The gravity-darkening of the main-sequence components of spectral types A, F and G in detached close binary systems

From analysis of the photometric ellipticity effect in seven well-understood detached close binary systems, empirical values of the exponent of gravity-darkening have been practically deduced for eleven main-sequence components of spectral types A, F and G which should cover the range of structural change (from radiative to convective) in stellar atmospheres. The result indicate that values of the exponent diminish gradually with decreasing effective temperatures from 1.0 for radiative atmospheres with T > 8500 K to = 0.2 0.3 for convective atmospheres with T < 6500 K, in spite of some uncertainty in the reflection correction process.     

Shock Tube Instrumentation Techniques for Study of Hypervelocity Entry Problems

Shock tube instrumentation techniques developed for the study of convective heat transfer and the radiative properties of high temperature gases at conditions simulating hypervelocity entry into planetary atmospheres are described. An electrically heated helium driven shock tube is used; measurement methods suitable for conventional shock tubes must be modified before they can be used in the hypervelocity shock tube. Extremely high shock velocities necessary for proper simulation are associated with very short test times imposing requirements for fast response instrumentation systems. Methods for evaluating test gas quality are illustrated. Techniques described have been applied to several studies; typical results are shown and instrumentation requirements for the extension of aerothermodynamic investigation in the hypervelocity regime are outlined.     

机身减速板流动特性研究（英文）

现役高机动战斗机普遍采用机身减速板来减小飞行速度和转弯半径并提高机动能力。采用物面测压及空间流场测量相结合的实验方法,在机身减速板开度60°,机身迎角0°～70°条件下,研究了机身减速板铰链力矩随迎角的变化规律,分析了减速板迎风侧和背风侧的流动结构。研究结果表明：减速板铰链力矩按迎角可分为3个区域：常值区（α=0°～16°）,减速板铰链力矩基本不变,因为减速板迎风侧正压力逐渐减小,而背风侧负压力逐渐增加,两种相反的变化趋势相互抵消。非线性增长区（α=16°～32°）,减速板铰链力矩显著增加,因为减速板铰链力矩主要贡献区为背风侧,该迎角区内减速板背风侧存在一对不断增强的旋涡,背风侧负压力显著增加。在非线性衰减区（α=32°～70°）,减速板铰链力矩在迎角32°～36°范围内急剧减小,因为在迎角36°减速板背风侧旋涡流动变为速度较低的再附流动;减速板铰链力矩在迎角36°～44°范围内逐渐增加,因为该迎角区作用于减速板迎风侧的机身涡不断增强,导致减速板迎风侧正压力显著增加;减速板铰链力矩在迎角44°～70°范围内逐渐减小,因为该迎角区作用于减速板迎风侧的机身涡不断减弱直至破裂,导致减速板迎风侧正压力逐渐减小。     

Thermal radio emission from the major planets

The use of long-wavelength radio measurements of brightness temperature to remotely measure the thermal structure of the atmospheres of the major planets at great depths (>10 atm.) is discussed. Data are presented which show that the gross features of Jupiter's and Saturn's microwave spectra, as determined from ground based observations, can be explained in terms of thermal emission from ammonia in deep convective atmospheres of He and H₂.This is one of the publications by the Science Advisory Group.     

火箭发动机喷管辐射及壁温的计算研究

研究了火箭发动机复合喷管的耦合换热及瞬态壁温的计算方法,考虑了扩散控制的C/C喉衬的稳态烧蚀,建立了封闭腔-净辐射模型计算喷管内的辐射换热,改进了喷管辐射换热的计算方法.计算了两种复合喷管的壁温随时间的变化,并与有关文献的结果进行对比.研究表明:在火箭发动机喷管的入口段,高温燃气对壁面的辐射换热热流比对流换热热流强;采用封闭腔-净辐射法计算火箭发动机喷管的辐射精度较高.      

Radiative properties of alumina/aluminum particles and influence on radiative heat transfer in solid rocket motor

The thermal radiation of micron-sized condensed phase particles plays a dominant role during the heat transfer process in aluminized Solid Rocket Motors（SRMs）. Open research mainly focuses on the radiative properties of alumina particles while the study considering the presence of aluminum is lacking. In addition, the thermal radiation inside the SRM with consideration of the participating particles is seldom studied. In this work, the multiscale method of predicting the thermal environment insi...     

