轴对称矢量喷管的气膜冷却及红外辐射耦合计算分析

为考察喷管壁面气膜冷却以及红外辐射特性对高性能航空发动机壁温分布的影响,对燃气红外波带的光谱特性采用窄波段模型计算,对壁面-燃气辐射采用封闭腔模型计算,对喷管收敛段的气膜冷却采用绝热温比计算。对于包含喷管壁面、隔热屏、套筒的多层结构传热建立壁温-热流耦合的热平衡方程,用Newt on-Raphson求解得到喷管及内外结构的壁温。对NASA TN D-1988中试验台架发动机喷管扩张段的气膜冷却及壁温进行验证计算,并详细计算了收敛段采用多排缝槽气膜冷却的轴对称矢量喷管。结果表明:气膜冷却有效降低了喷管收敛段的壁温,使得喷管扩张段成为受热严峻的部位;扩张段偏转改变了扩张段壁面温度和红外辐射的圆周分布,沿偏转方向的壁温和红外辐射都明显低于偏转反方向的,2个方向上的平均壁温相差约4.8%,喷管在后半球的辐射沿偏转方向增强。数值模拟结果与试验测量值吻合良好,可用于发动机喷管壁温分布精确计算。     

基于VLBI的上行组阵标校技术研究

天线组阵能否完全替代大口径天线有一个关键性难题,就是天线阵是否支持上行链路组阵。深空航天器无法将不同地面天线的上行信号对齐,所以上行链路信号的调整必须在地面完成。针对上行组阵发射机相位调整问题,提出一种基于VLBI(Very Long Baseline Interferometry,甚长基线干涉测量)技术的接收模式天线上行组阵标校方案,并对标校精度进行了简要分析。将上行链路时延分解为几何时延和发射系统时延,建立了几何时延模型,通过标定接收时延和发射时延,便可以得到天线阵元间的相位标校值。理论分析结果表明,该方案具有一定的可行性,对上行组阵相位标校的研究具有一定的借鉴意义。     

基于波位聚类的相控阵雷达群目标调度模型

如何有效分配有限的能量和时间资源,从而实现大量密集群目标的跟踪测量,是相控阵雷达资源调度面临的难点问题。在采用基于最小期望时间和时间槽优先占用的自适应资源调度模型的基础上,论述了基于波位动态聚类及分区识别算法的相控阵雷达群目标调度模型,详细描述了群目标调度流程图。群目标调度模型根据距离门宽度、方位俯仰波束宽度、目标速度、航迹预测误差和点迹测量误差等确定群目标的分区位置及大小,自动实现群目标的聚类和跟踪。仿真分析表明:该模型能够适应目标群的动态演化过程,实现群内外所有目标的独立跟踪,有效节约群目标跟踪时的资源开销,并已在实际工程应用中得到了验证。     

线形浮标阵搜潜时无人机监听航路规划

航空反潜时,无人机代替有人机对浮标阵进行监听是无人机在未来战场上的重要应用之一。以无人机独立执行监听线形浮标阵任务为背景,在对巡逻搜潜时线形浮标阵的布设进行分析并提出无人机航路的代价函数后,根据浮标阵的特点,规划出了平行监听和垂直监听2种无人机监听浮标阵方案,并对所规划航路的技术指标进行了分析。通过仿真,对这2种方案进行了验证,仿真结果分析表明了2种方案的优劣。     

Thermal protection mechanism of heat pipe in leading edge under hypersonic conditions

Sharp local structure, like the leading edge of hypersonic aircraft, confronts a severe aerodynamic heating environment at a Mach number greater than 5. To eliminate the danger of a material failure, a semi-active thermal protection system is proposed by integrating a metallic heat pipe into the structure of the leading edge. An analytical heat-balance model is established from traditional aerodynamic theories, and then thermal and mechanical characteristics of the structure are studied at Mach number 6–8 for three refractory alloys, Inconel 625, C-103, and T-111. The feasibility of this simple analytical method as an initial design tool for hypersonic aircraft is assessed through numerical simulations using a finite element method. The results indicate that both the isothermal and the maximum temperatures fall but the von Mises stress increases with a longer design length of the leading edge. These two temperatures and the stress rise remarkably at a higher Mach number. Under all investigated hypersonic conditions, with a 3 mm leading edge radius and a0.15 m design length, the maximum stress exceeds the yield strength of Inconel 625 at Mach numbers greater than 6, which means a material failure. Moreover, both C-103 and T-111 meet all requirements at Mach number 6–8.     

