发动机舱内部传热和蒙皮的降温规律

建立了简化的发动机舱物理模型,对通风冷却和辐射遮挡的蒙皮降温效果进行了数值模拟和实验研究,并对发动机舱内部传热规律进行了分析.结果表明:数值计算得到的发动机舱蒙皮表面沿程分布与实验结果吻合良好.在加热壁面分段的热边界条件下,无辐射遮挡且无通风时蒙皮内侧表面接受的热流占热壁面加热热流的比值约为78%,当发动机舱通风速度达到1m/s时该比值降至20%;当通风速度从0m/s增大至3.5m/s时,发动机舱蒙皮峰值温度的降幅约为10%;无通风条件下有辐射遮挡的蒙皮峰值温度相对于无辐射遮挡的情形降幅约为6%;在通风冷却和辐射遮挡的综合作用下,蒙皮峰值温度相对于无通风且无辐射遮挡的基准状况可降低约50K,相对降幅约为14%.      

组合发动机蒙皮壁温计算方法研究

为满足组合发动机总体热防护的需要,分别采用参考温度法和大气透过率计算软件MODTRAN4计算了组合发动机蒙皮所受的气动加热和环境热辐射。利用本文建立的稳态热平衡方程,迭代求解得到组合发动机蒙皮在典型飞行工况下的一维稳态温度分布。将本文计算的结果与美国航空航天局(NASA)的实验结果进行对比,误差不大于6%。对典型飞行工况下不同蒙皮壁面发射率、不同飞行攻角进行了系列研究。结果表明:随着发射率的提高,蒙皮壁温逐渐降低,随着攻角的增加,蒙皮壁温逐渐增高。在某标准工况下,发射率为1.0的蒙皮温度比发射率为0.1的蒙皮温度低98.01K,降幅为12.76%。攻角为45°的蒙皮温度比攻角为0°的蒙皮温度高95.45K,增幅为13.14%。     

蒙皮材料对浮空器热特性影响的研究

分析临近空间浮空器热特性的影响因素,并建立临近空间浮空器热特性的数学模型,采用Fortran语言编写程序,对蒙皮材料热辐射特性对浮空器热特性的影响进行了研究.结果表明,选用短波吸收率较低且长波辐射发射率较高的蒙皮材料时,氦气平均温度的昼夜差值较低,浮空器热性能越好.夜晚蒙皮温差随长波辐射发射率的增加而增加;而白天随短波辐射吸收率的增加而增加,在长波辐射发射率较大时,其对蒙皮温差的影响不大,然而长波辐射发射率比较小时,蒙皮温差会非常大,蒙皮温差的峰值出现于黎明和黄昏时段这两个时段.     

航空电子设备冷却用环路热管冷凝器热沉分析

为确定环路热管用于机载电子设备散热的适用性,讨论了应用于航空电子设备冷却的环路热管冷凝器可用热沉,提出将机翼蒙皮作为环路热管冷凝器的热沉.通过机翼蒙皮的传热分析,计算了飞行任务包线下机翼蒙皮内表面温度,以确定环路热管冷凝器热沉温度范围.理论计算表明,利用环路热管将机载电子设备的热量耗散于飞机蒙皮是一种可行的热管理技术.      

直升机传热与红外特征建模与分析(英文)

直升机蒙皮表面及排气温度分布受到发动机排气系统、旋翼下洗气流和太阳辐射的直接影响。为了能够精确地模拟直升机蒙皮表面及排气温度分布,在进行处于悬停状态的直升机三维流场和温度场建模与分析时,综合考虑了旋翼下洗对喷流的影响和太阳辐射对机身加热的影响。基于温度场和流场数据,通过正反射线踪迹法对直升机红外波段辐射强度的分布进行计算。针对一假想的排气系统与后机身融合的直升机模型,本文对其热特性和红外辐射特性进行了数值计算和分析。     

大气及地面红外辐射对高空飞机长波低发射率红外隐身效果的影响

计算分析了蒙皮反射的大气及地面红外辐射对高空飞机采用低发射率材料的红外隐身效果的影响.蒙皮温度采用恢复温度,红外辐射采用反向蒙特卡罗法计算.考虑了夏季和冬季两种典型大气和地面条件,亚声速巡航和超声速巡航两种飞行状态.结果表明:蒙皮对背景红外辐射的反射使得低发射率材料对飞机红外辐射强度的抑制效率降低1.5%~6%;考虑反射的背景红外辐射时,探测距离增加20%~70%;背景红外辐射对低速飞机的红外辐射影响较大,且夏季比冬季更明显;当飞行速度较低时,降低飞机上表面发射率,当飞行速度较高时,降低飞机全部表面的发射率,可获得更好的红外隐身效果.      

