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131.
Frédéric Schmidt Bernard Schmitt Francois Forget Patrick Martin Jean-Pierre Bibring the OMEGA Team 《Planetary and Space Science》2010,58(10):1129-1138
The polar condensation/sublimation of CO2, that involve about one fourth of the atmosphere mass, is the major Martian climatic cycle. Early observations in visible and thermal infrared have shown that the sublimation of the Seasonal South Polar Cap (SSPC) is not symmetric around the geographic South Pole.Here we use observations by OMEGA/Mars Express in the near-infrared to detect unambiguously the presence of CO2 at the surface, and to estimate albedo. Second, we estimate the sublimation of CO2 released in the atmosphere and show that there is a two-step process. From Ls=180° to 220°, the sublimation is nearly symmetric with a slight advantage for the cryptic region. After Ls=220° the anti-cryptic region sublimation is stronger. Those two phases are not balanced such that there is 22% ± 9 more mass the anti-cryptic region, arguing for more snow precipitation. We compare those results with the MOLA height measurements. Finally we discuss implications for the Martian atmosphere about general circulation and gas tracers, e.g. Ar. 相似文献
132.
中祁连东段绿岩带可区分出绿岩部分和基底部分两套地层。恢复湟源群建群初期的划分观点。化隆超基性“岩带”和零星分布于西宁盆地边部产状不明的“岩体”应归属绿岩带下部镁铁质—超镁铁质岩系中。 相似文献
133.
在评述中国地壳形变、应变连续观测技术30年发展成就的基础上,论述和分析建立我国地壳形变、应变连续观测台网数字化网络系统的必要性及实施思路和方法。提出了该领域待深入研究的几个问题,为本领域跨世纪持续发展、跟踪国际前沿做好技术准备 相似文献
134.
滩间山金矿田产出部位及矿体延展严格受断裂构造制约。矿田区主要发育北西向压扭性断裂、北东向张扭性断裂和近东西向扭性断裂。北西向、北东向断裂均为控矿断裂,但北东向断裂的控矿作用更为明显。 相似文献
135.
F. Paganelli M.A. Janssen R. West J.I. Lunine S.D. Wall R.M. Lopes R.L. Kirk L. Roth the Radar Team 《Icarus》2007,191(1):211-222
The first five Titan flybys with Cassini's Synthetic Aperture RADAR (SAR) and radiometer are examined with emphasis on the calibration and interpretation of the high-resolution radiometry data acquired during the SAR mode (SAR-radiometry). Maps of the 2-cm wavelength brightness temperature are obtained coincident with the SAR swath imaging, with spatial resolution approaching 6 km. A preliminary calibration shows that brightness temperature in these maps varies from 64 to 89 K. Surface features and physical properties derived from the SAR-radiometry maps and SAR imaging are strongly correlated; in general, we find that surface features with high radar reflectivity are associated with radiometrically cold regions, while surface features with low radar reflectivity correlate with radiometrically warm regions. We examined scatterplots of the normalized radar cross-section σ0 versus brightness temperature, finding differing signatures that characterize various terrains and surface features. Implications for the physical and compositional properties of these features are discussed. The results indicate that volume scattering is important in many areas of Titan's surface, particularly Xanadu, while other areas exhibit complex brightness temperature variations consistent with variable slopes or surface material and compositional properties. 相似文献
136.
The way in which galaxy properties are influenced by environment is an important constraint on models of galaxy formation.
Using the complete2dF Galaxy Redshift Survey (2dFGRS, see Colless et al., 2001),containing over 225,000 galaxy redshifts,
we construct the largest and most uniform group catalogue to date. Here we present tests of our methodology, which is underpinned
by mock 2dFGRS catalogues made from a combination of high resolution N-body simulations and the Cole et al. semi-analytic
model of galaxy formation. Some basic characteristics of the 2dFGRS group catalogue are given.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
137.
