固体火箭冲压发动机导弹一体化遗传算法优化设计

遗传算法能以很高的概率找到全局最优解，适合工程优化设计要求。研究以固体火箭冲压发动机为动力的导弹的冲仑方案设计，探讨采用遗传算法实现冲压发动机导弹一体化优化设计，给出满足战术技术指标的最优总体方案和冲压发动机方案。算例表明，遗传算法是用于固体火箭冲压发动机导弹一体化优化设计的很好的优化算法，通过一体化优化设计，可以提高冲压发动机和导弹的总体性能。     

二维实验固体燃料冲压发动机冷流数值分析

本文在冷流情况下，对已初步完成设计的二维实验ＳＦＲＪ建立了数学模型并进行了数值解，得出了一些有用的结构，对ＳＦＲＪ的精确设计和实验数据提供了有用的理论研究基础。     

中心进气旋转射流冲压燃烧室湍流流动数值模拟

采用Reynolds应力方程模型及涡耗散燃烧模型,对头部进气式固体火箭冲压发动机二次燃烧二维轴对称反应流场进行了数值模拟,研究了空气射流和燃气射流无旋、同向旋转和反向旋转3种进气方式对二次燃烧的影响。研究结果表明,当空气射流和燃气射流以有旋状态进入补燃室时,燃料与空气的混合速度变快,化学反应更快,燃烧也更为充分。     

金属/水反应冲压发动机进水管路的工作特性

基于水与金属燃料反应的水冲压发动机是一种新型的水下动力装置。进水管路是金属/水反应冲压发动机的一个重要部件。为了研究进水管路的工作特性,在理论分析和一维设计的基础上,设计出某一工作状态下的进水管路结构参数,并进行了数值模拟。结果表明,管路中出现汽蚀现象;随着出口压强的增大,总压损失减小,流量系数减小;随着来流速度的增大,总压损失增大,流量系数先增大后减小;随着工作深度的增加,总压损失增大,流量系数增大。     

压缩空气瓶内凝结水水位检测方法的探讨

由于压缩空气瓶在使用过程中会出现瓶内残留凝结水的现象,从而影响压缩空气瓶的容积,并产生化学腐蚀,影响气瓶的整体强度和耐压性能及其的寿命。为此,应掌握气瓶内凝结水水位情况,并且提高检测水位准确度。提出了一种利用气体状态方程来计算压缩空气瓶的冷凝水水位新见解,对压缩空气瓶的安全使用具有重要意义。     

固体燃料冲压发动机自持燃烧的影响因素

采用试验和仿真方法,研究了固体燃料冲压发动机(SFRJ)自持燃烧的主要影响因素。研究结果表明:SFRJ内为典型的扩散火焰,化学反应特征时间与反应物停留特征时间的比值是影响发动机自持燃烧的关键参数,该值越小,扩散火焰越稳定;本文研究工况下,较小的后台阶高度即可保证发动机实现自持燃烧,后台阶稳定火焰的物理原因是在固体燃料表面附近形成一个低速区,保证了固体燃料的分解燃烧,当台阶高度为0时,由于化学反应特征时间与反应物停留特征时间的比值迅速增加,SFRJ无法自持燃烧;台阶高度较小时,点火过程会对SFRJ的稳定燃烧产生影响,SFRJ可能会出现熄火复燃现象。     

Kinetics of gas-Grain Reactions in the Solar Nebula

Thermochemical equilibrium calculations predict gas phase, gas-grain, and solid phase reactions as a function of pressure and temperature in the solar nebula. However, chemical reactions proceed at different rates, which generally decrease exponentially with decreasing temperature. At sufficiently low temperatures (which vary depending on the specific reaction) there may not have been enough time for the predicted equilibrium chemistry to have taken place before the local environment cooled significantly or before the gaseous solar nebula was dispersed. As a consequence, some of the high temperature chemistry established in sufficiently hot regions of the solar nebula may be quenched or frozen in without the production of predicted low temperature phases. Experimental studies and theoretical models of three exemplary low temperature reactions, the formation of troilite (FeS), magnetite (Fe₃O₄), and hydrous silicates, have been done to quantify these ideas. A comparison of the chemical reaction rates with the estimated nebular lifetime of 0.1-10 million years indicates that troilite formation proceeded to completion in the solar nebula. Magnetite formation was much slower and only thin magnetite rims could have formed on metal grains. Hydrous silicate formation is predicted to be even slower, and hydrous silicates in meteorites and interplanetary dust particles probably formed later on the parent bodies of these objects, instead of in the solar nebula. This revised version was published online in June 2006 with corrections to the Cover Date.     

