高超声速热化学非平衡对气动热环境影响

高超声速气动加热严重,考虑热化学非平衡对气动热环境影响,可以为热防护系统设计提供有效保障。采用Park和Gupta热化学非平衡模型,数值计算研究5组元(N_2,O_2,N,O,NO),17组化学反应的热化学非平衡效应对高超声速飞行器气动热环境影响,并与完全气体和热化学平衡模型进行对比分析。热化学非平衡模型流场温度及激波距离均比完全气体模型小。激波后气体密度因离解、化学反应而增大,且气体密度越大,激波距离越小,热化学平衡模型激波距离最小。完全气体和热化学平衡模型热流载荷计算值均比实验值偏大。Park和Gupta热化学非平衡模型数值计算激波距离及气动力载荷差别小。Park模型热流载荷计算值偏大,Gupta模型与实验结果相符,它可对气动热环境可靠预测。     

激发跃迁速率对热力学非平衡氮气紫外辐射的影响

基于氮气的碰撞-辐射（CR）模型,计算了速度为6.2 km/s、初始压力为133 Pa的高超声速流动激波中N₂和N₂+分子电子能级的分布情况,分析了不同激发跃迁速率模型对电子能级分布及辐射光谱模拟的影响。针对流动中热力学非平衡区域和平衡区域,在300~440 nm的辐射光谱开展了逐线法的数值模拟,并与激波管实验测量光谱进行了对比。结果表明,目前的激发跃迁速率均存在偏差,综合Park模型的爱因斯坦系数和Johnston模型的碰撞激发速率可以得到与实验结果最为接近的辐射光谱。      

高超声速热流计算湍流模型性能评估

采用计算流体力学方法,通过对高超声速来流下双椭球热流计算,综合分析了影响壁面热流预测精度的因素.针对工程上4种常用的湍流模型:BL(Baldwin-Lomax)模型、SA(Spalart-Allmaras)模型、k-ω模型及SST(Shear-Stress Transport)模型,评估了其在高超声速热流预测中的性能,获得了湍流模型下壁面法向网格雷诺数对热流计算的影响规律.此外,对高马赫数下不同后掠角钝舵模型进行热流计算,获得了后掠角对钝舵前缘热流峰值的影响规律.研究表明,两方程湍流模型相比一方程和零方程模型更适合高超声速气动热计算,其中SST模型对热流预测精度更高,总体性能更为优异;钝舵驻点线最大热流随后掠角增大呈非单调变化,在后掠角约为22°时热流达到峰值.      

高超声速三维化学非平衡流动的数值模拟

高温非平衡化学反应对高超声速再入飞行器绕流流场的气动热特性有较大影响.通过采用有限体积NND(Non-oscillatory, containing No free parameters and Dissipative scheme)格式求解三维N-S方程,分别计算了小攻角条件下球锥的完全气体粘性流场和化学反应非平衡气体流场.比较并分析了化学非平衡作用对三维高超声速钝头体绕流流场的影响.所得结果与国外文献结果符合的较好,证明了计算方法与程序的有效性和实用性.      

发动机燃气喷流红外辐射场的数值模拟

在高温流动中热辐射与流场是耦合的,但在发动机燃气喷流流场的温度范围内可以在流场计算中忽略热辐射的影响,于是流场与辐射场的模型方程可解耦.为此提出了模拟飞行器绕流流场红外辐射的解耦模型以及相应的算法.该算法首先采用总变差减小TVD(Total Variation Diminishing)格式对流场进行模拟,再引入有限体积概念,应用所取得的流场参数,在同一组网格上计算流场中的红外辐射特征.以轴对称喷管内N₂,O₂,CO₂,H₂O,CO,HCl,H₂等7组分高度欠膨胀冻结流与均匀绕流干扰流场为算例进行了验证性的模拟计算,并与已有试验和计算数据进行了对比,表明该算法是可靠的,可在较大幅度地降低计算量的情况下给出满足工程需要的结果.     

飞行器进入火星大气的流场预测

针对火星着陆探测器进入-下降-着陆过程的高超声速进入阶段, 利用三维并 行程序求解流体动力学Navier-Stokes方程与化学反应动力学模型, 分析火星 科学实验室进入火星大气时探测器周围的流场结构、化学非平衡效应影响和气 动特性变化规律. 结果表明, 对于完全气体模型, 来流的热力学性质参数选 取影响激波位置和强度. 在化学非平衡效应影响下, 探测器头部激波脱体距离 大幅减小, 驻点压力变化不大, 波后温度显著降低. CO₂在激波后大量分解, 消耗相当能量. 流线结构显示, 探测器尾迹流动中存在复杂的旋涡运动等流动 分离现象.      