Energization of Plasma Species by Intermittent Kinetic Alfvén Waves

We propose a new phase-mixing sweep model of coronal heating and solar wind acceleration based on dissipative properties of kinetic Alfvén waves (KAWs). The energy reservoir is provided by the intermittent ∼1 Hz MHD Alfvén waves excited at the coronal base by magnetic restructuring. These waves propagate upward along open magnetic field lines, phase-mix, and gradually develop short wavelengths across the magnetic field. Eventually, at 1.5–4 solar radii they are transformed into KAWs. We analyze several basic mechanisms for anisotropic energization of plasma species by KAWs and find them compatible with observations. In particular, UVCS (onboard SOHO) observations of intense cross-field ion energization at 1.5–4 solar radii can be naturally explained by non-adiabatic ion acceleration in the vicinity of demagnetizing KAW phases. The ion cyclotron motion is destroyed there by electric and magnetic fields of KAWs.     

The James Webb Space Telescope

The James Webb Space Telescope (JWST) is a large (6.6 m), cold (<50 K), infrared (IR)-optimized space observatory that will be launched early in the next decade into orbit around the second Earth–Sun Lagrange point. The observatory will have four instruments: a near-IR camera, a near-IR multiobject spectrograph, and a tunable filter imager will cover the wavelength range, 0.6 < ; < 5.0 μ m, while the mid-IR instrument will do both imaging and spectroscopy from 5.0 < ; < 29 μ m.The JWST science goals are divided into four themes. The key objective of The End of the Dark Ages: First Light and Reionization theme is to identify the first luminous sources to form and to determine the ionization history of the early universe. The key objective of The Assembly of Galaxies theme is to determine how galaxies and the dark matter, gas, stars, metals, morphological structures, and active nuclei within them evolved from the epoch of reionization to the present day. The key objective of The Birth of Stars and Protoplanetary Systems theme is to unravel the birth and early evolution of stars, from infall on to dust-enshrouded protostars to the genesis of planetary systems. The key objective of the Planetary Systems and the Origins of Life theme is to determine the physical and chemical properties of planetary systems including our own, and investigate the potential for the origins of life in those systems. Within these themes and objectives, we have derived representative astronomical observations.To enable these observations, JWST consists of a telescope, an instrument package, a spacecraft, and a sunshield. The telescope consists of 18 beryllium segments, some of which are deployed. The segments will be brought into optical alignment on-orbit through a process of periodic wavefront sensing and control. The instrument package contains the four science instruments and a fine guidance sensor. The spacecraft provides pointing, orbit maintenance, and communications. The sunshield provides passive thermal control. The JWST operations plan is based on that used for previous space observatories, and the majority of JWST observing time will be allocated to the international astronomical community through annual peer-reviewed proposal opportunities.     

红外目标旋转模拟器校准方法的研究设想

文章简要介绍了红外目标旋转模拟器的结构组成、工作原理,给出了红外目标旋转模拟器的目标温度、平均角速度、角速度波动的校准方法,该校准方法能为光电设备的量值溯源提供解决方案.     

ALGORITHMS FOR TRACKING MANEUVERING TARGET WITH PHASED ARRAY RADAR

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The Silicate Material in Comets

Silicates in comets appear to be a mix of high-temperature crystalline enstatite and forsterite plus glassy or amorphous grains that formed at lower temperatures. The mineral identifications from the 10 and 20 μm cometary spectra are consistent with the composition of anhydrous chondritic aggregate IDPs. The origin of the cometary silicates remains puzzling. While the evidence from the IDPs points to a pre-solar origin of both crystalline and glassy components, the signatures of crystalline silicates appear in the spectra of young stellar objects only at a late evolutionary stage, when comets are the likely source of the dust. This revised version was published online in June 2006 with corrections to the Cover Date.