全文获取类型
收费全文 | 1263篇 |
免费 | 86篇 |
国内免费 | 18篇 |
专业分类
测绘学 | 62篇 |
大气科学 | 103篇 |
地球物理 | 327篇 |
地质学 | 363篇 |
海洋学 | 89篇 |
天文学 | 285篇 |
综合类 | 2篇 |
自然地理 | 136篇 |
出版年
2023年 | 1篇 |
2022年 | 1篇 |
2021年 | 32篇 |
2020年 | 31篇 |
2019年 | 38篇 |
2018年 | 51篇 |
2017年 | 36篇 |
2016年 | 47篇 |
2015年 | 49篇 |
2014年 | 48篇 |
2013年 | 76篇 |
2012年 | 61篇 |
2011年 | 68篇 |
2010年 | 54篇 |
2009年 | 84篇 |
2008年 | 66篇 |
2007年 | 64篇 |
2006年 | 75篇 |
2005年 | 68篇 |
2004年 | 67篇 |
2003年 | 55篇 |
2002年 | 52篇 |
2001年 | 43篇 |
2000年 | 27篇 |
1999年 | 34篇 |
1998年 | 31篇 |
1997年 | 12篇 |
1996年 | 11篇 |
1995年 | 11篇 |
1994年 | 10篇 |
1993年 | 8篇 |
1992年 | 4篇 |
1991年 | 6篇 |
1990年 | 1篇 |
1989年 | 6篇 |
1988年 | 6篇 |
1987年 | 4篇 |
1986年 | 6篇 |
1985年 | 3篇 |
1984年 | 4篇 |
1983年 | 3篇 |
1982年 | 1篇 |
1981年 | 4篇 |
1980年 | 3篇 |
1979年 | 3篇 |
1978年 | 1篇 |
1975年 | 1篇 |
排序方式: 共有1367条查询结果,搜索用时 421 毫秒
971.
新疆叶城晚新生代山前盆地演化与高原北缘的隆升—Ⅰ地层学与岩石学证据 总被引:21,自引:2,他引:19
叶城晚新生代山前盆地的岩性主要由中新世的细粒泥岩和砂岩(乌恰群),上新世的砂岩夹薄层砾岩(阿图什组)及上新世-更新世的粗粒砾岩(西域组)构成。中新世的沉积以细颗粒泥砂岩为主,表明物源区较远,古流域坡度较小,搬运距离较长。古流向分析显示物源区位于南和偏南方,此时昆仑山的地势起伏尚不大。到上新世的阿图什组沉积时,开始出现砾石沉积,反映西昆仑山已经开始有规模地隆升。西域砾岩的沉积标志着作为物源区的西昆仑山民有相当的高度,随着山系的隆升,基底岩石被暴露和剥蚀。 相似文献
972.
973.
On the redshift cut-off for steep-spectrum radio sources 总被引:1,自引:0,他引:1
Matt J. Jarvis Steve Rawlings Chris J. Willott Katherine M. Blundell Steve Eales Mark Lacy 《Monthly notices of the Royal Astronomical Society》2001,327(3):907-917
We use three samples (3CRR, 6CE and 6C*) selected at low radio frequency to constrain the cosmic evolution in the radio luminosity function (RLF) for the 'most luminous' steep-spectrum radio sources. Though intrinsically rare, such sources give the largest possible baseline in redshift for the complete flux-density-limited samples currently available. Using parametric models to describe the RLF, incorporating distributions in radio spectral shape and linear size, as well as the usual luminosity and redshift, we find that the data are consistent with a constant comoving space density between and . We find that this model is favoured over a model with similar evolutionary behaviour to that of optically selected quasars (i.e., a roughly Gaussian distribution in redshift) with probability ratios of and for spatially flat cosmologies with and respectively. Within the uncertainties, this evolutionary behaviour may be reconciled with the shallow decline preferred for the comoving space density of flat-spectrum sources by Dunlop & Peacock and Jarvis & Rawlings, in line with the expectations of unified schemes. 相似文献
974.
Chris Koen 《Monthly notices of the Royal Astronomical Society》2005,360(3):1132-1142
The results of more than 100 h of CCD photometric monitoring of 10 L dwarfs and two T dwarfs are presented. Reasonable evidence is shown for I C band variability in DENIS 0255−4700, DENIS 1705−0516 and 2M 2104−1037. Substantial brightening of the T dwarf binary ε Indi Bab was observed over the course of 3.6 h; it is unlikely that this could have been caused by surface spots. No unequivocal variability could be detected in the R C band. 相似文献
975.
