排序方式： 共有14条查询结果，搜索用时 15 毫秒
1.
James B. Garvin 《Earth, Moon, and Planets》2004,94(3-4):221-232
The Vision for U.S. Space Exploration offers new opportunities for aggressively increasing the pace of scientific discoveries across the Solar System by empowering an on-site partnership between humans and robotics, enhanced by new technology-enabled capabilities. In particular, the early emphasis of this new Vision will be on development of new scientific activities on the Moon, and later on Mars. Integration of in situ traditional science activities with creative new types of applied scientific research on the Moon and Mars is a key ingredient in the US Vision. The Apollo era record of achievement involving human exploration is particularly informative, as it demonstrates the accelerated pace of scientific discovery and understanding that resulted from human “on site” activities, however briefly, on planetary surfaces. An example of how integrated human and robotic exploration can enable breakthrough science on the planet Mars is provided in order to illustrate these points. The scientific opportunities associated with the Vision for US Space Exploration are many, and with the incorporation of human-based capabilities on the Moon and Mars, an accelerated pace of discovery and understanding will be possible. 相似文献
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基于Clementine热红外数据的Apollo17登月点区域氧化钙含量反演 总被引：1，自引：0，他引：1
为了研究利用Clementine热红外数据反演月球表面岩石的氧化钙(Ca O)含量,论文选取了两景覆盖Apollo17登月点的Clementine热红外影像,将其覆盖的区域选为研究区。利用月球表面温度物理模型模拟月表温度,结合普朗克函数,完成发射率反演。在此基础上,对LPI中35个除Apollo17登月计划外所采集的样品Ca O含量与其热红外发射率特征做回归统计分析,发现存在很好的线性关系(R2=0.661)。由此,基于Clementine热红外发射率实现了研究区Ca O含量反演。通过利用LPI Apollo17月岩(壤)样品实际Ca O含量分析数据对反演结果进行精度评价,发现8组反演值与实际值的相对误差最小为1.77%,最大为9.29%,均方根误差为0.767。研究结果表明,使用发射率进行Ca O含量反演方法可行,为利用Clementine热红外数据对月表矿物成分含量定量反演提供一种新的思路。 相似文献
3.
中国嫦娥工程三期将进行月球样品的采集与返回,这是继美国Apollo和前苏联Luna之后,国际上最新的月球样品返回计划。月球样品的存储与管理方法将成为中国探月工程中亟待解决的重要问题之一。特别是如何最大程度地保持月球样品的科学研究价值,避免或减少可能的样品污染等问题,不仅为工程部门所关心,也是月球科学家所极为关注的问题。文中主要回顾和总结了美国Apollo月球样品的处理与保存方法,包括月球样品实验室简况、月球样品初步处理方法、月球样品初步测试分析及相关实验简介和月球样品的保存方法等内容,以期为中国月球样品的返回和地面存储提供有益的借鉴。 相似文献
4.
