共查询到20条相似文献，搜索用时 31 毫秒
1.
Michael C. Malin 《Earth and Planetary Science Letters》1974,21(4):331-341
Some anomalous red features observed on the moon by Whitaker are examined in detail. Crater counts and regional stratigraphy suggest that ages for these features are comparable to that of lunar highland material. Initial gamma-ray spectrometry indicates higher than average native radioactivity is associated with certain red areas. A possible explanation for these observations is that the red objects are the surface manifestation of highly radioactive pre-mare basalts (Apollo 14/KREEP/norite material). Conclusive proof of the nature of these objects will depend on the study of returned samples, making them ideal candidates for future space missions, especially for unmanned vehicles such as the Soviet Union's Luna 20. 相似文献
2.
Explorations for the interior structure of the Moon mainly involve three technologies: the early gravitational observations via circumlunar satellites, the moonquake observations during the Apollo period, and the recent high-resolution remote sensing observations. Based on these technologies, we divided the development of the moon’s interior structure into three stages. The first stage is the discovery of high-density anomalous masses (mascons) on the lunar surface with the low-order gravitational field models, which were obtained by observing perturbations of the early lunar orbital satellites. The second stage is the preliminary understanding of the layer structure with the help of moonquake observations during the Apollo period. The third stage is the deep understanding of the structure of the lunar crust, mantle, and core, with the use of high-resolution remote sensing data and the reassessment of moonquake data from the Apollo’s mission. This paper gave detailed introduction and comments on different observation technologies, gathered data, and data processing techniques used at the three stages. In addition, this paper analyzed the current issues in the researches on the Moon’s internal structure and discussed the prospects for future explorations. 相似文献
3.
The relation between the local mean lunar time τ of earthquake occurrence and their fault trends is studied in this paper.
The local mean lunar times τ of 53 earthquakes in 24 groups are calculated. Because the tidal generation force arisen by the
moon is a cyclic function of about 12 hours 25 minutes in the main, the two tidal generation forces anywhere in the earth
arising by the moon are equal in general when the moon lies to the two sites of 180° interval of local mean lunar time. Based
on this phenomenon the values Δτ of τ1–τ2 or τ1–τ2 ± 180° of two earthquakes occurring repetitiously in the same place are also calculated. The calculated results show that
if the fault trends of the two earthquakes in the same place is near, the Δτ is usually smaller and if the fault trends of
the two ones is not near, the Δτ is usually larger and the distribution of the local mean lunar time τ of earthquakes in different
places is dispersive even if fault trends of these earthquakes are near, and the τ does not concentrate on the lower and upper
transit of the moon. The above phenomena clear up that the triggering earthquake of earth solid tide arisen by the moon is
relative with the fault trends of earthquakes and we ought to think over the difference of environmental conditions of earthquake
preparation of each seismogenic zone and can not make statistics to earthquakes in different places when we study the relation
between the solid earth tide arisen by the moon and earthquakes. 相似文献
4.
M. R. Thapar 《Pure and Applied Geophysics》1972,94(1):15-32
Summary The seismic records obtained from the seismic station ALSEP (Apollo Lunar Surface Experiments Package) on the moon, due to the impact of the LM (Lunar Module) of the Apollo XII and the S-IVB rocket state of the Apollo XIII moon missions show the seismic signals decaying in amplitude slowly with time. The observed ringing phenomenon on these records along with the fact that the disturbances lasted for a long period were unexpected. Laboratory experiments on homogeneous spheres have produced this ringing. The physical explanation of this may be complicated, and it is quite possible that this observed ringing is due to the combined effect of the filtering, reflections and scattering of energy due to the curvature of the homogeneous (in the seismic sense) sphere. The explanation of the ringing of the moon may very well lie in such a study. 相似文献
5.