高温化学非平衡计算中源项处理方法

高超声速三维化学非平衡绕流流场的数值模拟中,在计算初期容易发生组元密度出现负值的非物理现象,另外源项的刚性是影响计算稳定性和收敛速度的主要原因。根据源项线性化理论,采用2种源项线性化方法处理化学反应源项.一种为根据流场内化学反应物理规律构造的线性化方法,该方法能抑制在计算过程中组元密度出现负值现象,提高了计算稳定性,加速了收敛速度.同时采用了时间预处理矩阵的线性化方法,较好地解决了非平衡化学反应与流场耦合的刚性问题。证明了所构造源项线性化方法相容性.数值实验表明该方法有效地避免了源项计算中密度出负的问题,加快了计算的收敛速度,从而提高了计算效率.      

限制器对高超声速体表面热流数值模拟的影响

采用Roe的FDS（Flux Difference Splitting）差分格式结合min mod,van Leer和Osher-C限制器,对高超声速体外部流场进行数值模拟.研究了限制器对高超声速体气动力/热数值模拟的区别,对比分析了3种限制器对三维模型表面热流数值模拟结果的影响.研究表明,限制器对数值模拟精度有重要影响,且对气动热数值模拟的影响大于对气动力的影响;对简单或较复杂的气动外形,采用Roe的FDS格式结合min mod限制器获得的表面热特性比它结合van Leer和Osher-C限制器时要好,可为热防护设计提供可靠结果.      

离解反应速率常数中的方位因素

以碰撞理论为基础探讨了结构方位因素对离解反应速率常数的影响,建立了计及方位特征的离解反应模型,计算对比了热平衡假设下空气中几个典型的离解反应的Arrhenius图.结果表明,在所选实例中,除了反应N₂+N和O₂+O外,考虑方位因素后确实能够更好地理论估算出反应速率常数.对上述例外文中做了一定的讨论.     

Polar/TIMAS statistical results on the outflow of molecular ions from earth at solar minimum

Ion composition data from the first 22 months of operation of the Polar/TIMAS instrument, covering the 15-eV/e to 33-keV/e energy range, have been surveyed to determine the typical abundance, at solar minimum, of N₂⁺, NO⁺ and O₂⁺ ions in the auroral ion outflow, as compared to that of the better known O⁺ ions. The results indicate that molecular ions have roughly the same energy distribution as the O⁺ ions, with maximum differential flux occurring below 400 eV, but are far less abundant, by two orders of magnitude. The molecular ions also differ from the O⁺ ions in that they seem more specifically associated with enhanced geomagnetic activity.     

火星大气模型参数对MSL气动特性的影响

火星大气与地球大气截然不同,飞行器在进入火星时气动特性不同于地球再入. 大气模型的差异主要表现为气体组份、密度和温度等物理参数. 针对火星进入器MSL在进入-下降-着陆过程中的高超声速进入段,利用三维并行程序求解耦合真实气体模型的流体动力学Navier-Stokes方程,分析MSL进入火星大气时大气模型参数对进入器气动特性的影响. 结果表明,通过与海盗号飞行数据的对比,验证了所采用的火星气体模型和计算方法,且其与NASA的 LAURA代码气动特性计算结果也较为一致;大气模型气体性质,即CO₂环境对进入器阻力系数和俯仰力矩系数影响较大,利用空气得到的计算和实验数据必须考虑CO₂效应;密度增大促进了化学非平衡效应,但对进入器气动特性基本没有影响;温度升高大大增强了化学非平衡效应,而对进入器气动特性影响较小.      