纳米碳酸盐对复合固体推进剂燃烧性能的影响

研究了纳米碳酸盐对丁羟三组元、丁羟四组元、低燃速NEPE推进剂燃烧性能的影响。结果表明:纳米碳酸盐使丁羟三组元推进剂在高压(10～18MPa)和低压(4～10MPa)段的压强指数降低到0.2以下,同时使燃速明显降低;使丁羟四组元推进剂在高压段(10～18MPa)的压强指数降低到0.26左右;使低燃速NEPE推进剂的的压强指数(4～9MPa)从0.77左右降至0.55以下。从研究结果可以看出,添加该纳米碳酸盐是降低复合推进剂压强指数行之有效的途径。     

燃烧产物二氧化碳高温辐射的窄谱带模型参数

窄谱带模型法与CG近似及LS近似结合能够很好处理非灰、非等温、非均匀介质的辐射传输问题,在飞行器发动机燃烧室及尾喷焰高温辐射传输问题研究中多被采用。二氧化碳是含碳类推进剂主要的燃烧产物,其辐射特性的研究一直受到国内外重视,但其现有的窄谱带模型数据不完整或分辨率太低。本文利用最新的高分辨率高温燃气光谱数据库HITEMP(序列号:3153),并将其中的谱线光谱参数外推到300～3000K的温度范围内,计算得到了一个新的、完整的、分辨率较高的二氧化碳窄谱带模型参数库。以本文计算的模型参数为基础,采用窄谱带模型计算了各种光学路径下的发射率、穿透率,其结果与实验值符合很好。      

用数值计算方法对出口温度与压力指数关系的研究

通过对两种不同类型的燃气轮机燃烧室的数值计算 ,研究了不同燃烧类型对燃气轮机燃烧效率模化试验中压力指数选取的影响 ,结果表明压力指数除受到燃料、余气系数等影响之外 ,燃烧类型对其也有很大影响。对于以碳氢化合物为燃料 ,化学动力学控制类型燃烧室模化中n值相对较大 ,范围为 1 .6～ 2 .0。当燃烧过程受扩散火焰控制时 ,n值相对较小 ,范围为 1 .0～ 1 .4      

at％合金晶化动力学

ａｔ％非晶合金晶化动力学。在恒加热速率晶化曲线上,随升温率在１～４０Ｋ／ｍｉｎ范围变化,分别出现３～４个放热峰。利用Ｋｉｓｉｎｇｅｒ法,Ｏｚａｗａ法和Ａｒｈｅｎｉｕｓ法分别计算了晶化激活能,认为Ａｌ８３Ｙ１０Ｎｉ７非晶合金在Ａｌ－Ｙ－Ｎｉ系有较高的结构稳定性,晶化时第一个放热峰晶化相的等温晶化动力学在０. １５＜ｘ＜０. ８５范围内符合Ｊ－Ｍ－Ａ方程,Ａｖｒａｍｉ指数ｎ＝２. ５;引用阶段Ａｖｒａｍｉ指数和阶段激活能,研究了等温晶化过程中不同阶段的形核和长大行为。     

三维数值模拟再生冷却喷管的换热

为了解液体火箭发动机喷管再生冷却的换热特点，采用数值模拟的方法，对内喷管燃气、壁面和冷却液建立不同的三维控制方程，进行流动和传热的耦合计算。在计算中，假定喷管流动为冻结流动，考虑燃气向壁面的对流换热和辐射换热；采用二阶迎风格式离散控制方程，采用DO模型离散求解辐射换热方程，水蒸气的吸收系数根据Leckner公式计算。计算模型采用缩比热试车发动机，数值计算结果与实验结果吻合较好，较准确地模拟出了喷管的壁面热流密度，得到了喷管燃气和冷却液的流场和温度场，对高压再生冷却喷管的设计具有指导意义。     

Light scattering in planetary atmospheres

This paper reviews scattering theory required for analysis of light reflected by planetary atmospheres. Section 1 defines the radiative quantities which are observed. Section 2 demonstrates the dependence of single-scattered radiation on the physical properties of the scatterers. Section 3 describes several methods to compute the effects of multiple scattering on the reflected light.     

离散光谱分辨率对喷流红外特性FVM计算的影响

建立了辐射传递方程(RTE)的有限元体积法(FVM)计算模型,研究了离散光谱分辨率对FVM计算精度的影响,提出了离散光谱分辨率无关解的概念,并编制了相应的FORTRAN源程序,结合大气飞行发动机标准算例进行了一系列计算和比较.结果表明;在给定的红外光谱域中,随着离散光谱的分辨率的提高,计算出的方向光谱辐射强度渐渐趋向于同一个值.在航空发动机喷流2～5μm红外光谱区间中,当划分150个以上等间隔光谱微元后,FVM可以保证达到离散光谱分辨率无关解.      