基于假想衰减项法的超压气球结构有限元分析

采用基于假想衰减项的非线性有限元显式动力学方法对超压气球结构模型进行了仿真,探讨了加强筋数量对球体应力和变形的影响。结果表明,超压气球经向布置的加强筋能显著降低气球蒙皮经线方向上的应力水平,同时由于加强筋对蒙皮的约束作用使气球蒙皮产生"鼓包",改变了蒙皮纬线方向的曲率半径,从而减小了纬向张力,提高气球整体的耐超压水平;根据仿真计算结果,当加强筋数量从0增加到36时,蒙皮的经、纬向应力值均显著下降,其中经向下降幅度更大,达64.4%。     

直升机发动机舱通风、遮挡和隔热对红外辐射特性的影响

为了降低直升机发动机舱蒙皮的温度,减弱直升机红外辐射能量,采用数值仿真的方法研究其处于悬停状态、考虑了旋翼下洗作用的发动机舱蒙皮温度场和直升机红外辐射特性.针对基准发动机舱结构提出了在舱内加设辐射遮挡套、增开通风百叶窗、排气管尾缘修型和蒙皮内侧敷设隔热层等改进方案,研究了上述改进方案对直升机发动机舱蒙皮温度场和红外辐射特性的影响,得到了如下结论:①在发动机舱内加设辐射遮挡套后,整机侧向探测方位角内3~5μm红外辐射强度出现了约25%的增幅,8~14μm波段红外辐射与原始结构相当.②在发动机舱顶部增开通风百叶窗,直升机3~5μm红外辐射低于原始结构约12%,8~14μm波段红外辐射与原始结构相当.③在发动机舱顶部增开通风百叶窗的基础上,对排气管尾缘采取延伸遮挡以及在发动机舱蒙皮内侧敷设隔热层,整机3~5μm波段红外辐射的最大值下降约70%,8~14μm波段红外辐射的最大值下降约10%.      

基于内外传热耦合的热气防冰系统仿真计算

基于内外传热耦合原理,建立了热气防冰系统的AMESim仿真模型,研究热气防冰系统在不同引气状态下,管路流量、压力及蒙皮温度的变化规律.采用所建立的仿真方法,计算飞机机翼热气防冰系统的内部流动特性和内外耦合传热特性,将计算结果与热气防冰系统流量分配试验结果进行对比.结果表明:管路流量、压力和蒙皮温度的仿真计算结果与试验结果最大误差为9%,验证了该仿真模型的正确性.在此基础上,对飞机短舱热气防冰系统进行了仿真,分析了飞行包线下系统内外的换热、温度变化、加热效率等关键参数的瞬态特性.仿真结果为热气防冰系统的设计、分析与优化提供依据.      

加装红外抑制器的直升机红外辐射的计算及测量

计算了光谱在3～5 μm及8～12 μm范围内,加装与机身结构一体化红外抑制器的某型直升机排气系统的红外辐射特性.计算中考虑了排气系统部分蒙皮的红外辐射、双喷管发动机喷气流的红外辐射、背景辐射及大气的吸收衰减对直升机排气系统红外辐射信号的影响.实验发现,一架加装与机身结构一体化红外抑制器的直升机排气系统红外辐射特性的计算结果,与实测结果基本一致.     

Radiation climate map for analyzing risks to astronauts on the mars surface from galactic cosmic rays

The potential risks for late effects including cancer, cataracts, and neurological disorders due to exposures to the galactic cosmic rays (GCR) is a large concern for the human exploration of Mars. Physical models are needed to project the radiation exposures to be received by astronauts in transit to Mars and on the Mars surface, including the understanding of the modification of the GCR by the Martian atmosphere and identifying shielding optimization approaches. The Mars Global Surveyor (MGS) mission has been collecting Martian surface topographical data with the Mars Orbiter Laser Altimeter (MOLA). Here we present calculations of radiation climate maps of the surface of Mars using the MOLA data, the radiation transport model HZETRN (high charge and high energy transport), and the quantum multiple scattering fragmentation model, QMSFRG. Organ doses and the average number of particle hits per cell nucleus from GCR components (protons, heavy ions, and neutrons) are evaluated as a function of the altitude on the Martian surface. Approaches to improve the accuracy of the radiation climate map, presented here using data from the 2001 Mars Odyssey mission, are discussed.     

