共查询到20条相似文献，搜索用时 46 毫秒
1.
Christensen PR Wyatt MB Glotch TD Rogers AD Anwar S Arvidson RE Bandfield JL Blaney DL Budney C Calvin WM Fallacaro A Fergason RL Gorelick N Graff TG Hamilton VE Hayes AG Johnson JR Knudson AT McSween HY Mehall GL Mehall LK Moersch JE Morris RV Smith MD Squyres SW Ruff SW Wolff MJ 《Science (New York, N.Y.)》2004,306(5702):1733-1739
The Miniature Thermal Emission Spectrometer (Mini-TES) on Opportunity investigated the mineral abundances and compositions of outcrops, rocks, and soils at Meridiani Planum. Coarse crystalline hematite and olivine-rich basaltic sands were observed as predicted from orbital TES spectroscopy. Outcrops of aqueous origin are composed of 15 to 35% by volume magnesium and calcium sulfates [a high-silica component modeled as a combination of glass, feldspar, and sheet silicates (approximately 20 to 30%)], and hematite; only minor jarosite is identified in Mini-TES spectra. Mini-TES spectra show only a hematite signature in the millimeter-sized spherules. Basaltic materials have more plagioclase than pyroxene, contain olivine, and are similar in inferred mineral composition to basalt mapped from orbit. Bounce rock is dominated by clinopyroxene and is close in inferred mineral composition to the basaltic martian meteorites. Bright wind streak material matches global dust. Waterlain rocks covered by unaltered basaltic sands suggest a change from an aqueous environment to one dominated by physical weathering. 相似文献
2.
Gemini-N observed the properties of dust ejected from the nucleus of comet 9P/Tempel 1 before and after its encounter with Deep Impact. Marked changes were seen in the 7.8- to 13-micrometer spectral energy distribution and derived grain properties of the inner coma. A strong, broad silicate feature dominated by emission from amorphous pyroxene, amorphous olivine, and magnesium-rich crystalline olivine had developed by 1 hour after impact. The ejected dust mass is congruent with 10(4) to 10(6) kilograms on the basis of our models. Twenty-six hours later the silicate feature had faded, leaving a smooth featureless spectrum, similar to that observed before the impact, suggesting that the impact did not produce a new active region releasing small particles on the nucleus. 相似文献
3.
McSween HY Arvidson RE Bell JF Blaney D Cabrol NA Christensen PR Clark BC Crisp JA Crumpler LS Des Marais DJ Farmer JD Gellert R Ghosh A Gorevan S Graff T Grant J Haskin LA Herkenhoff KE Johnson JR Jolliff BL Klingelhoefer G Knudson AT McLennan S Milam KA Moersch JE Morris RV Rieder R Ruff SW De Souza PA Squyres SW Wänke H Wang A Wyatt MB Yen A Zipfel J 《Science (New York, N.Y.)》2004,305(5685):842-845
The Spirit landing site in Gusev Crater on Mars contains dark, fine-grained, vesicular rocks interpreted as lavas. Pancam and Mini-Thermal Emission Spectrometer (Mini-TES) spectra suggest that all of these rocks are similar but have variable coatings and dust mantles. Magnified images of brushed and abraded rock surfaces show alteration rinds and veins. Rock interiors contain 相似文献
4.
