全文获取类型
收费全文 | 6450篇 |
免费 | 282篇 |
国内免费 | 81篇 |
专业分类
测绘学 | 235篇 |
大气科学 | 512篇 |
地球物理 | 1522篇 |
地质学 | 2160篇 |
海洋学 | 523篇 |
天文学 | 1187篇 |
综合类 | 28篇 |
自然地理 | 646篇 |
出版年
2022年 | 30篇 |
2021年 | 76篇 |
2020年 | 87篇 |
2019年 | 122篇 |
2018年 | 178篇 |
2017年 | 161篇 |
2016年 | 231篇 |
2015年 | 173篇 |
2014年 | 196篇 |
2013年 | 407篇 |
2012年 | 257篇 |
2011年 | 342篇 |
2010年 | 291篇 |
2009年 | 382篇 |
2008年 | 336篇 |
2007年 | 293篇 |
2006年 | 270篇 |
2005年 | 259篇 |
2004年 | 261篇 |
2003年 | 205篇 |
2002年 | 214篇 |
2001年 | 116篇 |
2000年 | 145篇 |
1999年 | 103篇 |
1998年 | 115篇 |
1997年 | 82篇 |
1996年 | 86篇 |
1995年 | 83篇 |
1994年 | 90篇 |
1993年 | 73篇 |
1992年 | 88篇 |
1991年 | 67篇 |
1990年 | 55篇 |
1989年 | 50篇 |
1988年 | 57篇 |
1987年 | 52篇 |
1986年 | 56篇 |
1985年 | 67篇 |
1984年 | 64篇 |
1983年 | 76篇 |
1982年 | 57篇 |
1981年 | 65篇 |
1980年 | 55篇 |
1979年 | 65篇 |
1978年 | 51篇 |
1977年 | 34篇 |
1976年 | 28篇 |
1975年 | 26篇 |
1974年 | 26篇 |
1973年 | 30篇 |
排序方式: 共有6813条查询结果,搜索用时 15 毫秒
841.
842.
Everett K. Gibson David E. Lange Klaus Keil Terry E. Schmidt J. Michael Rhodes 《Meteoritics & planetary science》1977,12(2):95-107
The Kramer Creek, Colorado, chondrite was found in 1966 and identified as a meteorite in 1972. Bulk chemical analysis, particularly the total iron content (20.36%) and the ratio of Fetotal/SiO2 (0.52), as well as the compositions of olivine (Fa21.7) and orthopyroxene (Fs18.3) place the meteorite into the L-group of chondrites. The well-defined chondritic texture of the meteorite, the presence of igneous glass in the chondrules and of low-Ca clinopyroxene, as well as the slight variations in FeO contents of olivine (2.4% MD) and orthopyroxene (5.6% MD) indicate that the chondrite belongs to the type 4 petrologic class. 相似文献
843.
An ion-exchange technique was used to concentrate ammonia from seawater. Precipitation of bivalent cations, prior to concentration, reduced the variability of ammonia recovery from the ion-exchange column and lengthened column life. Analysis of the eluate was by the phenolhypochlorite reaction. The method was designed for use with small seawater samples (>10ml) and has the advantage that it can be adapted for use with small volumes of seawater with no loss in sensitivity. In a 10 ml seawater example NH3-N concentrations of 10–150 μg l?1 were accurately determined. 相似文献
844.
Michael W. Ovenden Terry Feagin Otis Graf 《Celestial Mechanics and Dynamical Astronomy》1974,8(4):455-471
The Principle of Least Interaction Action, which explains the observed preference in the Solar System for two-satellite resonant configurations, is shown to apply also to the Laplacean satellites of Jupiter and Uranus, in the sense that these triplet resonant structures lie close to configurations for which the time-mean of the action associated with the mutual interaction of the satellites is an overall minimum. Far from the minimum configuration, significant changes take place in the major semi-axes on time-scales ~106-107y. Both systems require times ~108 y to come close to the minimum configuration; to approach resonance to the observed precision of the Laplace relationship (3×10?4 for the Uranian case, 2×10?7 for the Jovian case) requires, for both systems, a time closely comparable with the age of the solar system. 相似文献
845.
