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排序方式: 共有107条查询结果,搜索用时 281 毫秒
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深空探测车辆在星球表面巡视过程中,应避免过度沉陷,保障其可靠的通过性能具有重要意义。月球和火星表面重力加速度分别约为地球表面重力加速度的1/6和2/5,地面实现低重力环境的模拟具有一定局限性,因此基于相似理论进行轮壤相互作用系统的量纲分析,研制二分之一缩比模型车;开展缩比模型车轮壤试验,重点研究滑转条件下车轮沉陷行为和牵引特性;基于地面力学理论,结合轮壤接触应力分布的线性化方法,建立与沉陷和滑转率相关联的星球车挂钩牵引力预测模型。通过土槽试验数据对模型进行验证,结果表明该模型具有较高的准确性。能够为星球车通过性评估提供一定的理论技术基础。 相似文献
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由于距离地球较远、测控延时误差较大、飞行环境十分复杂且难以提前预测,行星软着陆的自主制导技术目前存在水平位置估计困难、导航参考信息匮乏、复杂地形着陆困难等挑战。针对行星软着陆存在的困难和挑战,提出了基于引导策略搜索算法的有模型强化学习制导方法,实现了着陆器在初始状态受到扰动时,无需重新规划,仍能在满足约束条件的情况下降落在指定位置。该方法将迭代线性二次调节器作为控制器,产生初始轨迹;其次,使用多层神经网络拟合制导策略;最后,利用控制器监督策略学习,进而收敛产生可行策略。针对行星表面软着陆的仿真验证结果显示该算法仅通过几次循环,即可以实现初始状态变化的快速软着陆。一方面表明了基于有模型强化学习的数据高效利用率,另一方面也证明了强化学习方法在深空探测领域中具有广阔的应用前景。 相似文献
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行星机构的结构设计缺陷、制造与安装误差、支撑构件刚度不足等原因可能会使系统发生一定程度的偏载,从而会影响整个机构的使用寿命与可靠性。利用最小次序统计量的概念建立了行星齿轮系的可靠度计算模型,模型反映了偏载对齿轮系可靠性的影响。首先,对行星机构进行了详细的运动学和力学分析,计算得到了各个齿轮的随机载荷历程。根据Miner线性疲劳累积损伤法则,将随机载荷历程转化为等效恒幅载荷谱,并将其作为可靠性模型的载荷输入变量。然后,将特定齿轮的疲劳寿命数据进行统计处理,将统计结果作为可靠性模型的强度输入变量。最后,根据模型的计算结果定量地说明了偏载对行星齿轮系可靠性的影响程度,同时利用随机截尾数据处理方法对可靠性模型的有效性进行了验证。 相似文献
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以2K?V行星传动机构中齿轮为研究对象,以齿轮啮合原理、传热学等为理论依据,分析了齿轮在不同啮合位置的相对滑动速度和齿面的接触应力的变化规律.精确计算了稳态温度场边界条件,包括齿轮一个啮合周期内的平均摩擦热流量和不同齿面的对流换热系数.建立单齿三维模型并导入ANSYS Workbench进行温度场的有限元分析.通过将啮... 相似文献
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S. Ota L. Sihver S. Kobayashi N. Hasebe 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2014
Depth dependency of neutrons produced by cosmic rays (CRs) in the lunar subsurface was estimated using the three-dimensional Monte Carlo particle and heavy ion transport simulation code, PHITS, incorporating the latest high energy nuclear data, JENDL/HE-2007. The PHITS simulations of equilibrium neutron density profiles in the lunar subsurface were compared with the measurement by Apollo 17 Lunar Neutron Probe Experiment (LNPE). Our calculations reproduced the LNPE data except for the 350–400 mg/cm2 region under the improved condition using the CR spectra model based on the latest observations, well-tested nuclear interaction models with systematic cross section data, and JENDL/HE-2007. 相似文献
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Herbert I. M. Lichtenegger Helmut Lammer Yuri N. Kulikov Shahin Kazeminejad Gregorio H. Molina-Cuberos Rafael Rodrigo Bobby Kazeminejad Gottfried Kirchengast 《Space Science Reviews》2006,126(1-4):469-501
The heating of the upper atmospheres and the formation of the ionospheres on Venus and Mars are mainly controlled by the solar
X-ray and extreme ultraviolet (EUV) radiation (λ = 0.1–102.7 nm and can be characterized by the 10.7 cm solar radio flux).
Previous estimations of the average Martian dayside exospheric temperature inferred from topside plasma scale heights, UV
airglow and Lyman-α dayglow observations of up to ∼500 K imply a stronger dependence on solar activity than that found on
Venus by the Pioneer Venus Orbiter (PVO) and Magellan spacecraft. However, this dependence appears to be inconsistent with
exospheric temperatures (<250 K) inferred from aerobraking maneuvers of recent spacecraft like Mars Pathfinder, Mars Global
Surveyor and Mars Odyssey during different solar activity periods and at different orbital locations of the planet. In a similar
way, early Lyman-α dayglow and UV airglow observations by Venera 4, Mariner 5 and 10, and Venera 9–12 at Venus also suggested
much higher exospheric temperatures of up to 1000 K as compared with the average dayside exospheric temperature of about 270
K inferred from neutral gas mass spectrometry data obtained by PVO. In order to compare Venus and Mars, we estimated the dayside
exobase temperature of Venus by using electron density profiles obtained from the PVO radio science experiment during the
solar cycle and found the Venusian temperature to vary between 250–300 K, being in reasonable agreement with the exospheric
temperatures inferred from Magellan aerobraking data and PVO mass spectrometer measurements. The same method has been applied
to Mars by studying the solar cycle variation of the ionospheric peak plasma density observed by Mars Global Surveyor during
both solar minimum and maximum conditions, yielding a temperature range between 190–220 K. This result clearly indicates that
the average Martian dayside temperature at the exobase does not exceed a value of about 240 K during high solar activity conditions
and that the response of the upper atmosphere temperature on Mars to solar activity near the ionization maximum is essentially
the same as on Venus. The reason for this discrepancy between exospheric temperature determinations from topside plasma scale
heights and electron distributions near the ionospheric maximum seems to lie in the fact that thermal and photochemical equilibrium
applies only at altitudes below 170 km, whereas topside scale heights are derived for much higher altitudes where they are
modified by transport processes and where local thermodynamic equilibrium (LTE) conditions are violated. Moreover, from simulating
the energy density distribution of photochemically produced moderately energetic H, C and O atoms, as well as CO molecules,
we argue that exospheric temperatures inferred from Lyman-α dayglow and UV airglow observations result in too high values,
because these particles, as well as energetic neutral atoms, transformed from solar wind protons into hydrogen atoms via charge
exchange, may contribute to the observed planetary hot neutral gas coronae. Because the low exospheric temperatures inferred
from neutral gas mass spectrometer and aerobraking data, as well as from CO+
2 UV doublet emissions near 180–260 nm obtained from the Mars Express SPICAM UV spectrograph suggest rather low heating efficiencies,
some hitherto unidentified additional IR-cooling mechanism in the thermospheres of both Venus and Mars is likely to exist.
An erratum to this article can be found at 相似文献