基工作马赫数上限和冲压发动机工作马赫数下限以实现并联式TBCC发动机模态转换,采用射流预冷技术扩展现有涡轮工作包线是短期内实现性较好的技术验证途径,开发高速涡轮发动机技术是未来发展的必然趋势。     

基于推力连续准则的小型涡轮冲压组合发动机模态转换过程分析

基于数值模拟方法开展了小型涡轮冲压组合发动机性能计算与匹配性分析.给出了详细的性能计算流程、设计点参数确定准则和模态转换过程参数计算方法.根据涡喷发动机压气机进口、涡轮出口的总静压参数沿飞行轨迹的变化规律,确定了涡轮模态向冲压模态转换的合理区间.根据冲压燃烧室进口参数和静压平衡等约束条件,确定了小型涡轮冲压组合发动机关键截面几何参数.分析了不同的流量调节阀开度对模态转换过程参数变化的影响.按照推力连续的准则,确定了模态转换过程流量调节阀开度随马赫数的变化规律.最后给出了沿飞行轨迹的涡轮冲压组合发动机推力、比冲和喷管喉道面积的变化.      

Ma4内并联TBCC发动机匹配设计与模态转换性能分析

由于发动机自身工作能力的限制,要想获得最大的发动机性能,在不同的飞行马赫数下,对应不同的发动机形式,因此为了达到宽马赫数飞行的目的,在不同工作区间采用不同发动机进行工作的组合循环发动机应运而生。涡轮基组合循环发动机(TBCC)作为组合动力的一种,采用涡轮发动机与冲压发动机组合的形式,可以在未来作为远程高速飞行器和可重复使用2级入轨(TSTO)飞行器的第1级动力,有广阔的使用前景。作为宽速域内工作的 TBCC,模态转换是实现 TBCC 发动机宽马赫数工作必须解决的关键技术问题之一。针对Ma4 速域 TBCC 发动机,建立了相应的涡轮发动机与亚燃冲压发动机并联模型,通过考虑2种发动机的设计点与非设计点工作条件,对模态转换马赫数进行了选择,并基于保持固定流量这个前体条件,给出了相应的并联TBCC 模态转换控制过程。基于建模并联模型,初步确定了采用涡轮与亚燃冲压动力的 TBCC 发动机的可行性,在合适的匹配条件下,TBCC 组合动力可以满足飞行器的推力需求。     

并联式涡轮冲压组合发动机安装性能数值模拟

为了研究涡轮基组合循环发动机的安装性能,基于美国Georgia大学工程技术研究中心提出的HSF高速飞行器,选择并联式涡扇-冲压组合发动机方案作为研究对象.采用数值模拟方法,研究了并联式涡扇-冲压组合发动机的工作模式转换点的确定方法,以及模式转换过程中气动参数变化和几何调节规律,建立了适用于并联式涡轮基组合发动机的进排气系统安装损失计算模型及安装性能计算模型.研究表明,通过几何和发动机供油规律调节,可保证在推力连续的准则下完成工作模式转换,发动机的安装性能满足飞行器的要求.     

基于二次流喷射的并联式TBCC排气系统性能提升技术研究

基于CFD数值模拟方法,分析了并联式涡轮基组合循环发动机(Turbine Based Combined Cycle,TBCC)排气系统的内外流场特性,提出了在涡轮喷管下壁面处喷入高压二次流以提升排气系统性能的方式,研究了不同飞行状态下二次流喷射对排气系统性能(推力系数、推力矢量角)的影响规律。计算结果表明:二次流喷射会产生弓形激波,与喷管上膨胀壁面附面层作用产生新的分离区,提升涡轮喷管和冲压喷管内的整体压力,从而改善并联式TBCC排气系统的推力及推力矢量性能,且对亚声速和跨声速飞行状态下的并联式TBCC排气系统性能改善比较明显,可使轴向推力系数最大提升7.34%,推力矢量角提升12.76°。     