An assessment of semi-analytical models based on the absorption coefficient in retrieving the chlorophyll-a concentration from a reservoir

Monitoring chlorophyll-a (Chl-a) concentrations in inland waters is crucial for water quality management, since Chl-a is a proxy for phytoplankton biomass and, thus, for ecological health of a water environment. Chl-a concentration can be retrieved through the inherent optical properties (IOPs) of a water system, which, in turn, can be remotely sensed obtained. Quasi-analytical algorithm (QAA), originally developed for ocean waters, can also retrieve IOPs for inland waters after re-parameterizations. This study is aimed at assessing the performance of sixteen schemes composed by QAA original and re-parameterized versions followed by models that use absorption coefficients as inputs for estimating Chl-a concentration in Ibitinga reservoir, located at Tietê River cascading system, São Paulo State, Brazil. It was verified that only QAA_V5 based schemes were able to obtain reasonable estimates for image data and that by four models tested presented similar and acceptable results for QAA_V5 outputs. The best model were applied to a Ocean and Land Colour Instrument (OLCI) image. Light absorption in the reservoir showed to be dominated by colored dissolved organic matter (CDOM), and wide spatial and temporal variability of optical and water quality properties was observed.     

Fronts and thermohaline structure of the Brazil–Malvinas Confluence System

Fronts and thermohaline structure of the Brazil–Malvinas Confluence System (BMCS) are studied from climatic data, “Marathon Exp. Leg.8, 1984” data, and Sea surface temperature (SST) data base “ds277-Reynolds” (1981–2000). The South Atlantic Central Water (SACW) is divided in two main types: tropical (TW) and subtropical water (ST). Water masses, Fronts, Inter-Frontal and Frontal Zones are analysed and classified: (a) the water masses: Tropical Low-Salinity Water, Tropical Surface Water, Tropical Tropospheric Water, Subtropical Low-Salinity Water, Subtropical Surface Water, Subtropical Tropospheric Water. T,S characteristics of intermediate, deep and bottom water defined by different authors are confirmed and completed; (b) the Inter-Frontal Zones: Tropical/Brazil Current Zone, Subtropical Zone and Subantarctic Zone; (c) the Frontal Zones: Subtropical, Subantarctic and Polar, and (d) the Fronts: Subtropical Front of the Brazil Current, Principal Subtropical Front, North Subtropical Front, Subtropical Surface Front, South Subtropical Front, Subantarctic Surface Front, Subantarctic Front and Polar Front. Several stable T–S relationships are found below the friction layer and at the Fronts. The maximum gradient of the oceanographic characteristics occurs at the Brazil Current Front, which can be any of the subtropical Fronts, depending on season. Minimum mean depth of the pycnocline coincides with the Fronts of the BMCS, indicating the paths of low-salinity shelf waters into the open ocean. In the work it is shown how to recover the horizontal and vertical thermohaline structure of waters from satellite data RSMAS SST.     

Cometary Deuterium

Deuterium fractionations in cometary ices provide important clues to the origin and evolution of comets. Mass spectrometers aboard spaceprobe Giotto revealed the first accurate D/H ratios in the water of Comet 1P/Halley. Ground-based observations of HDO in Comets C/1996 B2 (Hyakutake) and C/1995 O1 (Hale-Bopp), the detection of DCN in Comet Hale-Bopp, and upper limits for several other D-bearing molecules complement our limited sample of D/H measurements. On the basis of this data set all Oort cloud comets seem to exhibit a similar ratio in H₂O, enriched by about a factor of two relative to terrestrial water and approximately one order of magnitude relative to the protosolar value. Oort cloud comets, and by inference also classical short-period comets derived from the Kuiper Belt cannot be the only source for the Earth's oceans. The cometary O/C ratio and dynamical reasons make it difficult to defend an early influx of icy planetesimals from the Jupiter zone to the early Earth. D/H measurements of OH groups in phyllosilicate rich meteorites suggest a mixture of cometary water and water adsorbed from the nebula by the rocky grains that formed the bulk of the Earth may be responsible for the terrestrial D/H. The D/H ratio in cometary HCN is 7 times higher than the value in cometary H₂O. Species-dependent D-fractionations occur at low temperatures and low gas densities via ion-molecule or grain-surface reactions and cannot be explained by a pure solar nebula chemistry. It is plausible that cometary volatiles preserved the interstellar D fractionation. The observed D abundances set a lower limit to the formation temperature of (30 ± 10) K. Similar numbers can be derived from the ortho-to-para ratio in cometary water, from the absence of neon in cometary ices and the presence of S₂. Noble gases on Earth and Mars, and the relative abundance of cometary hydrocarbons place the comet formation temperature near 50 K. So far all cometary D/H measurements refer to bulk compositions, and it is conceivable that significant departures from the mean value could occur at the grain-size level. Strong isotope effects as a result of coma chemistry can be excluded for molecules H₂O and HCN. A comparison of the cometary ratio with values found in the atmospheres of the outer planets is consistent with the long-held idea that the gas planets formed around icy cores with a high cometary D/H ratio and subsequently accumulated significant amounts of H₂ from the solar nebula with a low protosolar D/H. This revised version was published online in June 2006 with corrections to the Cover Date.