全文获取类型
收费全文 | 1129篇 |
免费 | 38篇 |
国内免费 | 23篇 |
专业分类
测绘学 | 25篇 |
大气科学 | 132篇 |
地球物理 | 280篇 |
地质学 | 361篇 |
海洋学 | 107篇 |
天文学 | 175篇 |
综合类 | 9篇 |
自然地理 | 101篇 |
出版年
2024年 | 4篇 |
2023年 | 8篇 |
2022年 | 8篇 |
2021年 | 19篇 |
2020年 | 26篇 |
2019年 | 30篇 |
2018年 | 34篇 |
2017年 | 49篇 |
2016年 | 36篇 |
2015年 | 37篇 |
2014年 | 47篇 |
2013年 | 73篇 |
2012年 | 38篇 |
2011年 | 69篇 |
2010年 | 56篇 |
2009年 | 79篇 |
2008年 | 68篇 |
2007年 | 61篇 |
2006年 | 56篇 |
2005年 | 39篇 |
2004年 | 43篇 |
2003年 | 34篇 |
2002年 | 24篇 |
2001年 | 19篇 |
2000年 | 24篇 |
1999年 | 18篇 |
1998年 | 15篇 |
1997年 | 19篇 |
1996年 | 17篇 |
1995年 | 18篇 |
1994年 | 9篇 |
1993年 | 10篇 |
1992年 | 7篇 |
1991年 | 9篇 |
1990年 | 8篇 |
1989年 | 5篇 |
1988年 | 6篇 |
1987年 | 7篇 |
1986年 | 4篇 |
1985年 | 7篇 |
1984年 | 6篇 |
1983年 | 9篇 |
1982年 | 5篇 |
1981年 | 5篇 |
1980年 | 3篇 |
1979年 | 4篇 |
1978年 | 5篇 |
1977年 | 2篇 |
1976年 | 5篇 |
1967年 | 1篇 |
排序方式: 共有1190条查询结果,搜索用时 15 毫秒
51.
52.
Kevin Hall 《地球表面变化过程与地形》1982,7(1):45-51
Volcanic activity on sub-Antarctic Marion Island is found to have occurred only during the interglacials. The present volcano distribution is associated with a radial and peripheral fault system, the location of which appears to be related to the former glacier distribution. An hypothesis is presented suggesting that the faulting is a result of deglaciation and that the specific location of the faults is due to the differential stresses occurring between ice-covered and ice-free areas during isostatic uplift. The faulting initiates volcanism due to the location of the island within a volcanic region. 相似文献
53.
Pasachoff Jay M. Babcock Bryce A. Russell Kevin D. Seaton Daniel B. 《Solar physics》2002,207(2):241-257
As a part of a study of the cause of solar coronal heating, we searched for high-frequency (1 Hz) intensity oscillations in coronal loops in the [Fexiv] coronal green line. We summarize results from observations made at the 11 August 1999 total solar eclipse from Râmnicu-Vâlcea, Romania, through clear skies. We discuss the image reduction and analysis through two simultaneous series of coronal CCD images digitized at 10 Hz for a total time of about 140 s. One series of images was taken through a 3.6 Å filter isolating the 5303 Å[Fexiv] coronal green line and the other through a 100 Å filter in the nearby K-corona continuum. Previous observations, described in Pasachoff et al. (2000), showed no evidence for oscillations in the [Fexiv] green line at a level greater than 2% of coronal intensity. We describe several improvements made over the 1998 eclipse that led to increased image clarity and sensitivity. The corona was brighter in 1999 with the solar maximum, further improving the data. We use Fourier analysis to search in the [Fexiv] channel for intensity oscillations in loops at the base of the corona. Such oscillations in the 1-Hz range are predicted as a result of density fluctuations from the resonant absorption of MHD waves. The dissipation of a significant amount of mechanical energy from the photosphere into the corona through this mechanism could provide sufficient energy to heat the corona. A Monte Carlo model of the data suggests the presence of enhanced power, particularly in the 0.75–1.0 Hz range, and we conclude that MHD waves remain a viable method for coronal heating. 相似文献
54.
Kevin T. Kilty 《Tectonophysics》1981,77(3-4)
Analytic solutions to the stress fields resulting from the San Andreas and Queen Charlotte transform faults may be found by applying conformal mappings to the generalized plane stress solution of stresses in a half-plane. The mean stress fields (one-half the trace of the stress tensor) found in this manner show a similarity to the deformation found in western Canada and the western United States. The results refute the hypothesis that Alaska acts as a continental buttress against deformation of the Canadian Cordillera. Moreover, these results imply that the differences in the tectonics of major transform boundaries are caused primarily by differences in lithospheric structure and differences in stress distribution along the plate boundaries. 相似文献
55.
56.
Lisa Cheong Susanne Bleisch Allison Kealy Kevin Tolhurst Tom Wilkening Matt Duckham 《International journal of geographical information science》2016,30(7):1377-1404
The paper investigates whether the methods chosen for representing uncertain geographic information aid or impair decision-making in the context of wildfire hazard. Through a series of three human subject experiments, utilizing 180 subjects and employing increasingly difficult tasks, this research evaluates the effect of five different visualizations and a text-based representation on decision-making under uncertainty. Our quantitative experiments focus specifically on the task of decision-making under uncertainty, rather than the task of reading levels of uncertainty from the map. To guard against the potential for generosity and risk seeking in decision-making under uncertainty, the experimental design uses performance-based incentives. The experiments showed that the choice of representation makes little difference to performance in cases where subjects are allowed the time and focus to consider their decisions. However, with the increasing difficulty of time pressure, subjects performed best using a spectral color hue-based representation, rather than more carefully designed cartographic representations. Text-based and simplified boundary encodings were among the worst performers. The results have implications for the performance of decision-making under uncertainty using static maps, especially in the stressful environments surrounding an emergency. 相似文献
57.