Bell JF Squyres SW Arvidson RE Arneson HM Bass D Calvin W Farrand WH Goetz W Golombek M Greeley R Grotzinger J Guinness E Hayes AG Hubbard MY Herkenhoff KE Johnson MJ Johnson JR Joseph J Kinch KM Lemmon MT Li R Madsen MB Maki JN Malin M McCartney E McLennan S McSween HY Ming DW Morris RV Dobrea EZ Parker TJ Proton J Rice JW Seelos F Soderblom JM Soderblom LA Sohl-Dickstein JN Sullivan RJ Weitz CM Wolff MJ 《Science (New York, N.Y.)》2004,306(5702):1703-1709
Panoramic Camera (Pancam) images from Meridiani Planum reveal a low-albedo, generally flat, and relatively rock-free surface. Within and around impact craters and fractures, laminated outcrop rocks with higher albedo are observed. Fine-grained materials include dark sand, bright ferric iron-rich dust, angular rock clasts, and millimeter-size spheroidal granules that are eroding out of the laminated rocks. Spectra of sand, clasts, and one dark plains rock are consistent with mafic silicates such as pyroxene and olivine. Spectra of both the spherules and the laminated outcrop materials indicate the presence of crystalline ferric oxides or oxyhydroxides. Atmospheric observations show a steady decline in dust opacity during the mission. Astronomical observations captured solar transits by Phobos and Deimos and time-lapse observations of sunsets. 相似文献
5.
Constituents of lunar soils and rocks were studied by powder and singlecrystal x-ray diffraction. In addition to identification of minerals, including rare amphibole, mica, and aragonite, a detailed study of the important rock-forming minerals of the plagioclase, pyroxene, and olivine groups has begun. M?ssbauer spectra were recorded from lunar soils, ground rock samples, and separates of iron-bearing minerals. The proportions of iron-bearing minerals were estimated from computer-fitted areas for the bulk samples. The Fe(2+) in the lower-density fraction of pyroxene was ordered, whereas that of the higher-density fraction was disordered. 相似文献
6.
不同成因型母质发育土壤稀土元素的地球化学特征分析 总被引：6，自引：0，他引：6
唐南奇 《福建农林大学学报(自然科学版)》2002,31(3):383-387
分析了 1 7种母质发育土壤的稀土元素 (REE)的地球化学特征 ,结果表明 :(1 )基性岩浆岩母质发育土壤的稀土总丰度最高 ,红砂岩者最低 ;(2 )岩浆岩和喷出岩者的 REE科勃尔分布模式仍表现出母岩特征 ,沉积型者则相对平稳 ,但海相沉积型者变异显著 ;(3 )各类母质发育者∑ Ce/∑Y特征值达 3 .5 -4.7,∑ Ce与∑ Y分馏特征明显 ;(4 )砂页岩等 4种母质者δCe正异常 ,火山喷出岩等 3种母质者 δCe相对稳定 ,酸性岩浆岩等 1 0种母质者 δCe负异常 ;紫砂岩母质者 δEu正异常 ,页岩等 3种母质者δEu相对稳定 ,基性岩浆岩等 1 3种母质者 δEu负异常 ;(5 )逐步回归分析表明 ,∑ REE与 Ce、Sm、Dy、Lu,∑ Ce与 Pr、Sm,∑ Y与 Dy、Lu相关显著 ;(6)双重筛选逐步回归分析表明 ,∑ REE、∑ Ce与土壤 Fe2 O3相关极显著 ,∑ Y与土壤 p H值、粉砂粒、物理性粘粒相关显著 ;(7)通过 REE动态聚类分析 ,不同母质土壤可划分为基于岩性背景的三大类 相似文献
7.
Bell JF Squyres SW Arvidson RE Arneson HM Bass D Blaney D Cabrol N Calvin W Farmer J Farrand WH Goetz W Golombek M Grant JA Greeley R Guinness E Hayes AG Hubbard MY Herkenhoff KE Johnson MJ Johnson JR Joseph J Kinch KM Lemmon MT Li R Madsen MB Maki JN Malin M McCartney E McLennan S McSween HY Ming DW Moersch JE Morris RV Dobrea EZ Parker TJ Proton J Rice JW Seelos F Soderblom J Soderblom LA Sohl-Dickstein JN Sullivan RJ Wolff MJ Wang A 《Science (New York, N.Y.)》2004,305(5685):800-806
Panoramic Camera images at Gusev crater reveal a rock-strewn surface interspersed with high- to moderate-albedo fine-grained deposits occurring in part as drifts or in small circular swales or hollows. Optically thick coatings of fine-grained ferric iron-rich dust dominate most bright soil and rock surfaces. Spectra of some darker rock surfaces and rock regions exposed by brushing or grinding show near-infrared spectral signatures consistent with the presence of mafic silicates such as pyroxene or olivine. Atmospheric observations show a steady decline in dust opacity during the mission, and astronomical observations captured solar transits by the martian moons, Phobos and Deimos, as well as a view of Earth from the martian surface. 相似文献
8.