Steven J. Ostro Richard D. West Ralph D. Lorenz Gregory J. Black Lauren C. Wye Stephen D. Wall Laci Roth Kathleen Kelleher Yonggyu Gim Rudy A. Boehmer the Cassini RADAR Team 《Icarus》2006,183(2):479-490
Cassini 2.2-cm radar and radiometric observations of seven of Saturn's icy satellites yield properties that apparently are dominated by subsurface volume scattering and are similar to those of the icy Galilean satellites. Average radar albedos decrease in the order Enceladus/Tethys, Hyperion, Rhea, Dione, Iapetus, and Phoebe. This sequence most likely corresponds to increasing contamination of near-surface water ice, which is intrinsically very transparent at radio wavelengths. Plausible candidates for contaminants include ammonia, silicates, metallic oxides, and polar organics (ranging from nitriles like HCN to complex tholins). There is correlation of our targets' radar and optical albedos, probably due to variations in the concentration of optically dark contaminants in near-surface water ice and the resulting variable attenuation of the high-order multiple scattering responsible for high radar albedos. Our highest radar albedos, for Enceladus and Tethys, probably require that at least the uppermost one to several decimeters of the surface be extremely clean water ice regolith that is structurally complex (i.e., mature) enough for there to be high-order multiple scattering within it. At the other extreme, Phoebe has an asteroidal radar reflectivity that may be due to a combination of single and volume scattering. Iapetus' 2.2-cm radar albedo is dramatically higher on the optically bright trailing side than the optically dark leading side, whereas 13-cm results reported by Black et al. [Black, G.J., Campbell, D.B., Carter, L.M., Ostro, S.J., 2004. Science 304, 553] show hardly any hemispheric asymmetry and give a mean radar reflectivity several times lower than the reflectivity measured at 2.2 cm. These Iapetus results are understandable if ammonia is much less abundant on both sides within the upper one to several decimeters than at greater depths, and if the leading side's optically dark contaminant is present to depths of at least one to several decimeters. As argued by Lanzerotti et al. [Lanzerotti, L.J., Brown, W.L., Marcantonio, K.J., Johnson, R.E., 1984. Nature 312, 139-140], a combination of ion erosion and micrometeoroid gardening may have depleted ammonia from the surfaces of Saturn's icy satellites. Given the hypersensitivity of water ice's absorption length to ammonia concentration, an increase in ammonia with depth could allow efficient 2.2-cm scattering from within the top one to several decimeters while attenuating 13-cm echoes, which would require a six-fold thicker scattering layer. If so, we would expect each of the icy satellites' average radar albedos to be higher at 2.2 cm than at 13 cm, as is the case so far with Rhea [Black, G., Campbell, D., 2004. Bull. Am. Astron. Soc. 36, 1123] as well as Iapetus. 相似文献
138.
辽宁北部地区凡河群源于斋藤林次的凡河系,其时代归属尚有争议。目前多数人将凡河群与蓟县地区的中、上元古界对比;殷屯组的时代则以暂置震且纪居主导地位。笔者稂据凡河群地史演化、所处大地构造位置、变质作用、含海相火山岩夹层、同位素年龄资料等综合因素分析;认为凡河群的时代以归属长城纪为宜,殷屯组时代归属蓟县纪较合适。 相似文献
139.
Oliver L. White Ali Safaeinili Stephen M. Clifford The MARSIS Science Team 《Icarus》2009,201(2):460-473
The MARSIS radar experiment aboard the ESA Mars Express satellite has recorded several unusual reflections in the Ma'adim Vallis region of Mars. These reflections display a wide variety of morphologies which are very different from those of reflections seen beneath the Polar Layered Deposits, Medusae Fossae Formation and Dorsa Argentea Formation. Their morphologies are sometimes very laterally extensive, parabolic or hyperbolic, and apparently deep, but they can also appear horizontal and shallow. Aided by a geological map of the Ma'adim Vallis region, the morphological, locational and temporal characteristics of the reflections have been studied individually in an attempt to constrain their origin. While some may be subsurface reflections based on their shallow morphologies and correlation with the Eridania Planitia basin network, all of the reflections are ambiguous to some degree, displaying characteristics that do not allow a definite subsurface- or possibly ionospheric-sourced mechanism to be proposed for their creation. Those with more exaggerated morphologies are regarded as being much more likely to result from ionospheric distortion rather than subsurface inhomogeneity. 相似文献
140.
The origin of the martian chaotic terrains is still uncertain; and a variety of geologic scenarios have been proposed. We provide topographic profiles of different chaos landscapes, notably Aureum and Hydraotes Chaos, showing that an initial shallow ground subsidence occurred at the first step of the chaos formation. We infer that the subsidence was caused by intrusion of a volcanic sill; which could have produced consequent melting as well as release of ground water from disrupted aquifer. Signs of a volcanic activity are observed on the floor of Hydraotes Chaos, a complex and deep depression located at the junction of three channels. The volcanic activity is represented by small, 0.5 to 1.5 km diameter, rounded cones with summit pits. The cone's size and morphology, as well as the presence of possible surrounding lava flows, suggest that they are primary volcanic cones similar to terrestrial cinder cones. The identification of volcanic activity on the deepest chaos, where the lower crustal thickness and the faults/fractures system contributed to the magma rising, reveals that magmatic activity, proved by the cones, and possibly help by structural activity, has been a major factor in the formation of chaotic terrains. 相似文献