Gordon R. Osinski Pascal Lee Kelly Snook Darlene S.S. Lim 《Planetary and Space Science》2010,58(4):646-48
With the prospect of humans returning to Moon by the end of the next decade, considerable attention is being paid to technologies required to transport astronauts to the lunar surface and then to be able to carry out surface science. Recent and ongoing initiatives have focused on scientific questions to be asked. In contrast, few studies have addressed how these scientific priorities will be achieved. In this contribution, we provide some of the lessons learned from the exploration of the Haughton impact structure, an ideal lunar analogue site in the Canadian Arctic. Essentially, by studying how geologists carry out field science, we can provide guidelines for lunar surface operations. Our goal in this contribution is to inform the engineers and managers involved in mission planning, rather than the field geology community. Our results show that the exploration of the Haughton impact structure can be broken down into 3 distinct phases: (1) reconnaissance; (2) systematic regional-scale mapping and sampling; and (3) detailed local-scale mapping and sampling. This break down is similar to the classic scientific method practiced by field geologists of regional exploratory mapping followed by directed mapping at a local scale, except that we distinguish between two different phases of exploratory mapping. Our data show that the number of stops versus the number of samples collected versus the amount of data collected varied depending on the mission phase, as does the total distance covered per EVA. Thus, operational scenarios could take these differences into account, depending on the goals and duration of the mission. Important lessons learned include the need for flexibility in mission planning in order to account for serendipitous discoveries, the highlighting of key “science supersites” that may require return visits, the need for a rugged but simple human-operated rover, laboratory space in the habitat, and adequate room for returned samples, both in the habitat and in the return vehicle. The proposed set of recommendations ideally should be tried and tested in future analogue missions at terrestrial impact sites prior to planetary missions. 相似文献
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T.J. Stubbs D.A. Glenar W.M. Farrell R.R. Vondrak M.R. Collier J.S. Halekas G.T. Delory 《Planetary and Space Science》2011,59(13):1659-1664
Radio occultation measurements from the Soviet Luna 19 mission suggest that electron concentrations above the sunlit lunar surface can be significantly higher than that expected from either the photo-ionization of exospheric neutrals or any other well-known process. These measurements were used to infer the electron column concentrations above the lunar limb as a function of tangent height, which surprisingly indicated peak concentrations of ∼103 cm−3 at ∼5 km altitude. It has been speculated that electrically charged exospheric dust could contribute to such electron populations. This possibility is examined here using the exospheric dust abundances inferred from Apollo 15 coronal photographs to estimate the concentration of electrons produced by photo- and secondary emission from dust. These estimates far exceed the electron concentrations predicted by any other suggested mechanism, and are within a factor of ≈20 of those inferred from the Luna 19 measurements. It is possible that this discrepancy is due to an under-estimate in dust grain capacitances and/or the presence of much higher exospheric dust abundances during the Luna 19 measurements. These results suggest that electrons emitted from exospheric dust could be responsible for the Luna 19 measurements, and that this process could dominate the formation and evolution of the lunar ionosphere. 相似文献
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Marc D. Norman Vickie C. BennettGraham Ryder 《Earth and Planetary Science Letters》2002,202(2):217-228
Highly siderophile element compositions of lunar impact melt breccias provide a unique record of the asteroid population responsible for large cratering events in the inner Solar System. Melt breccias associated with the 3.89 Ga Serenitatis impact basin resolve at least two separate impact events. KREEP-rich melt breccias representing the Apollo 17 poikilitic suite are enriched in highly siderophile elements (3.6-15.8 ppb Ir) with CI-normalized patterns that are elevated in Re, Ru and Pd relative to Ir and Pt. The restricted range of lithophile element compositions combined with the coherent siderophile element signatures indicate formation of these breccias in a single impact event involving an EH chondrite asteroid, probably as melt