Principles of Invariance in Radiative Transfer

We have reviewed the principle of invariance, its applications and its usefulness for obtaining the radiation field in semi-infinite and finite atmospheres. Various laws of scattering in dispersive media and the consequent radiation field are studied. The H-functions and X- and Y-functions in semi-infinite and finite media respectively are derived in a few cases. The Discrete Space Theory (DST) which is a general form of the Principle of Invariance is described. The method of addition of layers with general properties, is shown to describe all the properties of multiple scattering. A few examples of the application of DST such as polarization, line formation in expanding stellar atmospheres, etc., and a numerical analysis of DST are presented. Other developments in the theory of radiative transfer are briefly described. This revised version was published online in June 2006 with corrections to the Cover Date.     

Element Settling in the Solar Interior

Element settling inside the Sun now becomes detectable from the comparison of the observed oscillation modes with the results of the theoretical models. This settling is due, not only to gravitation, but also to thermal diffusion and radiative acceleration (although this last effect is small compared to the two others). It leads to abundance variations of helium and heavy elements of ≅ 10% below the convective zone. Although not observable from spectroscopy, such variations lead to non-negligible modifications of the solar internal structure and evolution. Helioseismology is a powerful tool to detect such effects, and its positive results represent a great success for the theory of stellar evolution. Meanwhile, evidences are obtained that the element settling is slightly smoothed down, probably due to mild macroscopic motions below the convective zone. Additional observations of the abundances of both 7Li and 3He lead to specific constraints on these particular motions. This revised version was published online in June 2006 with corrections to the Cover Date.     

Molecular spectroscopy of planetary atmospheres

Summary Clearly spectroscopy has already provided considerable insight into the nature of the planetary atmospheres. Several molecular constituents have been positively identified and upper limits have been placed on the abundances of others which are of particular significance in devising planetary models. But, equally clearly, the inadequacy of the spectral data, due to low spectral and/or spatial resolution, renders deductions of abundances, temperatures and pressures very uncertain. With the sole exception of the Martian CO₂ abundance, knowledge of the concentrations of planetary atmospheric constituents is unsatisfactory, and all numbers given must be regarded as only crude estimates. This latter comment applies equally well to the derived temperatures and pressures.What is urgently needed is the development of a reasonably complete theory of line formation in planetary atmospheres. This, coupled with more detailed spectroscopic work, should produce numerical values of atmospheric parameters which can be used with assurance.This work was performed with the aid of NASA Grant NsG-101-61 with funds administered by the University of California.     

Hydrodynamic atmosphere models for hot luminous stars II. Method and improvements over unified models

In a paper submitted to A&A we present the first line blanketed hydrodynamic models of spherically expanding atmospheres of hot stars. This paper is complementary to the submitted paper. Here, we emphasize the advantages and the weak points of our approach and we present additional technical aspects.The models are characterised by a simultaneous solution of the equation of motion, the non-LTE populations of H and He, and radiation transfer in a line blanketed atmosphere. The entire domain from the optically thick photosphere out to the terminal velocity of the wind is treated. The radiative forces are evaluated consistently with the depth-dependent radiation field, taking into account multiple scattering by metal lines and line overlap.     

气壁镀镍和冷却剂入口对再生冷却的影响

考虑冷却剂入口模型及气壁镀镍,对液体火箭发动机推力室再生冷却通道和冷却剂进行三维流动与传热耦合计算.采用经验公式计算燃气侧对流及辐射换热,冷却剂为甲烷,考虑其物性随温度和压力的变化.所得结果表明:冷却剂入口二次流及突扩流场的叠加,使局部压力损失变大,影响进口下游较大区域流动传热状况;气壁镀镍能提高气壁的耐高温性,降低气壁锆铜的温度.      

Spectral analyses of Wolf-Rayet stars: Theory,results, conclusions

Stratified Non-LTE models for expanding atmospheres became available in the recent years. They are based on the idealizing assumptions of spherical symmetry, stationarity and radiative equilibrium. From a critical discussion we conclude that this standard model is basically adequate for describing real Wolf-Rayet atmospheres and hence can be applied for quantitative spectral analyses of their spectra.By means of these models, the fundamental parameters have been determined meanwhile for the majority of the known Galactic WR stars. Most of them populate a vertical strip in the Herzsprung-Russell diagram at effective temperatures of 35 kK, the luminosities ranging from 10^4.5 to 10^5.9 L . Only early-type WN stars with strong lines and WC stars are hotter. The chemical composition of WR atmospheres corresponds to nuclear-processed material (WN: hydrogen burning in the CNO cycle; WC: helium burning). Hydrogen is depleted but still detectable in the cooler part of the WN subclass.Different scenarios for the evolutionary formation of the Wolf-Rayet stars are discussed in the light of the empirical data provided from the spectral analyses. Post-red-supergiant evolution can principally explain the basic observational properties, except the rather low luminosities of a considerable fraction of WN stars. Among the alternative scenarios, close-binary evolution can theoretically produce the least-luminous WN stars. However, final conclusions about the evolutionary formation of the WR stars are not yet possible.