Herkenhoff KE Squyres SW Arvidson R Bass DS Bell JF Bertelsen P Cabrol NA Gaddis L Hayes AG Hviid SF Johnson JR Kinch KM Madsen MB Maki JN McLennan SM McSween HY Rice JW Sims M Smith PH Soderblom LA Spanovich N Sullivan R Wang A 《Science (New York, N.Y.)》2004,305(5685):824-826
The Microscopic Imager on the Spirit rover analyzed the textures of the soil and rocks at Gusev crater on Mars at a resolution of 100 micrometers. Weakly bound agglomerates of dust are present in the soil near the Columbia Memorial Station. Some of the brushed or abraded rock surfaces show igneous textures and evidence for alteration rinds, coatings, and veins consistent with secondary mineralization. The rock textures are consistent with a volcanic origin and subsequent alteration and/or weathering by impact events, wind, and possibly water. 相似文献
9.
Plagioclase and olivine crystals in the crystalline rocks from the Sea of Tranquillity show little or no evidence of either static or dynamic deformation. The large disorientations in many of the pyroxene crystals are commonly consistent with slip on the system T -(100), t = [001], but these distortions are not due to plastic flow. They are ascribed to rapid growth and quenching phenomena as deduced from studies of chondrules and of quenched natural and experimentally produced melts. Some of the silicates in the breccias and regolith show evidence of shock deformation, from mild to intense, as indicated by pervasive featuring, shock lamallae, and partial transformatiion of pyroxene and plagioclase crystals to glass. 相似文献
10.
Gellert R Rieder R Anderson RC Brückner J Clark BC Dreibus G Economou T Klingelhöfer G Lugmair GW Ming DW Squyres SW D'Uston C Wänke H Yen A Zipfel J 《Science (New York, N.Y.)》2004,305(5685):829-832
The alpha particle x-ray spectrometer on the Spirit rover determined major and minor elements of soils and rocks in Gusev crater in order to unravel the crustal evolution of planet Mars. The composition of soils is similar to those at previous landing sites, as a result of global mixing and distribution by dust storms. Rocks (fresh surfaces exposed by the rock abrasion tool) resemble volcanic rocks of primitive basaltic composition with low intrinsic potassium contents. High abundance of bromine (up to 170 parts per million) in rocks may indicate the alteration of surfaces formed during a past period of aqueous activity in Gusev crater. 相似文献
11.
Skinner BJ 《Science (New York, N.Y.)》1970,167(3918):652-654
Complex intergrowths of troilite (FeS) and iron in the igneous rocks from Tranquillity Base contain 8.4 percent native iron by volume. The intergrowths were derived from an initially homogeneous sulfide liquid that separated immiscibly from the magma at 1140 degrees C or above. Textures show that the sulfide liquid formed late in the crystallization and cooling history of the igneous rocks and after the major ilmenite and pyroxene had formed. 相似文献
12.
湘南红壤区三种土壤水热状况的研究 总被引：1，自引：2，他引：1
对同一地形和同一气候条件下湘南三种典型红壤的水热状况及它们的持水和渗透性质进行了研究。这三种土壤是：花岗岩母质发育的红壤、第四纪红土发育的红壤和紫色土。试验结果表明：第四纪红土发育的红壤持水性好，团聚度高，整个土体水分含量高，然而水分有效性低，渗透性好；花岗岩母质红壤则相反；紫色土则由于含有较多的块状物，因此渗透性也比较好。三种土壤的热量状况有很大的区别，紫色土在整个测定期间始终保持着较高的温度，而且温度的变幅大，花岗岩母质红壤的土体温度是三种土壤中最低的。植被影响土壤的水热状况，而水热状况又反过来影响作物的生长。 相似文献
13.