Chris Koen 《Monthly notices of the Royal Astronomical Society》2001,325(4):1335-1340
The observation of flux sources near the limit of detection requires a careful evaluation of possible biases in magnitude determination. Both the traditional logarithmic magnitudes and the recently proposed inverse hyperbolic sine (asinh) magnitudes are considered. Formulae are derived for three different biasing mechanisms: the statistical spread of the observed flux values arising from e.g. measurement error; the dependence of these errors on the true flux; and the dependence of the observing probability on the true flux. As an example of the results, it is noted that biases at large signal-to-noise ratios R , at which the two types of magnitude are similar, are of the order of −( p +1)/ R 2 , where the exponent p parametrizes a power-law dependence of the probability of observation on the true flux. 相似文献
976.
Shaun Cole Peder Norberg Carlton M. Baugh Carlos S. Frenk Joss Bland-Hawthorn Terry Bridges Russell Cannon Matthew Colless Chris Collins Warrick Couch Nicholas Cross Gavin Dalton Roberto De Propris Simon P. Driver George Efstathiou Richard S. Ellis Karl Glazebrook Carole Jackson Ofer Lahav Ian Lewis Stuart Lumsden Steve Maddox Darren Madgwick John A. Peacock Bruce A. Peterson Will Sutherland Keith Taylor 《Monthly notices of the Royal Astronomical Society》2001,326(1):255-273
977.
Christopher Thom Chris Flynn Michael S. Bessell Jyrki Hänninen Timothy C. Beers Norbert Christlieb Dionne James Johan Holmberg Brad K. Gibson 《Monthly notices of the Royal Astronomical Society》2005,360(1):354-359
Large samples of field horizontal branch (FHB) stars make excellent tracers of the Galactic halo; by studying their kinematics, one can infer important physical properties of our Galaxy. Here we present the results of a medium-resolution spectroscopic survey of 530 FHB stars selected from the Hamburg/ESO survey. The stars have a mean distance of ∼7 kpc and thus probe the inner parts of the Milky Way halo. We measure radial velocities from the spectra in order to test the model of Sommer-Larsen et al., who suggested that the velocity ellipsoid of the halo changes from radially dominated orbits to tangentially dominated orbits as one proceeds from the inner to the outer halo. We find that the present data are unable to discriminate between this model and a more simple isothermal ellipsoid; we suggest that additional observations towards the Galactic Centre might help to differentiate them. 相似文献
978.
979.
The Buffalo Hills kimberlites define a province of kimberlite magmatism occurring within and adjacent to Proterozoic crystalline basement termed the Buffalo Head Terrane in north-central Alberta, Canada. The kimberlites are distinguished by a diverse xenocryst suite and most contain some quantity of diamond. The xenocryst assemblage in the province is atypical for diamondiferous kimberlite, including an overall paucity of mantle indicator minerals and the near-absence of compositionally subcalcic peridotitic garnet (G10). The most diamond-rich bodies are distinguished by the presence of slightly subcalcic, chromium-rich garnet and the general absence of picroilmenite, with the majority forming a small cluster in the northwestern part of the province. Barren and near-barren pipes tend to occur to the south, with increasing proximity to the basement structure known as the Peace River Arch. Niobian picroilmenite, compositionally restricted low-to moderate-Cr peridotitic garnet, and megacrystal titanian pyrope occur in kimberlites closest to the arch. Major element data for clinopyroxene and trace element data for garnet from diamond-rich and diamond-poor kimberlites suggests that metasomatism of lithospheric peridotite within the diamond stability field may have caused destruction of diamond, and diamond source rocks proximal to the arch were the most affected. 相似文献
980.
Asymptotic methods provide an efficient way to compute seismograms in heterogeneous media. However, zeroth-order ray theory, the simplest of the asymptotic methods, often fails because of the presence of caustics. Maslov theory is an extension of zeroth-order ray theory, which gives a uniformly valid expression of the wavefield everywhere, including the caustics. This result is given in terms of an integral of ray data over one or two ray parameters. It is shown in this paper how geometrical arrivals are constructed in the one and two-parameter Maslov integrals.In practice Maslov seismograms have been computed using only one ray parameter. However, in three-dimensional media two parameters are needed to uniquely define a ray. In this paper we present an efficient algorithm to compute two-parameter Maslov integrals. The Maslov integral is evaluated by computing the frequency-to-time Fourier transform prior to integration over the ray parameters. The wavefield is then discretized by smoothing with a boxcar function. The resulting expression, which only requires the results of ordinary kinematic and dynamic ray tracing, cen be computed efficiently and robustly. A numerical example is given that illustrates the use of this algorithm. 相似文献