热力学计算模拟对初始月幔结构的约束SCIEI北大核心CSCD     

鞠东阳  庞润连  李瑞  杜蔚 《岩石学报》2022,38(4):1025-1042

月球岩浆洋结晶形成的初始月球内部结构是其后续演化过程的开端,其结晶过程受月球岩浆洋的初始深度和物质组成这两个参数的制约。由于缺少直接来自月球深部的岩石样品,目前关于月球岩浆洋演化过程的探讨主要依赖实验和计算模拟手段。岩浆洋模型中形成的月壳厚度是否与探测结果一致是月球岩浆洋演化模型合理性的重要约束。最新的GRAIL(Gravity Recovery and Interior Laboratory)探测数据推算月壳厚度为34~43km,低于阿波罗时期认为的约70km,这对已有的月球岩浆洋演化模型提出了挑战。本文采用并修正FXMOTR程序包,针对月球岩浆洋在不同的初始深度和物质组成情况下的结晶过程,进行了一系列热力学计算模拟。通过量化月球岩浆洋的初始深度和物质组成对月壳厚度的影响,结合关于月球内部微量元素分配的研究结果,对比了月球岩浆洋结晶后期的残余熔体与原始克里普组分(urKREEP)的成分。本文的模拟结果显示,一个全月幔熔融且初始成分为月球初始上月幔组成(LPUM)的岩浆洋将在其深部结晶2.5%石榴子石,形成的月壳厚度符合GRAIL的约束,并且结晶出了合适的urKREEP成分。在此模型的基础上获取了月球初始的内部成分和密度结构,并对后期月幔翻转(Overturn)的程度进行了探讨。  相似文献   

基于测月雷达机制月壤相对介电常数反演方法模拟研究     

邢树果  苏彦 《天文研究与技术》2015,(3)

嫦娥三号卫星于2013年12月2日发射,并成功着陆月球,其巡视器上搭载的测月雷达实现了首次雷达就位探测月球。基于测月雷达的探测机制,给出了两种计算月壤相对介电常数的方法,标定件标定法和双天线时延法,并通过仿真验证了两种计算方法的有效性,文中同时给出了两种计算方法存在的局限性,为后期基于嫦娥三号雷达数据进行月球次表层的介电特性反演提供了重要依据。  相似文献   

建立WebGIS的月球三维可视化关键技术     

邢丽平  ;左维  ;李春来 《天文研究与技术》2014,(3):299-304

嫦娥工程获得了大量月球探测数据。针对让公众用户通过网络获取月球信息,更好了解月球知识的需求,地面应用系统提出了建立基于WebGIS的月球三维可视化系统的解决方案。首先介绍了国内外三维月球的发展现状,详细分析了开发WebGIS系统的客户端和服务器端技术,重点阐述了月球空间数据模型和三维场景可视化渲染等三维GIS可视化关键技术,为建立我国的三维月球可视化系统提供了理论支持。  相似文献   

Influence of the asymmetrical cratering rate on the lunar cratering chronology     

Tomokatsu Morota  Takashi Ukai  Muneyoshi Furumoto 《Icarus》2005,173(2):322-324

The lunar cratering rate studied over the past 1.1 Gyr, which is a foundation of the lunar cratering chronology, is a decreasing function of the angular distance from the apex of the orbital motion due to the synchronous rotation of the Moon. We here evaluate an influence of the asymmetrical rate upon the age determination.  相似文献   

3. Solar System Formation and Early Evolution: the First 100 Million Years     

Thierry Montmerle  Jean-Charles Augereau  Marc Chaussidon  Mathieu Gounelle  Bernard Marty  Alessandro Morbidelli 《Earth, Moon, and Planets》2006,98(1-4):39-95

The solar system, as we know it today, is about 4.5 billion years old. It is widely believed that it was essentially completed 100 million years after the formation of the Sun, which itself took less than 1 million years, although the exact chronology remains highly uncertain. For instance: which, of the giant planets or the terrestrial planets, formed first, and how? How did they acquire their mass? What was the early evolution of the “primitive solar nebula” (solar nebula for short)? What is its relation with the circumstellar disks that are ubiquitous around young low-mass stars today? Is it possible to define a “time zero” (t ₀), the epoch of the formation of the solar system? Is the solar system exceptional or common? This astronomical chapter focuses on the early stages, which determine in large part the subsequent evolution of the proto-solar system. This evolution is logarithmic, being very fast initially, then gradually slowing down. The chapter is thus divided in three parts: (1) The first million years: the stellar era. The dominant phase is the formation of the Sun in a stellar cluster, via accretion of material from a circumstellar disk, itself fed by a progressively vanishing circumstellar envelope. (2) The first 10 million years: the disk era. The dominant phase is the evolution and progressive disappearance of circumstellar disks around evolved young stars; planets will start to form at this stage. Important constraints on the solar nebula and on planet formation are drawn from the most primitive objects in the solar system, i.e., meteorites. (3) The first 100 million years: the “telluric” era. This phase is dominated by terrestrial (rocky) planet formation and differentiation, and the appearance of oceans and atmospheres.  相似文献   

Comment on the paper “Fast tidal cycling and the origin of life” by Richard Lathe     