GERALD K. MOORE 《水文科学杂志》2013,58(4):477-485
Abstract Remote sensing is the use of electromagnetic energy to measure the physical properties of distant objects. It includes photography and geophysical surveying as well as newer techniques that use other parts of the electromagnetic spectrum. The history of remote sensing begins with photography. The origin of other types of remote sensing can be traced to World War II, with the development of radar, sonar, and thermal infrared detection systems. Since the 1960s, sensors have been designed to operate in virtually all of the electromagnetic spectrum. Today a wide variety of remote sensing instruments are available for use in hydrological studies; satellite data, such as Skylab photographs and Landsat images are particularly suitable for regional problems and studies. Planned future satellites will provide a ground resolution of 10–80 m. Remote sensing is currently used for hydrological applications in most countries of the world. The range of applications includes groundwater exploration determination of physical water quality, snowfield mapping, flood-inundation delineation, and making inventories of irrigated land. The use of remote sensing commonly results in considerable hydrological information at minimal cost. This information can be used to speed-up the development of water resources, to improve management practices, and to monitor environmental problems. 相似文献
6.
An interpretation of previously reported measurements of the Apollo 15/16 alpha-particle spectrometer on the distribution of 222Rn and 210Po across the lunar surface suggests that continuation of these measurements is a method of monitoring current activity on the moon. Since the two isotopes are relatively short-lived with effective half-lives of 3 days and 21 years, respectively, the activity detected has had to have been released during this current epoch. Changes in the rate of lunar emanation can be measured on three different time scales: (1) of a few days or less by detecting 222Rn at discrete sites such as the crater Aristarchus; (2) of a month by measuring 222Rn activity at the sunrise terminator; (3) of a few years by measuring 210Po activity at various locations. These observations could be carried out very effectively from a lunar polar orbiting satellite. 相似文献
7.
Alan B. Binder 《Earth and Planetary Science Letters》1978,41(3):381-385
Observations of solar-type spectroscopic binary stars show that most of these objects were formed by rotational fission. By analogy, this empirical confirmation of the fission process is used to support the fission origin of the moon.The depletion of the volatile elements in the moon is explained as being due to their preferential evaporation from the initially hot (2000–4000°C) moon into an early primitive atmosphere. This atmosphere was simultaneously lost from the moon via transfer through theL1 point and captured by the earth. 相似文献
8.
R. CASSINIS 《Geophysical Prospecting》1972,20(1):142-154
“Remote sensing” techniques have been used for many years as an exploration tool; broadly speaking, any method using sensors not directly connected to the earth's surface falls into this group. It is preferable, however, to use the term solely with reference to a number of new sensors which have recently become available to earth scientists for the detection of various radiations of the electromagnetic spectrum in the wave length range from 0.1 micron (UV) to some centimeters including the visible and infrared regions. Radiations artificially induced in the earth (active sensing) or spontaneous radiations (passive sensing) can be detected. Some of the bands investigated seem promising for application to geological surveys, especially using sensors on aircraft and satellites, which allow synoptic and large scale investigations. A brief account is given of the results already achieved and of future developments such as the ERTS and manned satellite (post Apollo) “earth observation” programmes. The potential role of Europe in the field is discussed. Details are given of some applications of thermal I.R. imagery to geological and vulcanological problems, with special emphasis on the research carried out in Italy. 相似文献
9.
Conceptual study of lunar-based SAR for global change monitoring 总被引：1，自引：0，他引：1
HuaDong Guo YiXing Ding Guang Liu DaoWei Zhang WenXue Fu Lu Zhang 《中国科学:地球科学(英文版)》2014,57(8):1771-1779
As an active microwave remote sensing imaging sensor, Synthetic Aperture Radar (SAR) plays an important role in earth observation. Here we establish a SAR system based on the platform of the moon. This will aid large-scale, constant, and long-term dynamic Earth observations to better meet the needs of global change research and to complement the space borne and airborne earth observations. Lunar-based SAR systems have the characteristics of high resolution and wide swath width. The swath width could be thousands of kilometers in the stripe mode and it could cover 40% of earth’s surface with 10 meters or even higher spatial resolution in the scanning mode. Using the simplified observation model, here we quantitatively analyze the spatial resolution and coverage area of lunar-based SAR and simulate the observation on the Qinghai-Tibet plateau and the Amazon plain. The results show that this system could provide near 100% daily coverage of the Qinghai-Tibet plateau, whereas 40% to 70% daily coverage of the Amazon plain. Lunar-based SAR could provide large-scale, long-term and stable time series data in order to support future research of global change. 相似文献
10.
