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151.
David P. O’Brien Andre Izidoro Seth A. Jacobson Sean N. Raymond David C. Rubie 《Space Science Reviews》2018,214(1):47
The planetary building blocks that formed in the terrestrial planet region were likely very dry, yet water is comparatively abundant on Earth. Here we review the various mechanisms proposed for the origin of water on the terrestrial planets. Various in-situ mechanisms have been suggested, which allow for the incorporation of water into the local planetesimals in the terrestrial planet region or into the planets themselves from local sources, although all of those mechanisms have difficulties. Comets have also been proposed as a source, although there may be problems fitting isotopic constraints, and the delivery efficiency is very low, such that it may be difficult to deliver even a single Earth ocean of water this way. The most promising route for water delivery is the accretion of material from beyond the snow line, similar to carbonaceous chondrites, that is scattered into the terrestrial planet region as the planets are growing. Two main scenarios are discussed in detail. First is the classical scenario in which the giant planets begin roughly in their final locations and the disk of planetesimals and embryos in the terrestrial planet region extends all the way into the outer asteroid belt region. Second is the Grand Tack scenario, where early inward and outward migration of the giant planets implants material from beyond the snow line into the asteroid belt and terrestrial planet region, where it can be accreted by the growing planets. Sufficient water is delivered to the terrestrial planets in both scenarios. While the Grand Tack scenario provides a better fit to most constraints, namely the small mass of Mars, planets may form too fast in the nominal case discussed here. This discrepancy may be reduced as a wider range of initial conditions is explored. Finally, we discuss several more recent models that may have important implications for water delivery to the terrestrial planets. 相似文献
152.
90°强曲率弯管内三维湍流流场的数值分析 总被引:1,自引:0,他引:1
本文根据作者发展的一种能计算任意截面形状 90°弯管内三维不可压缩湍流流场的分析方法,利用作者实验的圆截面弯管数据 ( Rc/D=0.87)检验 k- ε双方程湍流模型预示强曲率三维湍流流场的精度。计算了 Rc/D=2.3的矩形截面和 Rc/D=0.87的圆截面 90°弯管,并将计算结果与相应实验数据进行了比较分析。结果表明,即使对曲率很强的弯管,吸力面 (内侧壁 )不出现二次流迁移所形成的低速区前,标准 k- ε双方程模型仍能较好地预示出平均速度场。 相似文献
153.
首先根据载人航天器轨道运行段的基本特征,利用球面三角公式推导了:①阳光方向与载人航天器太阳能帆板法向的最佳夹角公式;②圆轨道的受晒因子公式。然后根据理论分析,引入帆板的效率系数。最后借助于计算机代数mathematica系统,建立了一种分析帆板最佳受晒的直观、清晰、简便的方法。所得的结论为确定载人航天器的发射窗口提供了依据。 相似文献
154.
155.
飞机构型控制技术初探 总被引:3,自引:2,他引:3
为了对现代飞机制造业中存在的复杂飞机构型进行有效地管理,解决产品数据管理中所遇到的构型控制难题,分析了现代飞机制造的特点以及对当今飞机制造业提出的问题,强调了构型控制技术的重要性.在明确了构型控制技术一些主要相关概念的基础上,借鉴波音公司实施构型控制技术的经验,针对中国飞机制造业的现状和未来发展,指出了飞机构型控制技术的4个关键内容,阐明了为实现飞机构型控制技术目前应开展的工作. 相似文献
156.
S.?N.?Grigor’ev V.?A.?DolgovEmail author A.?V.?Krasnov A.?A.?Kabanov N.?S.?Andreev 《Russian Aeronautics (Iz VUZ)》2015,58(2):244-250
A method of technologic audit for technical re-equipment of enterprises is considered. The method developed is intended to verify technological solutions of projects of technical re-equipment of enterprises according to indicators of productivity. 相似文献
157.
卫星通信与卫星定位系统的应用发展,对终端设备天线的性能提出了更高的应用需求。为实现宽频带宽波束圆极化天线的设计,采用正交移相馈电网络对含有背腔的交叉偶极子天线馈电,实现了宽带圆极化单向辐射特性,同时利用磁电偶极子对交叉偶极子进行加载,展宽了天线的波束宽度,促使天线在50.7%的相对带宽内S11<-10dB,在1.3~1.75GHz的频带内轴比小于3dB,轴比小于3dB的圆极化波束宽度可达180°,增益不小于6.6dB。经实测验证,所设计的天线具有宽频带宽波束特性,同时具有结构紧凑、性能稳定的优点,适用于卫星通信与导航终端系统。 相似文献
158.
航天器的发电能力与太阳电池阵有效发电面积成正比。针对圆柱形载人航天器,提出了一种体装太阳电池阵有效发电面积计算方法。首先,将太阳电池阵沿圆周方向划分为多个子阵,通过坐标变换,计算太阳矢量与每个子阵法线的夹角(即太阳入射角);然后,将每个子阵面积与对应太阳入射角的余弦相乘并求和,得到体装太阳电池阵的有效发电面积。对不同轨道日照角、不同飞行姿态下体装太阳电池阵有效发电面积进行仿真分析,仿真结果表明:三轴对地姿态下平均有效发电面积为安装面积的25%~32%,通过固定角度偏航可将有效发电面积提高至安装面积的30%~44%。 相似文献
159.
V.?A.?Afanas’ev G.?L.?Degtyarev A.?S.?MeshchanovEmail author 《Russian Aeronautics (Iz VUZ)》2018,61(1):23-31
Real values of parameters for a space vehicle and its steering devices are specified by using the motion parameters measured in flight based on solving the differential equations of motion. 相似文献
160.
Asteroids and comets are the remnants of the swarm of planetesimals from which the planets ultimately formed, and they retain records of processes that operated prior to and during planet formation. They are also likely the sources of most of the water and other volatiles accreted by Earth. In this review, we discuss the nature and probable origins of asteroids and comets based on data from remote observations, in situ measurements by spacecraft, and laboratory analyses of meteorites derived from asteroids. The asteroidal parent bodies of meteorites formed \(\leq 4\) Ma after Solar System formation while there was still a gas disk present. It seems increasingly likely that the parent bodies of meteorites spectroscopically linked with the E-, S-, M- and V-type asteroids formed sunward of Jupiter’s orbit, while those associated with C- and, possibly, D-type asteroids formed further out, beyond Jupiter but probably not beyond Saturn’s orbit. Comets formed further from the Sun than any of the meteorite parent bodies, and retain much higher abundances of interstellar material. CI and CM group meteorites are probably related to the most common C-type asteroids, and based on isotopic evidence they, rather than comets, are the most likely sources of the H and N accreted by the terrestrial planets. However, comets may have been major sources of the noble gases accreted by Earth and Venus. Possible constraints that these observations can place on models of giant planet formation and migration are explored. 相似文献