涡流管结构参数对其性能的影响

用实验方法研究了热端管管长、分离室直径、冷孔板孔径等主要结构参数对涡流管的制冷制热性能的影响。实验中以空气为介质分别对不同结构参数涡流管的性能进行了研究,得出了热端管管长、分离室直径以及冷孔板孔径等参数对涡流管制冷制热性能的影响规律。研究结果表明:在一定范围内增加热端管长度有利于涡流管的能量分离;在大冷流率下,大直径涡流管的制冷性能优于小直径涡流管;冷孔板孔径愈小,涡流管的制冷制热效应都愈好,在冷孔板孔径与热端管内径之比为50%时,取得最佳的制冷制热效应。      

添加剂含量对二硅化钼发热体抗氧化性能的影响研究

研究了添加剂含量对MoSi2发热体性能的影响,使用SEM观察各种添加剂含量试样的微观组织,测定各种添加剂含量试样的氧化动力学曲线、致密度、烧损温度。     

A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by IR-radiating molecules like CO₂, NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen and high Jeans’ escape rates for heavier species like H₂, He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO₂, N₂ and H₂O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian magnetosphere against solar wind induced ion pick up erosion. We find that the early martian magnetic field could decrease the ion-related non-thermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount of ∼250 bar of O⁺ ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial ocean (TO (1 TO ∼1.39×10²⁴ g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and compare our findings with the results of preceding studies.     

The Genesis Solar Wind Concentrator Target: Mass Fractionation Characterised by Neon Isotopes

The concentrator on Genesis provided samples of increased fluences of solar wind ions for precise determination of the oxygen isotopic composition. The concentration process caused mass fractionation as a function of the radial target position. This fractionation was measured using Ne released by UV laser ablation and compared with modelled Ne data, obtained from ion-trajectory simulations. Measured data show that the concentrator performed as expected and indicate a radially symmetric concentration process. Measured concentration factors are up to ∼30 at the target centre. The total range of isotopic fractionation along the target radius is 3.8%/amu, with monotonically decreasing ²⁰Ne/²²Ne towards the centre, which differs from model predictions. We discuss potential reasons and propose future attempts to overcome these disagreements.     

正庚烷液滴在微细直管中的燃烧特性实验

为了解微细直管对液滴形成和燃烧稳定性的影响,采用正庚烷作为燃料在内径为4mm的石英直管中的进行了实验研究.其结果显示:首先在不加热时,容易形成液滴,正庚烷体积流量小于40μL/min 时,火焰稳定性受液滴滴落的影响较大,液滴的蒸发主要受到空气体积流量影响下的火焰位置的影响;大于40μL/min时,液膜形成,火焰受液滴滴落影响不大.其次,管壁加热温度为180℃时,正庚烷体积流量低于60μL/min时难以形成液滴,大于60μL/min时液滴滴落后不形成液膜,液滴的蒸发受空气流速的影响较大,在液滴滴落以及空气流速的影响下,微燃烧器温度的变化对燃料的蒸发产生更大的影响,富燃较贫燃更易形成连续的火焰.空气流速大小对管壁温度影响明显,空气流速越小,管壁温度越高,液滴蒸发速率越大.      

高超声速复杂气动问题数值方法研究进展

高超声速流场具有复杂流动特征,其中真实气体效应、磁流体干扰效应和力热结构耦合效应等对气动力分析产生了重要影响。将流体力学研究扩展到分子动力学、电磁流体力学以及流固耦合等交叉学科领域,这给数值模拟方法带来了巨大挑战。针对高超声速气动力/热分析的热点问题,重点关注高温效应与低密度流动效应、磁流体干扰效应和力热结构耦合效应等,结合算例分析了相应的数值求解技术;在气动热方面主要比较了3类求解方法(纯工程方法、纯数值方法和基于Prandtl边界层理论的方法),并给出了相应算例;对于气动力/热/结构耦合问题,从耦合模型及耦合计算方法两方面开展了分析。最后指出了高超声速复杂气动问题数值求解技术未来需重点关注的几个方面。     

基于再入轨迹和气动热环境的返回舱烧蚀研究

针对再入全过程合理预测热防护罩表面材料烧蚀深度和温度的动态变化问题,提出融合再入轨迹、气动热以及Newton-Raphson和三对角矩阵算法（TDMA）构建动态烧蚀的方法。该方法建立直入式和跳跃式三自由度再入轨迹,应用修正的牛顿流体理论估算气动参数,以及修正的Fay-Riddell和Sutton-Grave理论计算驻点区域的热流密度,利用一维非线性热传导方程模拟了热防护材料的烧蚀过程。仿真结果表明：此方法实现了再入全过程热防护材料烧蚀深度和温度连续动态变化的预测,同样适用于更为复杂结构飞行器的动态烧蚀预测,与热平衡积分法（HBI）相比其结果可靠合理,为进一步优化热防护系统（TPS）提供了一定的参考依据。     

高超声速飞行器跨流域气动力／热预测技术研究

分析了跨流域流动特点、工程背景需求、国内外研究现状,针对高超声速飞行器跨流域气动力／热预测存在的主要问题,从粘性干扰参数与克努森数搭接的跨流域模拟准则、微量天平结构优化及测力技术、红外大面积中低量值热流测量技术、流场显示与测量技术和 N-S／DSMC 自适应紧耦合数值模拟方法等方面,总结了近年来取得的研究进展,并讨论了下一步研究方向。     

蓄热式太阳能热光伏-热推进双模系统换热特性数值模拟研究

本文通过三维数值模拟研究蓄热式太阳能热光伏-热推进双模系统的蓄/释热特性和推进性能。在蓄热式太阳能热推进系统工程模型的基础上,通过射线光学的光路分析验证了聚光器设计的合理性,并获得吸热腔壁面能量分布情况,进一步研究了相变蓄热过程的影响因素。基于场协同原理对热光伏再生冷却结构进行了优化设计,使热光伏具有较好的散热特性,提高发电功率;通过整机流动换热仿真,分析了工质流体在推进器内部的换热情况,计算结果表明,蓄热式热推进器具有达到734s比冲和0.9N推力的推进性能,以及能够满足日蚀区微小卫星的供电和推力需求。     

高超声速飞行器受热壁板的气动弹性声振分析

高超声速飞行器壁板在非定常气动力、热载荷和噪声载荷构成的多物理场联合作用下,将表现出复杂的非线性气动弹性声振响应,特别是在颤振临界动压附近,受热载荷以及声载荷作用,壁板表现出复杂的跳变运动。基于von Karman大变形板理论,建立了热-声载荷和气动力共同作用下的壁板运动方程,分析了超声速气流中受热壁板的屈曲变形及热屈曲稳定性,借助势阱概念初步分析了壁板跳变运动产生的机理。通过定义“穿零频次”给出了跳变运动定量的分类方法,并计算得到不同温升和动压情况下,壁板发生跳变运动所对应的临界声压级。结果表明：在颤振临界动压之前,随着动压的增加,受热壁板势阱的深度先增大后减小,且受热壁板的势阱深度随着温升的增加而增大。