The purpose of the geoscientific Observatory at Schiltach in the Black Forest in SW-Germany is to measure and monitor motions and deformations of the earth in a frequency band as broad as possible. The spectrum of geodynamic signal contains
- • - the short period waves (up to 40 Hz) of near earthquakes,
- • - the longer period body and surface waves from teleseismic events,
- • - the free oscillations of the earth excited by giant earthquakes,
- • - the earth tide deformations caused by the gravitational forces of the moon and the sun having periods of 12 h and longer,
- • - deformations of the earth in a wide period range from other sources (e.g. atmosphere).
11.
《水文科学杂志》2013,58(4):725-740
Abstract Appropriate representation of landscape heterogeneity at small to medium scales is a central issue for hydrological modelling. Two main hydrological modelling approaches, deductive and inductive, are generally applied. Here, snow-cover ablation and basin snowmelt runoff are evaluated using a combined modelling approach that includes the incorporation of detailed process understanding along with information gained from observations of basin-wide streamflow phenomena. The study site is Granger Basin, a small sub-arctic basin in the mountains of the Yukon Territory, Canada. The analysis is based on the comparison between basin-aggregated and distributed landscape representations. Results show that the distributed model based on “hydrological response” landscape units best describes the observed magnitudes of both snow-cover ablation and basin runoff, whereas the aggregated approach fails to represent the differential snowmelt rates and to describe both runoff volumes and dynamics when discontinuous snowmelt events occur. 相似文献
12.
本文根据一个由较新的月震、月球形状、月球重力及月球天平动资料所建立的真实月球内部结构模型,解算了在地球和太阳的引潮力作用下月球表面的弹性潮汐形变。得到了表征月球弹性潮汐形变的特征数--月球勒夫数。这个结果与国外一些学者采用假想或简单月球模型所得结果有较大不同。同时,本文还根据近年来出现的新的地球模型,再次求解了地球的静态勒夫数。结果表明,采用不同的地球模型对解算地球的静态弹性潮汐形变的结果影响很小。 相似文献
13.
Prof. Dr. A. Berroth 《Pure and Applied Geophysics》1948,13(3-4):65-74
Summary The largest members in longitude and latitude of the theoretical movement of the earth's moon, developped byHill 1891 fromDelaunays theory of the moon, have been here calculated with new, now better known numerical values. Effectively a highly better accordance of the observed values with the theoretical ones has been obtained. This method will be able to give an important contribution to the determination of the figure of the earth with regard to the geometrical and the static flattening, specially by moons observation material of 1850–1950.
Résumé Les membres les plus grands en longitude et latitude du mouvement théorique de la lune développés parHill 1891, fondés sur la théorie deDelaunay, sont ici calculés avec de nouvelles valeurs numériques de meilleure connaissance. C'est pourquoi une bonne accordance est obtenue des valeurs observées avec les valeurs théoriques. La méthode donne une contribution importante à la détermination de la figure de la terre par rapport à l'aplatissement géométrique et l'aplatissement statique, principalement par égard aux observations de la lune 1850–1950.相似文献
14.
Bulk compositions of igneous and microbreccia lithic fragments, glasses, and chondrules from Luna 16 fines as well as compositions of minerals in basaltic lithic fragments were determined with the electron microprobe. Igneous lithic fragments and glasses are divided into two groups, the anorthositic-noritic-troctolitic (hereafter referred to as ANT) and basaltic groups. Chondrules are always of ANT composition and microbreccia lithic fragments are divided into groups 1 and 2. The conclusions reached may be summarized as follows: (1) Luna 16 fines are more similar in composition to Apollo 11 than to Apollo 12 and 14 materials (e.g. Apollo 11 igneous lithic fragments and glasses fall into similar ANT and basaltic groups; abundant norites in Luna 16 and Apollo 11 are not KREEP as in Apollo 12 and 14; Luna 16 basaltic lithic fragments may represent high-K and low-K suites as is the case for Apollo 11; rare colorless to greenish, FeO-rich and TiO2-poor glasses were found in both Apollo 11 and Luna 16; Luna 16 spinels are similar to Apollo 11 spinels but unlike those from Apollo 12). (2) No difference was noted in the composition of lithic fragments, glasses and chondrules from Luna 16 core tube layers A and D. (3) Microbreccia lithic fragments of group 1 originated locally by mixing of high proportions of basaltic with small proportions of ANT materials. (4) Glasses are the compositional analogs to the lithic fragments and not to the microbreccias; most glasses were produced directly from igneous rocks. (5) Glasses show partial loss of Na and K due to vaporization in the vitrification process. (6) Luna 16 chondrules have ANT but not basaltic composition. It is suggested that either liquid droplets of ANT composition are more apt to nucleate from the supercooled state; or basaltic droplets have largely been formed in small and ANT droplets in large impact events (in the latter case, probability for homogeneous and inhomogeneous nucleation is larger. (7) No evidence for ferric iron and water-bearing minerals was found. (8) Occurrence of a great variety of igneous rocks in Luna 16 samples (anorthosite, noritic anorthosite, anorthositic norite, olivine norite, troctolite, and basalt) confirm our earlier conclusion that large-scale melting or partial melting to considerable depth and extensive igneous differentiation must have occurred on the moon. 相似文献
15.