串联式TBCC发动机风车冲压模态性能模拟

建立了基于部件低转速特性匹配的串联式涡轮基组合循环（TBCC）发动机风车冲压模态性能计算模型,提出了压气机低转速大流量特性扩展方法,由换算扭矩代替等熵效率表示旋转部件特性,解决了低转速部件效率不连续相关问题。分析了冲压外涵面积变化和涡轮功率提取对风车冲压模态性能及部件匹配的影响规律,并基于推力、流量连续准则设计了涡轮模态至冲压模态转换过程（含风车冲压模态）的参数调节规律。计算结果表明:在风车冲压模态下,冲压外涵面积变化对风扇工作状态有显著影响,对压气机影响较小;涡轮可提取功率随着风车转速的减小先增加后降低,比冲随提取功率的增加基本呈线性降低趋势,功率提取位置（高、低压涡轮）对部件匹配有显著影响。      

TBCC发动机涡轮进气道喷水冷却特性数值研究

对涡轮基组合循环(Turbine Based Combined Cycle, TBCC)发动机涡轮进气道进行喷水冷却是解决TBCC发动机推力不连续问题的有效方式之一。本文基于实际流场条件选取某型TBCC发动机涡轮进气道结构,对进气道内喷水冷却特性进行了数值仿真,研究飞行器不同工况下水滴的蒸发特性及喷水对来流高温空气的预冷效果。结果表明,来流空气温度降幅随水气比提高而增大,最高温降可达152.4K。水气比提高后水滴蒸发率逐渐降低,但蒸发总量仍会继续上升。相同水气比条件下,飞行马赫数越高,喷水冷却效果越明显。在Ma3.5飞行速度和水气比0.03条件下有最高蒸发率,达83.05%。喷水冷却有效扩展了涡轮模态飞行马赫数,最高能使飞行速度提升至Ma2.84,即喷水冷却扩展了TBCC从涡轮模态向超燃冲压模态转换的衔接速域。     

捷变频磁控管用高频直线振荡电机设计

捷变频磁控管的快速捷变特性取决于驱动电机的性能,要求电机功耗小、体积小、效率高,能实现高频稳幅直线振动.文章介绍了音圈直线电机、电磁开关式直线电机和电磁混合式直线电机等三种方案,通过对其工作原理和性能特点分析,确定了音圈直线电机驱动方案,进行了电磁场仿真分析和电磁参数设计,进行了样机试验测试.结果表明,设计的音圈直线电...     

桨叶实度及轴间距对摆线桨气动特性影响研究

悬停状态下,设计参数和摆线桨间距离对摆线桨的气动特性有较大影响。首先通过算例验证滑移网格计算方法应用于摆线桨悬停状态下气动力计算的准确性,然后研究摆线桨在不同半径、弦长和桨叶数时的气动参数特性,最后计算分析不同距离时,摆线桨间的气动干扰特性。结果表明:随着半径增大,桨叶气动力和单位面积上载荷均增大;弦长越大,气动力越大,桨叶单位面积上载荷反而越小;4叶片摆线桨产生的气动力比3叶片和6叶片大,而3叶片的桨叶载荷最大;合力偏转角分别随转速和实度的增大而减小;随着摆线桨间距离的增加,气动力损失系数和合力偏转角均减小。     

A new target tracking filter based on deep learning

At present, current filters can basically solve the filtering problem in target tracking, but there are still many problems such as too many filtering variants, too many filtering forms, loosely coupled with the target motion model, and so on. To solve the above problems, we carry out crossapplication research of artificial intelligence theory and methods in the field of tracking filters. We firstly analyze the computation graphs of typical a-β and Kalman. Through analysis, it is concluded that ...     

Investigations of entrainment characteristics and shear-layer vortices evolution in an axisymmetric rear variable area bypass injector

In this study,firstly,for the axisymmetric RVABI,the change-rule of adverse pressure gradient caused by radial velocity during the transition of internal flow mode in variable geometry is summarized,and a Bypass Ratio(BR) iterative algorithm based on the empirical correlation of non-equilibrium pressure is proposed.The algorithm can estimate the nonlinear relationship between area ratio and BR,with an error range falling below 6.5%.Then,we discuss the favorable effect of uniform mixing on the th...     