P. Varga  K.R. Rybicki 《Icarus》2006,180(1):274-276

We show that the fast tidal cycling postulated by Lathe [Lathe, R., 2004. Icarus 168, 18-22] is not a plausible mechanism to explain the origin of life on Earth about 3.9 Ga ago. The value of LOD at this remote epoch was probably comprised between 15 to 17 h, and the Earth-Moon distance was only about 20% smaller than nowadays, implying that the tidal frequencies and amplitudes were not so dramatically different from the present ones as stated in Lathe's paper.  相似文献   

Lunar and terrestrial tidal effects on the Moon's rotational motion     

E. Bois  A. Journet 《Celestial Mechanics and Dynamical Astronomy》1993,57(1-2):295-305

An accurate model of the rotation of the Moon, constructed by numerical integration, has been presented in a previous paper. All direct perturbations capable of producing at least 10^–4 seconds of arc on the Moon's rotational motion have been included, and the physical librations resulting from planetary effects and Earth-Moon figure-figure interactions have been presented. The present study deals with the Moon's physical librations resulting from the non-rigidities of the Moon and the Earth. The effects of the Moon's elasticity and of a lunar phase lag are analyzed. Physical librations due to lunar tides and those due to terrestrial tides are presented and described.  相似文献   

Shock metamorphism on the moon     

Yasunori Miura  Toshio Kato 《Celestial Mechanics and Dynamical Astronomy》1992,54(1-3):245-248

Shock metamorphism of the lunar samples is discussed. All types of lunar glasses formed by various-size collision-type impact are found as impact glass, ropy glass and agglutinates. The agglutinates bonded by crystal and glassy materials contain hydrogen and helium from the solar wind components. Lunar shocked minerals of plagioclase and silica show anomalous compositions and densities. There are typical two formation processes on planetary materials formed by shock events; that is (1) shocked quartz formed by silica-rich target rocks (esp. on evolved planets of the Earth and Mars), and (2) shocked silica with minor Al contents formed from plagioclase-rich primordial crusts of the Moon. The both shocked silica grows to coarse-grain normal crystals after high-temperature metamorphism which cannot distinguish the original main formation event of impact process.  相似文献   

A lunar cryptomare dome near Mee H and Drebbel F     

Raffaello Lena  Jim Phillips  Geologic Lunar Research Group 《Planetary and Space Science》2009,57(3):267-275

In this study, we examine the lunar mare dome Mee 1 situated near the craters Mee H and Drebbel F in a region showing evidence of ancient (pre-Orientale) mare volcanism and cryptomare deposits. Regional stratigraphic relations indicate that Mee 1 was formed prior to the Orientale impact at the beginning of the Imbrian period. Based on a combined photoclinometry and shape from shading technique applied to telescopic CCD images of the dome acquired under oblique illumination, we determined a diameter of Mee 1 of 25 km, a height of 250 m, a flank slope of 1.15^°, and a volume of . Based on rheologic modelling of the dome and a viscoelastic model of the feeder dike, we obtained a magma viscosity of , an effusion rate of , a duration of the effusion process of 1.6 years, a magma rise speed of , a width of the feeder dike of 32 m, and a horizontal dike length of 144 km. A comparison of Mee 1 with domes with similar morphometric properties, which are located near Milichius and inside the crater Petavius, reveals strong similarities with respect to the viscosity of the dome-forming magma and the feeder dike geometry, while the effusion rate and magma rise speed of Mee 1 are somewhat higher. The pronounced morphometric differences between Mee 1 and a smaller dome situated close to the crater Doppelmayer and characterised by a similar magma viscosity suggest that the growth of that dome was limited by exhaustion of the magma reservoir, while Mee 1 and the other larger domes display morphometric properties presumably coming closer to the cooling limit. The comparison of the ancient dome Mee 1 with the younger (Eratosthenian) edifices near Milichius and Doppelmayer suggests that the conditions in the upper mantle and the crust favoured high eruption volumes, effusion rates, and magma rise speeds, implying the occurrence of large magma reservoirs preventing the limitation of dome growth by magma exhaustion. On the other hand, we observe similar general morphometric, rheologic, and feeder dike characteristics and, thus, conclude that the formation conditions of lunar mare domes did not change fundamentally during the Imbrian period.  相似文献   

The C1XS X-ray Spectrometer on Chandrayaan-1   总被引：1，自引：0，他引：1  

M. Grande  B.J. Maddison  B.J. Kellett  J. Huovelin  C.L. Duston  M. Anand  A. Cook  B. Foing  J.N. Goswami  K.H. Joy  D. Kochney  S. Maurice  S. Narendranath  D. Rothery  A. Shrivastava  M. Wilding 《Planetary and Space Science》2009,57(7):717-724

The Chandrayaan-1 X-ray Spectrometer (C1XS) is a compact X-ray spectrometer for the Indian Space Research Organisation (ISRO) Chandrayaan-1 lunar mission. It exploits heritage from the D-CIXS instrument on ESA's SMART-1 mission. As a result of detailed developments to all aspects of the design, its performance as measured in the laboratory greatly surpasses that of D-CIXS. In comparison with SMART-1, Chandrayaan-1 is a science-oriented rather than a technology mission, leading to far more favourable conditions for science measurements. C1XS is designed to measure absolute and relative abundances of major rock-forming elements (principally Mg, Al, Si, Ca and Fe) in the lunar crust with spatial resolution ?25 FWHM km, and to achieve relative elemental abundances of better than 10%.  相似文献