H.J. Melosh 《Earth and Planetary Science Letters》1975,26(3):353-360
This paper investigates the idea that large impact events have caused the moon to change its orientation in space. It is found that the very largest impact events, such as those which formed Imbrium and Orientale, probably did reorient the moon. This reorientation is primarily due to the change in the moon's moments of inertia consequent upon crater formation. The impulse delivered by the impact can at most unlock the moon's synchronous rotation for a few thousand years, and is thus not of major importance. The moon will attain its new orientation in less than a few times 104 years as a result of tidal friction. Since the large craters eventually are filled by isostatic rebound and extrusive igneous activity, the moon may eventually regain its original orientation unless other phenomena cause new changes in the distribution of mass on its surface. 相似文献
16.
引潮力的全球位移场及应力场 总被引：1，自引：0，他引：1
本文将地球看作由若干层均匀弹性球壳及一个液核所组成。文中用弹性力学方法得出了在日月引潮力作用下全球位移场及应力场的解析解。由它们将易于分析各种参数变化所产生的效应,这有助于地球模型的构制。 作为例子,文中对1981年IGS及IUGG公布并建议采用的“初步参考地球模型”（简称PREM模型）计算了引潮力引起的全球位移场及应力场,给出了模型地球的内部位移及应力的分布曲线。同时,对PREM模型计算了勒夫数及潮汐因子。计算结果与观测值相当吻合。 相似文献
17.
The Apollo 17 KREEPy basalt is a unique lunar volcanic rock, observed only as clasts in the light friable breccia matrix (72275) of Boulder 1, Station 2 at Taurus-Littrow. Its status as a volcanic rock is confirmed by the absence of any meteoritic contamination, a lack of cognate inclusions or xenocrystal material, and low Ni contents in metal grains.The basalt was extruded 4.01 ± 0.04 b.y. ago, approximately contemporaneously with the high-alumina mare basalts at Fra Mauro; shortly afterwards it was disrupted, probably by the Serenitatis impact, and its fragments emplaced in the South Massif. The basalt, which is quartz-normative and aluminous, is chemically and mineralogically intermediate between the Apollo 15 KREEP basalts and the high-alumina mare basalts in most respects. It consists mainly of plagioclase and pigeonitic pyroxene in approximately equal amounts, and 10–30% of mesostatis. Minor phases outside of the mesostatis are chromite, a silica mineral, Fe-metal, and rare olivine; the mesostatis consists primarily of ilmenite, Fe-metal, troilite, and ferroaugite, set in a glassy or microcrystalline Si-rich base.Chemical and isotopic data indicate that an origin by partial melting of a distinct source region is more probable than hybridization or contamination of magmas, and is responsible for the transitional composition of the basalt. The moon did not produce two completely distinct volcanic groups, the KREEP basalts and the mare/mare-like basalts; some intermediate rock types were generated as well. A corresponding spectrum of source regions must exist in the interior of the moon. 相似文献
18.