Bertelsen P Goetz W Madsen MB Kinch KM Hviid SF Knudsen JM Gunnlaugsson HP Merrison J Nørnberg P Squyres SW Bell JF Herkenhoff KE Gorevan S Yen AS Myrick T Klingelhöfer G Rieder R Gellert R 《Science (New York, N.Y.)》2004,305(5685):827-829
The magnetic properties experiments are designed to help identify the magnetic minerals in the dust and rocks on Mars-and to determine whether liquid water was involved in the formation and alteration of these magnetic minerals. Almost all of the dust particles suspended in the martian atmosphere must contain ferrimagnetic minerals (such as maghemite or magnetite) in an amount of approximately 2% by weight. The most magnetic fraction of the dust appears darker than the average dust. Magnetite was detected in the first two rocks ground by Spirit. 相似文献
14.
Lunar sample Preliminary Examination Team 《Science (New York, N.Y.)》1971,173(3998):681-693
The major findings of the preliminary examination of the lunar samples are as follows: 1) The samples from Fra Mauro base may be contrasted with those from Tranquillity base and the Ocean of Storms in that about half the Apollo 11 samples consist of basaltic rocks, and all but three Apollo 12 rocks are basaltic, whereas in the Apollo 14 samples only two rocks of the 33 rocks over 50 grams have basaltic textures. The samples from Fra Mauro base consist largely of fragmental rocks containing clasts of diverse lithologies and histories. Generally the rocks differ modally from earlier lunar samples in that they contain more plagioclase and contain orthopyroxene. 2) The Apollo 14 samples differ chemically from earlier lunar rocks and from their closest meteorite and terrestrial analogs. The lunar material closest in composition is the KREEP component (potassium, rare earth elements, phosphorus), "norite," "mottled gray fragments" (9) from the soil samples (in particular, sample 12033) from the Apollo 12 site, and the dark portion of rock 12013 (10). The Apollo 14 material is richer in titanium, iron, magnesium, and silicon than the Surveyor 7 material, the only lunar highlands material directly analyzed (11). The rocks also differ from the mare basalts, having much lower contents of iron, titanium, manganese, chromium, and scandium and higher contents of silicon, aluminum, zirconium, potassium, uranium, thorium, barium, rubidium, sodium, niobium, lithium, and lanthanum. The ratios of potassium to uranium are lower than those of terrestrial rocks and similar to those of earlier lunar samples. 3) The chemical composition of the soil closely resembles that of the fragmental rocks and the large basaltic rock (sample 14310) except that some elements (potassium, lanthanum, ytterbium, and barium) may be somewhat depleted in the soil with respect to the average rock composition. 4) Rocks display characteristic surface features of lunar material (impact microcraters, rounding) and shock effects similar to those observed in rocks and soil from the Apollo 11 and Apollo 12 missions. The rocks show no evidence of exposure to water, and their content of metallic iron suggests that they, like the Apollo 11 and Apollo 12 material, were formed and have remained in an environment with low oxygen activity. 5) The concentration of solar windimplanted material in the soil is large, as was the case for Apollo 11 and Apollo 12 soil. However, unlike previous fragmental rocks, Apollo 14 fragmental rocks possess solar wind contents ranging from approximately that of the soil to essentially zero, with most rocks investigated falling toward one extreme of this range. A positive correlation appears to exist between the solar wind components, carbon, and (20)Ne, of fragmental rocks and their friability (Fig. 12). 6) Carbon contents lie within the range of carbon contents for Apollo 11 and Apollo 12 samples. 7) Four fragmental rocks show surface exposure times (10 x 10(6) to 20 x 10(6) years) about an order of magnitude less than typical exposure times of Apollo 11 and Apollo 12 rocks. 8) A much broader range of soil mechanics properties was encountered at the Apollo 14 site than has been observed at the Apollo 11, Apollo 12, and Surveyor landing sites. At different points along the traverses of the Apollo 14 mission, lesser cohesion, coarser grain size, and greater resistance to penetration was found than at the Apollo 11 and Apollo 12 sites. These variations are indicative of a very complex, heterogeneous deposit. The soils are more poorly sorted, but the range of grain size is similar to those of the Apollo 11 and Apollo 12 soils. 9) No evidence of biological material has been found in the samples to date. 相似文献
15.