The search for nitrogen compounds on the surface of Mars

Nitrogen is an essential element for life. Specifically, “fixed nitrogen” (i.e., NH₃, NH₄⁺, NO_x, or N that is chemically bound to either inorganic or organic molecules and is releasable by hydrolysis to NH₃ or NH₄⁺) is the form of nitrogen useful to living organisms. To date no direct analysis of Martian soil nitrogen content, or content of fixed nitrogen compounds has been done. Consequently, the planet's total inventory of nitrogen is unknown. What is known is that the N₂ content of the present-day Martian atmosphere is 0.2 mbar. It has been hypothesized that early in Mars' history (3 to 4 billion years ago) the Martian atmosphere contained much more N₂ than it does today. The values of N₂ proposed for this early Martian atmosphere, however, are not well constrained and range from 3 to 300 mbar of N₂. If the early atmosphere of Mars did contain much more N₂ than it does today the question to be answered is, Where did it go? The two main processes that could have removed it rapidly from the atmosphere include: 1) nonthermal escape of N-atoms to space; and 2) burial within the regolith as nitrates and nitrites. Nitrate will be stable in the highly oxidized surface soil of Mars, and will tend to accumulate in the soil. Such accumulations are observed in certain desert environments on Earth. Some NH₄⁺---N may also be fixed and stabilized in the soil by inclusion as a structural cation in the crystal lattices of certain phyllosilicates replacing K. Analysis of the Martian soil for traces of NO₃⁻ and NH₄⁺ during future missions will supply important information regarding the nitrogen abundance on Mars, its past climate as well as its potential for the evolution of life.     

Comparison of ion composition from the goddard comprehensive ionosphere database with the international reference ionosphere model

We compared the IRI values of T_e, N_e, T_i, O⁺, H⁺, He⁺, O₂₊, and NO⁺ with AE-C values, obtained from the Goddard Comprehensive Ionosphere Database (GCID), composed of data from the satellites, AE-B, OGO-6, ISIS-2, AE-C, AE-D, and AE-E. O⁺ - H⁺ transition levels were derived from the IRI and AE-C altitude profiles. Some discrepancies were found between IRI and the AE-C data. The IRI electron density was found to be about a factor of 2 higher than the data. The H⁺ composition agreed best among the IRI ions, with an average AE-C/IRI ratio of 1.05. The temperatures of both electrons and ions agreed quite well: the average ratios of AE-C/IRI was found to be .99 for electrons and 1.17 for ions.     

提高k-ωSST模型对翼型失速特性的模拟能力

采用CFD软件fluent,k-ω SST模型对S825翼型进行了二维数值模拟.针对k-ω SST模型对翼型分离失速特性模拟不准的情况,对分离区域内湍流的强非平衡输运特性进行了分析.研究表明:原始模型由于不能准确模拟分离区内湍流的强非平衡输运特性,导致其对翼型失速特性模拟失效;提出了通过修正模型系数a₁及β_∞^*,提高k-ω SST模型预测非平衡湍流输运特性的方法,从而提高对翼型失速特性的模拟精度.     

受控生态生保系统内红萍供氧特性研究

研究红萍载人供O₂特征, 为红萍生物部件进行系统总体地面模拟试验及空间应用奠定基础,构建了受控生态生保系统密闭试验舱和红萍栽培装置, 在“红萍-鱼-人”共存情况下, 测定密闭舱内O₂, CO₂浓度的变化. 试验结果显示, 单位重量的鱼耗O₂量. 0805～0.0831 L·kg-1·h-1, 排放CO₂量为0.0705～0.0736 L·kg-1·h-1; 试验志愿者耗O₂量19.71 L·h-1, 呼吸释放CO₂量18.90 L·h-1. 人工光照保持7000～8000 lx条件下, 红萍的光合作用与人和鱼的呼吸作用相辅相成, 舱内O₂, CO₂浓度趋于平衡. 密闭舱内CO₂浓度升高对促进红萍群体净光合效率有明显效果, 红萍光合放O₂能力很强, 能有效促使密闭舱内O₂, CO₂浓度朝着有利于人生存的环境方向平衡, 进而验证了红萍的空间应用前景.      

On the possible detection of solid O2 and O3 interstellar grains with ISO

In various models of interstellar grain chemistry, solid O₂ is formed by accretion as well as by surface reactions on grains. In dense molecular cloud models, at a later stage of the evolution, the O₂ molecule may become a substantial grain mantle constituent. Since IR dipole vibrational transitions for the homonuclear diatomic molecule O₂ are forbidden, the abundance of this potentially important grain mantle component can not be determined. However, embedded in a dirty ice matrix, the fundamental vibration of O₂ at 1550 cm⁻¹ becomes observable at 10 K, due to interactions with surrounding molecules, which break the symmetry of molecular oxygen. This process might be applicable for the dust mantle environment of interstellar grains. We have studied the role of solid O₂ and O₃ in astrophysically relevant ice mixtures and discuss the possible detection of solid O₂ and its major photolysis product O₃ in interstellar grains, in dense molecular clouds. Both molecules represent a specific target to be observed by the ISO satellite in the near future.