sheet deposits from the Serenitatis Basin. One exceptional sample, a split from melt breccia 77035, has a distinctive lithophile element composition and a siderophile element signature more like that of ordinary chondrites, indicating a discrete impact event. The recognition of multiple impact events, and the clear signatures of specific types of meteoritic impactors in the Apollo 17 melt breccias, shows that the lunar crust was not comprehensively reworked by prior impacts from 3.9 to 4.5 Ga, an observation more consistent with a late cataclysm than a smoothly declining accretionary flux. Late accretion of enstatite chondrites during a 3.8-4.0 Ga cataclysm may have contributed to siderophile element heterogeneity on the Earth, but would not have made a significant contribution to the volatile budget of the Earth or oxidation of the terrestrial mantle. Siderophile element patterns of Apollo 17 poikilitic breccias become more fractionated with decreasing concentrations, trending away from known meteorite compositions to higher Re/Ir and Pd/Pt ratios. The compositions of these breccias may be explained by a two-stage impact melting process involving: (1) deep penetration of the Serenitatis impactor into meteorite-free lower crust, followed by (2) incorporation of upper crustal lithologies moderately contaminated by prior meteoritic infall into the melt sheet. Trends to higher Re/Ir with decreasing siderophile element concentrations may indicate an endogenous lunar crustal component, or a non-chondritic late accretionary veneer in the pre-Serenitatis upper crust. 相似文献
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月震与月球内部结构 总被引：3，自引：0，他引：3
阿波罗（Apollo）登月计划在月球表面上布设的月震仪为探索月球内部结构提供了极佳资料来源,本文综述了近年来对月震资料的分析及利用月震资料研究月球内部结构的相关研究结果。月震仪记录到的振动信号主要分为天体撞击、月震和局域震动三类。天体撞击又分为流星体撞击和人造天体撞击,其震源位于月球表面。月震按震源深度分布分为浅源月震与深源月震,前者的震源深度大约为50～220km,释放的能量较大但发生次数较少,记录信号以高频成分为主;后者的震源深度大约为700～1150km,并具丛集性,与潮汐应力有关。局域震动在月球日出与日落时出现,被认为是由近月表的热破裂和变形过程所产生。月球内部结构的多数研究集中于月震仪下方月壳厚度计算及上月幔一维速度模型的建立。结果表明月壳平均厚度大约为40km,而不是早期研究得到的60km左右;通过现有的月震资料还不能得到月球下月幔、月核、月球深部间断面的相关信息。文章最后对月球内部的进一步研究做了总结和展望。 相似文献
10.
Brian J. O'Brien 《Planetary and Space Science》2011,59(14):1708-1726
This is the first review of 3 Apollo experiments, which made the only direct measurements of dust on the lunar surface: (i) minimalist matchbox-sized 270 g Dust Detector Experiments (DDEs) of Apollo 11, 12, 14 and 15, produced 30 million Lunar Day measurements 21 July 1969–30 September, 1977; (ii) Thermal Degradation Samples (TDS) of Apollo 14, sprinkled with dust, photographed, taken back to Earth into quarantine and lost; and (iii) the 7.5 kg Lunar Ejecta and Meteoroids (LEAM) experiment of Apollo 17, whose original tapes and plots are lost. LEAM, designed to measure rare impacts of cosmic dust, registered scores of events each lunation most frequently around sunrise and sunset. LEAM data are accepted as caused by heavily-charged particles of lunar dust at speeds of <100 m/s, stimulating theoretical models of transporting lunar dust and adding significant motivation for returning to the Moon. New analyses here show some raw data are sporadic bursts of 1, 2, 3 or more events within time bubbles smaller than 0.6 s, not predicted by theoretical dust models but consistent with noise bits caused by electromagnetic interference (EMI) from switching of large currents in the Apollo 17 Lunar Surface Experiment Package (ALSEP), as occurred in pre-flight LEAM-acceptance tests. On the Moon switching is most common around sunrise and sunset in a dozen heavy-duty heaters essential for operational survival during 350 h of lunar night temperatures of minus 170 °C. Another four otherwise unexplained features of LEAM data are consistent with the “noise bits” hypothesis. Discoveries with DDE and TDS reported in 1970 and 1971, though overlooked, and extensive DDE discoveries in 2009 revealed strengths of adhesive and cohesive forces of lunar dust. Rocket exhaust gases during Lunar Module (LM) ascent caused dust and debris to (i) contaminate instruments 17 m distant (Apollo 11) as expected, and (ii) unexpectedly cleanse Apollo hardware 130 m (Apollo 12) and 180 m (Apollo 14) from LM. TDS photos uniquely document in situ cohesion of dust particles and their adhesion to 12 different test surfaces. This review finds the entire TDS experiment was contaminated, being inside the aura of outgassing from astronaut Alan Shepard's spacesuit, and applies an unprecedented caveat to all TDS discoveries. Published and further analyses of Apollo DDE, TDS and LEAM measurements can provide evidence-based guidance to theoretical analyses and to management and mitigation of major problems from sticky dust, and thus help optimise future lunar and asteroid missions, manned and robotic. 相似文献