Kevin P. Rauch & Brian Ingalls 《Monthly notices of the Royal Astronomical Society》1998,299(4):1231-1241
It has recently been shown by Rauch 38 Tremaine that the rate of angular momentum relaxation in nearly Keplerian star clusters is greatly increased by a process termed 'resonant relaxation'; it was also argued, via a series of scaling arguments, that tidal disruption of stars in galactic nuclei containing massive black holes could be noticeably enhanced by this process. We describe here the results of numerical simulations of resonant tidal disruption which quantitatively test the predictions made by Rauch 38 Tremaine. The simulation method is based on an N -body routine incorporating cloning of stars near the loss cone and a semirelativistic symplectic integration scheme. Normalized disruption rates for resonant and non-resonant nuclei are derived at orbital energies both above and below the critical energy, and the corresponding angular momentum distribution functions are found. The black hole mass above which resonant tidal disruption is quenched by relativistic precession is determined. We also briefly describe the discovery of chaos in the Wisdom–Holman symplectic integrator applied to highly eccentric orbits and propose a modified integration scheme that remains robust under these conditions. We find that resonant disruption rates exceed their non-resonant counterparts by an amount consistent with the predictions; in particular, we estimate the net tidal disruption rate for a fully resonant cluster to be about twice that of its non-resonant counterpart. No significant enhancement in rates is observed outside the critical radius. Relativistic quenching of the effect is found to occur for hole masses M > M Q = (8 ± 3) × 107 M . The numerical results combined with the observed properties of galactic nuclei indicate that for most galaxies the resonant enhancement to tidal disruption rates will be very small. 相似文献
58.
Kevin Schawinski 《Monthly notices of the Royal Astronomical Society》2009,397(2):717-725
The time delay between the formation of the progenitor systems of Type Ia supernovae (SNe Ia) and their detonation is a vital discriminant between the various progenitor scenarios that have been proposed for them. We use Sloan Digital Sky Survey optical and Galaxy Evolution Explorer ( GALEX ) ultraviolet observations of the early-type host galaxies of 21 nearby SNe Ia and quantify the presence or absence of any young stellar population to constrain the minimum time delay for each supernova. We find that early-type host galaxies lack 'prompt' SNe Ia with time delays of ≲100 Myr and that ∼70 per cent SNe Ia have minimum time delays of 275 Myr–1.25 Gyr, with a median of 650 Myr, while at least 20 per cent SNe Ia have minimum time delays of at least 1 Gyr at 95 per cent confidence and two of these four SNe Ia are likely older than 2 Gyr. The distribution of minimum time delays observed matches most closely the expectation for the single-degenerate channel with a main sequence donor. Furthermore, we do not find any evidence that subluminous SNe Ia are associated with long time delays. 相似文献
59.
Pin-Song Zhao Hong Wu Cong Kevin Xu Ming Yang Fan Yang Yi-Nan Zhu Man I Lam Jun-Jie Jin Hai-Long Yuan Hao-Tong Zhang Shi-Yin Shen Jian-Rong Shi A-Li Luo Xue-Bing Wu Yong-Heng Zhao Yi-Peng Jing 《天文和天体物理学研究(英文版)》2019,(8)
We present optical luminosity functions(LFs) of galaxies in the~(0.1) g,~(0.1) r,~(0.1) i bands, calculated using data in~40 deg~2 sky area of the LAMOST Complete Spectroscopic Survey of Pointing Area(LaCoSSPAr) in the Southern Galactic Cap. Redshifts for galaxies brighter than r = 18.1 were obtained mainly with LAMOST. In each band, LFs derived using both parametric and non-parametric maximum likelihood methods agree well with each other. In the0.1 r band, our fitting parameters of the Schechter function are φ_*=(1.65 ± 0.36) × 10~(-2) h~3 Mpc~(-3), M_*=-20.69 ± 0.06 mag and α =-1.12 ± 0.08,which agree with previous studies. Separate LFs are also derived for emission line galaxies and absorption line galaxies. The LFs of absorption line galaxies show a dip at~(0.1) r ~18.5 and can be fitted well by a double-Gaussian function, suggesting a bimodality in passive galaxies. 相似文献
60.
Kevin R. T. Whelan Thomas J. Smith Donald R. Cahoon James C. Lynch Gordon H. Anderson 《Estuaries and Coasts》2005,28(6):833-843
We measured monthly soil surface elevation change and determined its relationship to groundwater changes at a mangrove forest
site along Shark River, Everglades National Park, Florida. We combined the use of an original design, surface elevation table
with new rod-surface elevation tables to separately track changes in the mid zone (0–4 m), the shallow root zone (0–0.35 m),
and the full sediment profile (0–6 m) in response to site hydrology (daily river stage and daily groundwater piezometric pressure).
We calculated expansion and contraction for each of the four constituent soil zones (surface [accretion and erosion; above
0 m], shallow zone [0–0.35 m], middle zone [0.35–4 m], and bottom zone [4–6]) that comprise the entire soil column. Changes
in groundwater pressure correlated strongly, with changes in soil elevation for the entire profile (Adjusted R2 = 0.90); this relationship was not proportional to the depth of the soil profile sampled. The change in thickness of the
bottom soil zone accounted for the majority (R2 = 0.63) of the entire soil profile expansion and contraction. The influence of hydrology on specific soil zones and absolute
elevation change must be considered when evaluating the effect of disturbances, sea level rise, and water management decisions
on coastal wetland systems. 相似文献