Rieder R Gellert R Anderson RC Brückner J Clark BC Dreibus G Economou T Klingelhöfer G Lugmair GW Ming DW Squyres SW d'Uston C Wänke H Yen A Zipfel J 《Science (New York, N.Y.)》2004,306(5702):1746-1749
The Alpha Particle X-ray Spectrometer on the Opportunity rover determined major and minor elements of soils and rocks in Meridiani Planum. Chemical compositions differentiate between basaltic rocks, evaporite-rich rocks, basaltic soils, and hematite-rich soils. Although soils are compositionally similar to those at previous landing sites, differences in iron and some minor element concentrations signify the addition of local components. Rocky outcrops are rich in sulfur and variably enriched in bromine relative to chlorine. The interaction with water in the past is indicated by the chemical features in rocks and soils at this site. 相似文献
16.
The rare gas distribution in lunar soil, breccias, and rocks was studied with a micro-helium-probe. Gases are concentrated in grain surfaces and originate from solar wind. Helium-4 concentrations of different mineral components vary by more than a factor of 10 apart from individual fluctuations for each type. Also grains with no detectable helium-4 exist. Titanium-rich components have the highest, calcium-rich minerals the lowest concentrations. The solar wind was redistributed by diffusion. Mean gas layer thicknesses are 10, 6, and 5 microm for helium, neon, and argon respectively. Lithic fragments in breccias contain no solar gases. Glass pitted surfaces of crystalline rocks contain about 10(-2) cubic centimeter of helium-4 per square centimeter. Etched dust grains clearly show spallogenic and radiogenic components. The apparent mean exposure age of dust is approximately 500 x 10(6) years, its potassium-argon age is approximately 3.5 x 10(9) yerars. Cavities of crystalline rocks contain helium-4, radiogenic argon, H(2), and N(2). 相似文献
17.
【目的】成土母质和植被类型是影响土壤酸化的2个主要因素,研究不同母质和植被类型下红壤pH和交换性酸的剖面变化及其酸化特征,为防治土壤酸化提供依据。【方法】选取3种植被类型（马尾松林、湿地松林、阔叶林）下4种母质（第四纪红土、红砂岩、板页岩和花岗岩）发育的红壤,通过测定不同层次（0—20、20—40、40—60、60—80和80—100 cm）土壤的pH及交换性酸,以及通过比较表层土壤（0—40 cm）与深层土壤（60—100 cm）pH的差异来表征红壤是否酸化及酸化程度大小。【结果】4种母质发育的剖面红壤均呈酸性或强酸性。在0—40 cm土层,4种母质红壤pH大小顺序为：花岗岩>红砂岩>第四纪红土>板页岩,3种植被类型下红壤pH大小顺序为：马尾松林>湿地松林>阔叶林,交换性酸含量则呈现相反的变化趋势;随着土层深度的增加,红砂岩、板页岩和花岗岩红壤pH呈减小趋势,交换性酸含量呈增加趋势,而第四纪红土红壤pH和交换性酸含量则呈现相反的变化趋势;在40—100 cm土层,4种母质红壤pH大小顺序为：花岗岩>第四纪红土>红砂岩>板页岩,3种植被类型下红壤pH的大小顺序为：湿地松林>马尾松林>阔叶林,交换性酸含量则呈现相反的变化趋势;随着土层深度的增加,第四纪红土、红砂岩和花岗岩红壤pH呈增加趋势,交换性酸含量呈减小趋势,而板页岩红壤pH和交换性酸含量变化不明显;通过比较表层土壤与深层土壤pH可得出：4种母质红壤的酸化程度大小顺序为：第四纪红土>红砂岩>花岗岩>板页岩;3种植被类型酸化效果的大小顺序为：湿地松林>阔叶林>马尾松林。【结论】3种植被类型下4种母质发育的红壤,剖面土壤pH和交换性酸的变异主要发生在0—40 cm土层,而40—100 cm土层pH和交换性酸的变化较小。在3种植被类型下,0—40 cm土层以第四纪红土红壤酸化最为严重,其次为红砂岩红壤和花岗岩红壤,再次为板页岩红壤;湿地松林的酸化效果最强,其次为阔叶林,以马尾松林的酸化效果最弱。 相似文献
18.
