排序方式: 共有60条查询结果,搜索用时 15 毫秒
11.
12.
袁海根%曾金芳%杨杰 《宇航材料工艺》2006,36(Z1):1-6
回顾了液晶聚合物和分子复合材料的发展历史,介绍了溶致型和热致型液晶聚合物分子复合材料及其常用制备方法,简述了原位复合材料的增强机理、界面相容性、影响液晶聚合物成纤的因素以及分子复合材料深入发展的相关问题. 相似文献
13.
针对二维叶片整体造型优化问题,提出一种基于边界涡量流的二维叶型优化模型,并对该模型进行求解。建立以含参数的Bezier曲线定义的二维叶型型线为边界、以边界涡量流正峰值的最小化为目标函数的优化模型,通过分析边界涡量流的生成机制,把叶型型线边界信息代入边界涡量流中,将边界涡量流用叶型型线参数和型线上的气动参数表示,进而获得新的目标函数表达式。该目标函数表达式可直接对叶型型线参数求导,仅使用简单的定步长梯度算法即可对优化模型求解。结果表明:优化后的叶型型线上的边界涡量流的正峰值显著降低。 相似文献
14.
15.
Gianfranco Vidali Ling Li Joseph E. Roser Ryan Badman 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
Silicates constitute an important class of interstellar grain material and are the site of catalytic activities, most notably the formation of molecular hydrogen. Here we report an analysis of experiments conducted in the laboratory to measure the efficiency of formation of molecular hydrogen on amorphous silicates, a realistic analogue of interstellar dust grains. From the measurements, we also obtain the energetics of key processes in the reaction and information on the mechanism of reaction. Comparison with earlier measurements of molecular hydrogen formation on a sample of polycrystalline olivine shows that amorphous materials are more efficient catalysts. 相似文献
16.
The mixing and combustion process has an important impact on the engineering realization of the scramjet engine. The nonreacting and reacting flow fields in a transverse injection channel have been investigated numerically, and the predicted results have been compared with the available experimental data in the open literature, the wall pressure distributions, the separation length, as well as the penetration height. Further, the influences of the molecular weight of the fuel and the jet-to-crossflow pressure ratio on the wall pressure distribution have been studied. The obtained results show that the predicted results show reasonable agreement with the experimental data, and the variable trends of the penetration height and the separation distance are almost the same as those obtained in the experiment. The vapor pressure model is suitable to fit the relationship between the penetration height, the separation distance and the jet-to-crossflow pressure ratio. The combustion process mainly occurs upstream of the injection port, and it makes a great difference to the wall pressure distribution upstream of the injection port, especially when the jet-to-crossflow pressure ratio is large enough, namely 17.72 and 25.15 in the range considered in the current study. For hydrogen, the combustion downstream of the injection port occurs more intensively, and this may be induced by its smaller molecular weight. 相似文献
17.
Aimed at the computational aeroacoustics multi-scale problem of complex configurations discretized with multi-size mesh, the flux reconstruction method based on modified Weight Essentially Non-Oscillatory (WENO) scheme is proposed at the interfaces of multi-block grids. With the idea of Dispersion-Relation-Preserving (DRP) scheme, different weight coefficients are obtained by optimization, so that it is in WENO schemes with various characteristics of dispersion and dissipation. On the basis, hybrid flux vector splitting method is utilized to intelligently judge the amplitude of the gap between grid interfaces. After the simulation and analysis of 1D convection equation with different initial conditions, modified WENO scheme is proved to be able to independently distinguish the gap amplitude and generate corresponding dissipation according to the grid resolution. Using the idea of flux reconstruction at grid interfaces, modified WENO scheme with increasing dissipation is applied at grid points, while DRP scheme with low dispersion and dissipation is applied at the inner part of grids. Moreover, Gauss impulse spread and periodic point sound source flow among three cylinders with multi-scale grids are carried out. The results show that the flux reconstruction method at grid interfaces is capable of dealing with Computational AeroAcoustics (CAA) multi-scale problems. 相似文献
18.