2001 Mars Odyssey Mission Summary

The 2001 Mars Odyssey spacecraft, now in orbit at Mars, will observe the Martian surface at infrared and visible wavelengths to determine surface mineralogy and morphology, acquire global gamma ray and neutron observations for a full Martian year, and study the Mars radiation environment from orbit. The science objectives of this mission are to: (1) globally map the elemental composition of the surface, (2) determine the abundance of hydrogen in the shallow subsurface, (3) acquire high spatial and spectral resolution images of the surface mineralogy, (4) provide information on the morphology of the surface, and (5) characterize the Martian near-space radiation environment as related to radiation-induced risk to human explorers. To accomplish these objectives, the 2001 Mars Odyssey science payload includes a Gamma Ray Spectrometer (GRS), a multi-spectral Thermal Emission Imaging System (THEMIS), and a radiation detector, the Martian Radiation Environment Experiment (MARIE). THEMIS and MARIE are mounted on the spacecraft with THEMIS pointed at nadir. GRS is a suite of three instruments: a Gamma Subsystem (GSS), a Neutron Spectrometer (NS) and a High-Energy Neutron Detector (HEND). The HEND and NS instruments are mounted on the spacecraft body while the GSS is on a 6-m boom. Some science data were collected during the cruise and aerobraking phases of the mission before the prime mission started. THEMIS acquired infrared and visible images of the Earth-Moon system and of the southern hemisphere of Mars. MARIE monitored the radiation environment during cruise. The GRS collected calibration data during cruise and aerobraking. Early GRS observations in Mars orbit indicated a hydrogen-rich layer in the upper meter of the subsurface in the Southern Hemisphere. Also, atmospheric densities, scale heights, temperatures, and pressures were observed by spacecraft accelerometers during aerobraking as the spacecraft skimmed the upper portions of the Martian atmosphere. This provided the first in-situ evidence of winter polar warming in the Mars upper atmosphere. The prime mission for 2001 Mars Odyssey began in February 2002 and will continue until August 2004. During this prime mission, the 2001 Mars Odyssey spacecraft will also provide radio relays for the National Aeronautics and Space Administration (NASA) and European landers in early 2004. Science data from 2001 Mars Odyssey instruments will be provided to the science community via NASA’s Planetary Data System (PDS). The first PDS release of Odyssey data was in October 2002; subsequent releases occur every 3 months.     

Radar observations of Mars

Radar observations in the past were used to investigate the astronomical properties of the planet and its reflectivity in radar frequencies. Because of the difficulties in signal detection and processing due to the low level of return signal, the data were published only in the form of Doppler spectrograms. In view of the increasing interest in Mars and the practicability of missions to Mars this paper uses the published data to evaluate the angular behavior of the radar backscattering characteristics of Mars; a required information for the design of radar equipment of spacecrafts. In addition, results of past observations are summarized, analyzed and discussed in terms of a general interpretation of the Martian surface. It is found that the generally accepted suggestion that Mars is a relatively smooth planet, smoother than the Moon, is confirmed by most of the results, but not all observations agree with this hypothesis. A surface model of relief and composition based on radar information in conjunction with other observations is reviewed. The processing methods of radar return signals are compared for a better understanding of the handling of the Doppler spectrogram, a form which is most widely used for the presentation of processed data.An extensive bibliography of available papers and reports relevant to radar observations and the surface and lower atmosphere of Mars is included. The literature is concerned mainly with post-Mariner IV experiment, the mission which changed considerably many conceptions of Mars.     

四种飞行器绕流的三维DSMC计算与传热分析

在地球大气层与火星大气层中,使用自己编制的DSMC(direct simulation Monte Carlo)源程序完成了四种飞行器(即Apollo,Orion,Mars Pathfinder以及Mars Microprobe)高超声速穿越稀薄气体时的三维绕流计算,给出了上述飞行器42个典型飞行工况(其中包括在地球大...     