Ultrathin amorphous coatings on lunar dust grains 总被引：1，自引：0，他引：1
Bibring JP Duraud JP Durrieu L Jouret C Maurette M Meunier R 《Science (New York, N.Y.)》1972,175(4023):753-755
UItrathin amorphous coatings have been observed by high-voltage electron microscopy on micrometer-sized dust grains from the Apollo 11, Apollo 12, Apollo 14, and Luna 16 missions. Calibration experiments show that these coatings result from an "ancient" implantation of solar wind ions in the grains. This phenomenon has interdisciplinary applications concerning the past activity of the sun, the lunar albedo, the ancient lunar atmosphere and magnetic field, the carbon content of lunar soils, and lunar dynamic processes. 相似文献
19.
Tilles D 《Science (New York, N.Y.)》1966,153(3739):981-984
Measurements of excess Ar(36) + Ar(38) ( released mainly at 1200 degrees C) in magnetic concentrates of Pacific sediments and in a dense concentrate of Greenland dust agree within an order of magnitude with expected concentrations implanted by solar-flare ion streams of energy less than 10 Mev per atomic-mass unit. The agreement implies that more than 10 percent of each concentrate may be extraterrestrial, depending on size distribution and flare spectra. Rare-gas measurements on fine-grained dust can provide data on: solar-flare "paleo-ion" fluxes, energy spectra, and isotopic abundances; identification, mineralogy, and chemistry of interplanetary dust; influx rates to Earth and sedimentation rates of oceanic cores; and lunar-surface residence and mixing times. 相似文献
20.
【目的】研究环境因素对新疆不同地区田旋花种子萌发的影响,为制定有效的杂草防除技术提供理论依据。【方法】通过室内测定,研究温度、盐碱度、干旱、pH值等环境因子对新疆阿拉尔市和新和县两个点田旋花种子萌发的影响。【结果】阿拉尔市、新和县田旋花种子在5～50℃恒温范围内,随着温度的升高发芽率先升高后降低;田旋花种子最低发芽温度为5℃,当温度上升到30～40℃,两个县市的田旋花种子发芽率均达到最大值,种子在15℃/5℃～45℃/35℃的变温条件下均可发芽,且当温度为40℃/30℃时发芽率最高。盐碱胁迫可降低田旋花种子的发芽率,当NaCl浓度大于300 mmol/L或NaHCO3浓度大于250 mmol/L时,两个县市的田旋花种子不能萌发;同时,田旋花种子的萌发受水势的影响较大,随着水势的增加,田旋花种子的发芽率逐渐降低,当水势达-0.6 MPa时,新和县田旋花种子已不能萌发,当水势达到-1.0 MPa时,阿拉尔市田旋花种子的萌发率仅为2%;pH值5～10,两个县市的田旋花种子均能正常萌发。【结论】室内模拟实验条件下,温度、盐碱和水势均是影响新疆不同地区田旋花种子萌发的关键环境因素,而农田生态系统中,干旱胁迫和pH不是限制田旋花萌发的主要因素。 相似文献