Surface temperature and the available effective energy strongly influence the mass flux of H2O and minor volatiles from the nucleus. We perform computer simulations to model the gas flux from volatile, icy components
in porous ice-dust surfaces, in order to better understand results from observations of comets. Our model assumes a porous
body containing dust, one major ice component (H2O) and up to eight minor components of higher volatility (e.g. CO, CH4, CH3OH, HCN, C2H2, H2S), The body's porous structure is modeled as a bundle of tubes with a given tortuosity and an initially constant pore diameter.
Heat is conducted by the matrix and carried by the vapors. The model includes radially inward and outward flowing vapor within
the body, escape of outward flowing gas from the body, complete depletion of less volatile ices in outer layers, and recondensation
of vapor in deeper, cooler layers. From the calculations we obtain temperature profiles and changes in relative chemical abundances,
porosity and pore size distribution as a function of depth, and the gas flux into the interior and into the atmosphere for
each of the volatiles at various positions of the body in its orbit.
In this paper we relate the observed relative molecular abundances in the coma of Comet C/1995 O1 (Hale-Bopp) and of Comet
46P/Wirtanen to molecular fluxes at the surface calculated from our model.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
19.
H.Y. Wei C.T. Russell M.K. Dougherty Y.J. Ma K.C. Hansen H.J. McAndrews A. Wellbrock A.J. Coates M.F. Thomsen D.T. Young 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
Observations of unusually large magnetic fields in the ionosphere indicate periods of maximum stress on Titan’s ionosphere and potentially of the strongest loss rates of ionospheric plasma. During Titan flyby T42, the observed magnetic field attained a maximum value of 37 nT between an altitude of 1200 and 1600 km, about 20 nT stronger than on any other Titan pass and close to five times greater in magnetic pressure. The strong fields occurred near the corotation-flow terminator rather than at the sub-flow point, suggesting that the flow which magnetized the ionosphere was from a direction far from corotation and possibly towards Saturn. Extrapolation of solar wind plasma conditions from Earth to Saturn using the University of Michigan MHD code predicts an enhanced solar wind dynamic pressure at Saturn close to this time. Cassini’s earlier exits from Saturn’s magnetosphere support this prediction because the Cassini Plasma Spectrometer instrument saw a magnetopause crossing three hours before the strong field observation. Thus it appears that Titan’s ionosphere was magnetized when the enhanced solar wind dynamic pressure compressed the Saturnian magnetosphere, and perhaps the magnetosheath magnetic field, against Titan. The solar wind pressure then decreased, leaving a strong fossil field in the ionosphere. When observed, this strong magnetic flux tube had begun to twist, further enhancing its strength. 相似文献
20.
《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2023,71(1):275-285
There are hundreds of satellites operating at the geosynchronous (GEO) orbit where relativistic electrons can cause severe damage. Thus, predicting relativistic electron fluxes is significant for spacecraft safety. In this study, using GOES satellite data during 2011–2020, we propose two neural network models with two hidden layers to predict geosynchronous relativistic electron fluxes at two energy channels (>0.8 MeV and > 2 MeV). The number of input neurons of the two channels (>0.8 MeV and > 2 MeV) are determined to be 36 and 44, respectively. The > 0.8 MeV model has 22 and 9 neurons in the hidden layers, while the > 2 MeV model has 25 and 15 neurons in the hidden layers. The input parameters include the north–south component of the interplanetary magnetic field, solar wind speed, solar wind dynamic pressure and solar wind proton density. Through the analysis of different time delays, we determine that the optimal time delays of two energy channels (>0.8 MeV and > 2 MeV) are 8 days and 10 days, respectively. The training set and validation set (Jan 2011-Dec 2018) are divided by the 10-fold cross-validation method, and the remaining data (Jan 2019-Feb 2020) is used to analyze the model performance as a test set. The prediction results of both energy channels show good agreement with satellite observations indicated by low RMSE (~0.3 cm-2sr-1s?1), high PE (~0.8) and CC (~0.9). These results suggest that only using solar wind parameters is capable of obtaining reasonable predictions of geosynchronous relativistic electron fluxes. 相似文献