PVC糊树脂对交联PVC泡沫塑料的影响

通过水煮发泡制备交联聚氯乙烯泡沫塑料,讨论了聚氯乙烯(PVC)糊树脂对泡沫制备过程中经制糊、模压和发泡工艺得到的产物的影响,研究了PVC糊树脂对制备的交联PVC泡沫压缩性能的影响.结果表明:制备交联聚氯乙烯泡沫塑料适宜的糊黏度是4～9 Pa·s;PVC糊树脂的K值较大或水萃取液pH值呈碱性可有效防止模压过程中PVC的降解;PVC糊树脂的水萃取液pH值呈碱性可催化发泡反应,有利于得到低密度泡沫且缩短发泡时间;随着其K值增加,制备的泡沫压缩强度增大,但是K值过大时,制备的泡沫泡孔较大,压缩强度反而降低,适宜的K值为70～80.     

Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

Multiframe weak target track-before-detect based on pseudo-spectrum in mixed coordinates

Traditional multiframe Track-Before-Detect(TBD) may incur adverse integration loss resulting from model mismatch in sensor coordinates. Its suboptimal integration strategy may cause target envelope degradation. To address these issues, a pseudo-spectrum-based multiframe TBD in mixed coordinates is proposed firstly. The data search for energy integration is conducted based on an accurate model in the x-y plane while target energy is integrated based on pseudo-spectrum in sensor coordinates. The a...     

Deep Impact: Working Properties for the Target Nucleus – Comet 9P/Tempel 1

In 1998, Comet 9P/Tempel 1 was chosen as the target of the Deep Impact mission (A’Hearn, M. F., Belton, M. J. S., and Delamere, A., Space Sci. Rev., 2005) even though very little was known about its physical properties. Efforts were immediately begun to improve this situation by the Deep Impact Science Team leading to the founding of a worldwide observing campaign (Meech et al., Space Sci. Rev., 2005a). This campaign has already produced a great deal of information on the global properties of the comet’s nucleus (summarized in Table I) that is vital to the planning and the assessment of the chances of success at the impact and encounter. Since the mission was begun the successful encounters of the Deep Space 1 spacecraft at Comet 19P/Borrelly and the Stardust spacecraft at Comet 81P/Wild 2 have occurred yielding new information on the state of the nuclei of these two comets. This information, together with earlier results on the nucleus of comet 1P/Halley from the European Space Agency’s Giotto, the Soviet Vega mission, and various ground-based observational and theoretical studies, is used as a basis for conjectures on the morphological, geological, mechanical, and compositional properties of the surface and subsurface that Deep Impact may find at 9P/Tempel 1. We adopt the following working values (circa December 2004) for the nucleus parameters of prime importance to Deep Impact as follows: mean effective radius = 3.25± 0.2 km, shape – irregular triaxial ellipsoid with a/b = 3.2± 0.4 and overall dimensions of ∼14.4 × 4.4 × 4.4 km, principal axis rotation with period = 41.85± 0.1 hr, pole directions (RA, Dec, J2000) = 46± 10, 73± 10 deg (Pole 1) or 287± 14, 16.5± 10 deg (Pole 2) (the two poles are photometrically, but not geometrically, equivalent), Kron-Cousins (V-R) color = 0.56± 0.02, V-band geometric albedo = 0.04± 0.01, R-band geometric albedo = 0.05± 0.01, R-band H(1,1,0) = 14.441± 0.067, and mass ∼7×10¹³ kg assuming a bulk density of 500 kg m⁻³. As these are working values, {i.e.}, based on preliminary analyses, it is expected that adjustments to their values may be made before encounter as improved estimates become available through further analysis of the large database being made available by the Deep Impact observing campaign. Given the parameters listed above the impact will occur in an environment where the local gravity is estimated at 0.027–0.04 cm s⁻² and the escape velocity between 1.4 and 2 m s⁻¹. For both of the rotation poles found here, the Deep Impact spacecraft on approach to encounter will find the rotation axis close to the plane of the sky (aspect angles 82.2 and 69.7 deg. for pole 1 and 2, respectively). However, until the rotation period estimate is substantially improved, it will remain uncertain whether the impactor will collide with the broadside or the ends of the nucleus.     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.