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131.
本文研究了对于飞行器如何更加合理地定义其静稳定裕度的问题.常用的静稳定裕度定义为无量纲化的质心位置与气动焦点之间的距离,这种定义对于常见的高升阻比的飞机导弹等飞行器是适用的,然而对于一些非常规飞行器,例如载人飞船返回舱这类大钝头大配平攻角阻力体,这种定义在反映其静稳定程度上存在一定的问题.本文举例说明了这个定义存在缺陷,指出定义静稳定裕度时不能只考虑升力变化的影响,而是应该根据气动合力的变化来进行综合考虑.提出了新的比较完备的静稳定裕度定义方法,指出常用的静稳定裕度定义方法是本文提出的定义方法在特定情况下的表述,并举例说明了本文定义具有更加广泛的适用性. 相似文献
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应用于飞行器风洞试验的绳牵引并联机构技术综述 总被引:19,自引:3,他引:19
首先概述了法国航空局SACSO项目关于绳牵引并联机构应用于飞行器风洞试验的研究工作,然后从六自由度绳牵引并联机构的结构设计、运动学及性能分析、工作空间的分析与综合、静刚度分析、运动控制和力控制等六方面,详细分析了六自由度绳牵引并联机构应用于飞行器风洞试验中的关键技术。分析结果表明:六自由度绳牵引并联机构必须根据飞行器的类型,以工作空间大小为依据进行构型设计;其运动控制方案可借用PID控制或自适应控制,其优点是便于动力学模型的线性化和解耦;其力控制方案可借用经典的阻抗控制和力/位置混合控制,但适用于飞行器风洞试验的六自由度绳牵引并联机构的更完善的力控制策略还有待进一步的研究。 相似文献
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通过引入反映湍流涡粘性的湍流松弛,得到了模拟高雷诺数湍流的BGK方程.在速度相空间、物理空间和时间上对BGK方程进行离散得到了三维十九速离散速度模型;结合分区计算技术,设计了格子Boltzmann并行算法;根据亚格子Smagorinsky模型,提出了直接从粒子分布函数计算湍流松弛时间的方法.用开发的并行计算程序对分体双箱截面和闭口箱梁截面的静风荷载进行了数值识别,得到的静力三分力系数和流场压力分布与风洞试验结果及CFD宏观方法计算结果吻合,并从表面压力分布入手分析了两种桥梁截面的绕流特点. 相似文献
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Yuri N. Kulikov Helmut Lammer Herbert I. M. Lichtenegger Thomas Penz Doris Breuer Tilman Spohn Rickard Lundin Helfried K. Biernat 《Space Science Reviews》2007,129(1-3):207-243
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. 相似文献
139.
V. S. Heber R. C. Wiens D. B. Reisenfeld J. H. Allton H. Baur D. S. Burnett C. T. Olinger U. Wiechert R. Wieler 《Space Science Reviews》2007,130(1-4):309-316
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. 相似文献
140.
H. J. Völk 《Space Science Reviews》2007,130(1-4):431-438
The dynamical and chemical effects of the Galactic Wind are discussed. This wind is primarily driven by the pressure gradient
of the Cosmic Rays. Assuming the latter to be accelerated in the Supernova Remnants of the disk which at the same time produce
the Hot Interstellar Medium, it is argued that the gas removed by the wind is enriched in the nucleosynthesis products of
Supernova explosions. Therefore the moderate mass loss through this wind should still be able to remove a substantial amount
of metals, opening the way for stars to produce more metals than observed in the disk, by e.g. assuming a Salpeter-type stellar
initial mass function beyond a few Solar masses. The wind also allows a global, physically appealing interpretation of Cosmic
Ray propagation and escape from the Galaxy. In addition the spiral structure of the disk induces periodic pressure waves in
the expanding wind that become a sawtooth shock wave train at large distances which can re-accelerate “knee” particles coming
from the disk sources. This new Galactic Cosmic Ray component can reach energies of a few×1018 eV and may contribute to the juncture between the particles of Galactic and extragalactic origin in the observed overall
Cosmic Ray spectrum. 相似文献