The seasonal cycle of water on Mars

A review of the behavior of water in the Mars atmosphere and subsurface is appropriate now that data from the Mariner and Viking spacecraft have been analyzed and discussed for several years following completion of those missions. Observations and analyses pertinent to the seasonal cycle of water vapor in the atmosphere of Mars are reviewed, with attention toward transport of water and the seasonal exchange of water between the atmosphere and various non-atmospheric reservoirs. Possible seasonally-accessible sources and sinks for water include water ice on or within the seasonal and residual polar caps; surface or subsurface ice in the high-latitude regions of the planet; adsorbed or chemically-bound water within the near-surface regolith; or surface or subsurface liquid water. The stability of water within each of these reservoirs is discussed, as are the mechanisms for driving exchange of the water with the atmosphere and the timescales for exchange. Specific conclusions are reached about the distribution of water and the viability of each mechanism as a seasonal reservoir. Discussion is also included of the behaviour of water on longer timescales, driven by the variations in solar forcing due to the quasi-periodic variations of the orbital obliquity. Finally, specific suggestions are made for future observations from spacecraft which would further define or constrain the seasonal cycle of water.     

The Radiation Assessment Detector (RAD) Investigation

The Radiation Assessment Detector (RAD) on the Mars Science Laboratory (MSL) is an energetic particle detector designed to measure a broad spectrum of energetic particle radiation. It will make the first-ever direct radiation measurements on the surface of Mars, detecting galactic cosmic rays, solar energetic particles, secondary neutrons, and other secondary particles created both in the atmosphere and in the Martian regolith. The radiation environment on Mars, both past and present, may have implications for habitability and the ability to sustain life. Radiation exposure is also a major concern for future human missions. The RAD instrument combines charged- and neutral-particle detection capability over a wide dynamic range in a compact, low-mass, low-power instrument. These capabilities are required in order to measure all the important components of the radiation environment. RAD consists of the RAD Sensor Head (RSH) and the RAD Electronics Box (REB) integrated together in a small, compact volume. The RSH contains a solid-state detector telescope with three silicon PIN diodes for charged particle detection, a thallium doped Cesium Iodide scintillator, plastic scintillators for neutron detection and anti-coincidence shielding, and the front-end electronics. The REB contains three circuit boards, one with a novel mixed-signal ASIC for processing analog signals and an associated control FPGA, another with a second FPGA to communicate with the rover and perform onboard analysis of science data, and a third board with power supplies and power cycling or “sleep”-control electronics. The latter enables autonomous operation, independent of commands from the rover. RAD is a highly capable and highly configurable instrument that paves the way for future compact energetic particle detectors in space.     

X-Rays From Mars

X-rays from Mars were first detected in July 2001 with the satellite Chandra. The main source of this radiation was fluorescent scattering of solar X-rays in its upper atmosphere. In addition, the presence of an extended X-ray halo was indicated, probably resulting from charge exchange interactions between highly charged heavy ions in the solar wind and neutrals in the Martian exosphere. The statistical significance of the X-ray halo, however, was very low. In November 2003, Mars was observed again in X-rays, this time with the satellite XMM-Newton. This observation, characterized by a considerably higher sensitivity, confirmed the presence of the X-ray halo and proved that charge exchange is indeed the origin of the emission. This was the first definite detection of charge exchange induced X-ray emission from the exosphere of another planet. Previously, this kind of emission had been detected from comets (which are largely exospheres) and from the terrestrial exosphere. Because charge exchange interactions between atmospheric constituents and solar wind ions are considered as an important nonthermal escape mechanism, probably responsible for a significant loss of the Martian atmosphere, X-ray observations may lead to a better understanding of the present state of the Martian atmosphere and its evolution. X-ray images of the Martian exosphere in specific emission lines exhibited a highly anisotropic morphology, varying with individual ions and ionization states. With its capability to trace the X-ray emission out to at least 8 Mars radii, XMM-Newton can explore exospheric regions far beyond those that have been observationally explored to date. Thus, X-ray observations provide a novel method for studying processes in the Martian exosphere on a global scale.     

8. The thermal balance of the atmosphere of venus

Current knowledge of the temperature structure of the atmosphere of Venus is briefly summarized. The principal features to be explained are the high surface temperature, the small horizontal temperature contrasts near the cloud tops in the presence of strong apparent motions, and the low value of the exospheric temperature. In order to understand the role of radiative and dynamical processes in maintaining the thermal balance of the atmosphere, a great deal of additional data on the global temperature structure, solar and thermal radiation fields, structure and optical properties of the clouds, and circulation of the atmosphere are needed. The ability of the Pioneer Venus Orbiter and Multiprobe Missions to provide these data is indicated.