Winifred Sawtell Cameron 《Physics of the Earth and Planetary Interiors》1977,14(3):194-216
The author has been compiling a catalog of LTP reports (temporary changes observed on the moon). More than 1,400 of these observations, of which 1,353 have ancillary data, were analyzed in an attempt to determine the possible causes of LTP. There were 201 sites reported at least once; about had two or more reports. One dozen sites contain 70% of all observations, and one site, Aristarchus, provides 30%. Of the dozen most reported sites, are rayed and are dark flat-floored craters. The distribution of sites strongly favors the borders of both the terra and marial sides of the maria. Many are within the maria, and a very few are inland; yet most of these are associated with dark flat areas.The phenomena manifest themselves in five categories, viz., Brightenings, or Darkenings, or as Gaseous, Reddish and Bluish events. Among the hypotheses proposed for their causes are tidal, low-illumination/thermoluminescence, magnetic-tail and solar-flare effects. Analyses were conducted to see if different phenomena had different causes. There is some suggestion that they do. As concerns the tidal effects. the strongest peaks are at 0.5 (apogee) for Gaseous and Darkenings phenomena, 0.6 for Reddish events, and 0.7 for Brightenings. Reddish LTP have the strongest correlation with sunrise, while Aristarchus, Plato, Ross D area, and Bluish phenomena have the strongest correlations with solar-flare activity that produced magnetic storms on earth. “All” observations, the ones labeled “Best” (probable true anomalies), and Aristarchus, showed minima in the first half and maxima in the last half of the anomalistic (tidal) period. Histograms of several individual sites, including neighboring ones, behave differently, e.g. Aristarchus and Herodotus. When observed data are compared with expected observations (assumed to be evenly distributed) there were various correlations. For the Best data, 12 and 10% of the LTP fall close to perigee and apogee, respectively, and 10% would be expected for each. Seventeen percent occur within one day after sunrise when 3% would be expected; 20% occur while the moon is in the earth's magnetopause where 14% would be expected, and 12% occurred the same day the earth had a magnetic storm where 3% would be expected.Charts of albedo vs. age of several points for ten features were constructed. From these the normal behavior of the features throughout a lunation period was obtained. Measures that depart 2 or more full steps in Elger's albedo scale, are considered to be anomalies. Several cases of anomalous measures show up; e.g., for points on the south wall of Eimmart an albedo of 3.5 was reported once at age 10 days while for age 9 days the average albedo was 8, as it was afterward at age 11 days. The 3.5 may have been an anomalous darkening but unnoticed by the observer. Most of the features remained stable. A few exceptions were found, with Dawes showing the most anomalies. These amounted to 12% by nights or 2% by individual measures. Thus, monitoring the moon may yield an LTP once in ten nights, or 50 observations.All hypotheses show correlations with some categories and some features. Sunrise correlation is the most frequent correlation. Few correlations involve as many as 50% of the observations. The distribution of all LTP sites is different from and unique compared with deep- and shallow-focus moonquake epicenters. Routine albedo measures reveal unobserved variations which amount to about 10% in nights of observation bu 2% of individual albedo measures. 相似文献
19.
Yosio Nakamura 《Physics of the Earth and Planetary Interiors》1977,14(3):217-223
A few large distant seismic events of distinctly high signal frequency, designated HFT (high-frequency teleseismic) events, are observed yearly by the Apollo lunar seismic network. Their sources are located on or near the surface of the moon, leaving a large gap in seismic activity between the zones of HFT sources and deep moonquakes. No strong regularities are found in either their spatial or temporal distributions. Several working hypotheses for the identity of these sources have been advanced, but many characteristics of the events seem to favor a hypothesis that they are shallow moonquakes. Simultaneous observations of other lunar phenomena may eventually enable the determination of their true identity. 相似文献
20.
Radial thickness variation in impact crater ejecta: implications for lunar basin deposits 总被引：1，自引：0，他引：1
A review of cratering data and available semi-empirical calculations suggests that the variation of ejecta thickness,t, with increasing range from lunar craters may be approximately modelled by the expression: t=0.14R0.74(r/R?3.0 wherer is range from the center of the crater andR, the crater radius, all in meters. This equation has been used to estimate the thickness of ejecta deposits at each of the Apollo sites contributed from the large multi-ringed frontside lunar basins. Predicted average thickness of Imbrium ejecta at Apollo 15 is 812 m; at Apollo 14, 130 m; at Apollo 17, 102 m; and at Apollo 16, 50 m. Since the sequence of formation of these basins is known, the stratigraphic column resulting from superimposed ejecta blankets can be calculated. Results suggest that pre-Nubium crustal material at upland Apollo sites lies at depths greater than 280 (Apollo 14) to 1940 m (Apollo 17). Predicted stratigraphic sections for the Apollo sites are tabulated. 相似文献