Michael Schulz 《Astrophysics and Space Science》1974,29(1):233-242
Properties of the steady state and transient behavior of geomagnetically trapped radiation are analyzed by means of phenomenological equations that concisely summarize the operative dynamical processes. The equations provide for a realistic coupling between electromagnetic wave energy, particle intensity, and pitch-angle anisotropy in the context of the outer zone. Applications include magnetospheric enforcement of a limit on stably trapped particle flux. the smooth transition between weak pitch-angle diffusion and strong diffusion, parasitic particle precipitation by natural and man-made radio signals, natural and artificial injections of trapped radiation, and the consequences of magnetospheric cold-plasma injection. 相似文献
846.
Summary. Post-depositional detrital remanent magnetization (pDRM) is the primary means whereby many sediments acquire their palaeomagnetic signal. We have studied the acquisition of this magnetization in a variety of natural sediments. Our technique involves determining the magnetic direction recorded by a sediment as a function of the water content present in the sediment when the sediment experiences a change in the direction of the applied magnetic field. Most of the sediments used in this study were collected wet from natural environments and were preserved in their original state until they were used in the experiments. Grain sizes were measured by the settling tube method which led to the determination of the clay, silt and sand fractions in each sediment. Isothermal remanent magnetization acquisition studies indicated that the predominant magnetic carriers were magnetite. In the pDRM acquisition studies two distinct modes of behaviour were found. For sediments with a sand content less than 60 per cent, the original direction of magnetization was preserved regardless of the water content. Such behaviour is not consistent with a theoretical model which assumes that at high water contents the magnetic carriers remain mobile within fluid-filled voids and hence are able to realign along a new magnetic field direction. For sediments with a sand content in excess of 60%, remagnetization along a new magnetic field direction occurred as expected, provided the sediments were sufficiently wet. Studies of natural sediments and corresponding samples of dried and reconstituted sediments have demonstrated that the magnetic characterization of a sediment can be reliably determined even for older, desiccated sediments. 相似文献
847.
Accepted practice dictates that waterflooding of gas reservoirs should commence, if ever, only when the reservoir pressure has declined to the minimum production pressure. Analytical proof of this hypothesis has yet to appear in the literature however. This paper considers a model for a gas-water reservoir with a variable production rate and enhanced recovery with waterflooding and, using an initial dynamic programming approach, confirms the above hypothesis. 相似文献
848.
The determination of the brightness temperature of Venus near 1.35 cm wavelength is reviewed. The observed brightness temperature is compared with models for the microwave emission based on the physical and chemical structure of the atmosphere as obtained from spacecraft. Upper limits are set on the concentrations of microwave-absorbing minor constituents. In particular, upper limits are determined for SO2 (180 ppm) and H2O (0.3%) for a mixing-ratio profile that is uniformly mixed up to the cloud bottom at 50 km and is rapidly depleted ( at higher altitudes. The total optical depth of the cloud region at or above 50 km is <0.17 at 1.35 cm wavelength. The SO2 upper limit is only in marginal agreement with the spacecraft results, and it may be that the latter have been overestimated, or that the distribution of SO2 is more complex than given by the uniform mixing model. 相似文献
849.
Summary. Travel times for central Asia studied by Gogna, Jeffreys and Shimshoni are modified. Corrected surface times of P and S are tabulated and a structure is computed. We tabulate also full travel-time tables for all usual depths of focus. 相似文献
850.
Michael Anthony Velbel 《Meteoritics & planetary science》1988,23(2):151-159
Abstract— The distribution of white evaporitic deposits differs among different meteorite compositional groups and weathering categories of Antarctic meteorites. Evaporites occur with unusual frequency on carbonaceous chondrites, and are especially common in carbonaceous chondrites of weathering categories A and B. Among achondrites, weathering categories A and A/B show the most examples of evaporite weathering. Unlike carbonaceous chondrites and achondrites, most evaporite-bearing ordinary (H and L) chondrites are from rustier meteorites of weathering categories B and, to a lesser degree, B/C and C. LL chondrites are conspicuous by their complete lack of any evaporitic weathering product. Almost two-thirds of all evaporite-bearing meteorites belong to weathering categories A, A/B, and B. Where chemical data are available, surficial evaporite deposits are associated with elemental anomalies in meteorite interiors. Meteorites of weathering classes B, A/B, and even A may have experienced significant element redistribution and/or contamination as a result of terrestrial exposure. Evaporite formation during terrestrial weathering cannot be neglected in geochemical, cosmochemical, and mineralogical studies of Antarctic meteorites. A lower-case “e” should be added to the weathering classification of evaporite-bearing Antarctic meteorites, to inform meteorite scientists of the presence of evaporite deposits and their associated compositional effects. 相似文献