全文获取类型
收费全文 | 263822篇 |
免费 | 5836篇 |
国内免费 | 5707篇 |
专业分类
测绘学 | 7777篇 |
大气科学 | 20232篇 |
地球物理 | 55062篇 |
地质学 | 93315篇 |
海洋学 | 22417篇 |
天文学 | 56297篇 |
综合类 | 1660篇 |
自然地理 | 18605篇 |
出版年
2021年 | 2727篇 |
2020年 | 3005篇 |
2019年 | 3333篇 |
2018年 | 3809篇 |
2017年 | 3470篇 |
2016年 | 6084篇 |
2015年 | 4684篇 |
2014年 | 7446篇 |
2013年 | 14732篇 |
2012年 | 6986篇 |
2011年 | 8179篇 |
2010年 | 7222篇 |
2009年 | 9848篇 |
2008年 | 8702篇 |
2007年 | 8081篇 |
2006年 | 10016篇 |
2005年 | 7981篇 |
2004年 | 7858篇 |
2003年 | 7265篇 |
2002年 | 6859篇 |
2001年 | 6150篇 |
2000年 | 6089篇 |
1999年 | 5378篇 |
1998年 | 5346篇 |
1997年 | 5158篇 |
1996年 | 4794篇 |
1995年 | 4519篇 |
1994年 | 4178篇 |
1993年 | 3902篇 |
1992年 | 3687篇 |
1991年 | 3641篇 |
1990年 | 3790篇 |
1989年 | 3551篇 |
1988年 | 3329篇 |
1987年 | 3857篇 |
1986年 | 3422篇 |
1985年 | 4245篇 |
1984年 | 4749篇 |
1983年 | 4421篇 |
1982年 | 4327篇 |
1981年 | 3938篇 |
1980年 | 3654篇 |
1979年 | 3513篇 |
1978年 | 3491篇 |
1977年 | 3283篇 |
1976年 | 3047篇 |
1975年 | 2959篇 |
1974年 | 2915篇 |
1973年 | 3072篇 |
1972年 | 2023篇 |
排序方式: 共有10000条查询结果,搜索用时 15 毫秒
991.
This paper is designed to bring to the attention the fact that the effect of focusing of solar energetic particles is always essential as compared with scattering, no matter how small the value of the mean free path may be. That is why, an ordinary (focusing-free) diffusion approach can not be applied to the solar cosmic ray transport. In the case of high-energy solar particles, the focused diffusion is demonstrated to lead to a power law decay of energetic particle intensity much like an ordinary diffusion. However, the power law index of the decay is renormalized by the focusing. 相似文献
992.
C. E. Alissandrakis F. Borgioli F. Chiuderi Drago M. Hagyard K. Shibasaki 《Solar physics》1996,167(1-2):167-179
The solar active region (AR) 7530 was observed at 6 cm on July 3 and 4, 1993 with the Westerbork Synthesis Radio Telescope, using a multi-channel receiver with very narrow bandwidth. We compare the radio data with Yohkoh SXT observations and with the magnetic field extrapolated from the Marshall vector magnetograms in the force-free and current-free approximations. The comparison with soft X-rays shows that, although a general agreement exists between the shape of the radio intensity map and the X-ray loops, the brightness temperature, T
b, obtained using the parameters derived from the SXT is much lower than that observed. The comparison with the extrapolated photospheric fields shows instead that they account very well for the observed T
b above the main sunspots, if gyroresonance emission is assumed. In the observation of July 4 an inversion and strong suppression of the circular polarization was clearly present above different portions of the AR, which indicates that particular relationships exist between the electron density and the magnetic field in the region where the corresponding lines of sight cross the field quasi-perpendicularly. The extrapolated magnetic field at a much higher level ( 1010 cm), satisfies the constraints required by the wave propagation theory all over the AR. However, a rather low electron density is derived. 相似文献
993.
A wind tunnel study of turbulent flow around single and multiple windbreaks, part I: Velocity fields 总被引:10,自引:5,他引:5
This paper describes wind-tunnel experiments on the flow around single and multiple porous windbreaks (height H), sheltering a model plant canopy (height H/3). The mean wind is normal to the windbreaks, which span the width of the wind tunnel. The incident turbulent flow simulates the adiabatic atmospheric surface layer. Five configurations are examined: single breaks of three solidities (low, medium, high; solidity = 1 - porosity), and medium-solidity multiple breaks of streamwise spacing 12H and 6H. The experimental emphases are on the interactions of the windbreak flow with the underlying plant canopy; the effects of solidity; the differences in shelter between single and multiple windbreaks; and the scaling properties of the flow. Principal results are: (1) the "quiet zones" behind each windbreak are smaller in multiple than single arrays, because of the higher turbulence level in the very rough-wall internal boundary layer which develops over the multiple arrays. Nevertheless, the overall shelter effectiveness is higher for multiple arrays than single windbreaks because of the "nonlocal shelter" induced by the array as a whole. (2) The flow approaching the windbreak decelerates above the canopy but accelerates within the canopy, particularly when the windbreak solidity is high. (3) A strong mixing layer forms just downwind of the top of each windbreak, showing some of the turbulence and scaling properties of the classical mixing layer formed between uniform, coflowing streams. (4) No dramatic increase in turbulence levels in the canopy is evident at the point where the deepening mixing layer contacts the canopy (around x/H = 3) but the characteristic inflection in the canopy wind profile is eliminated at this point. 相似文献
994.
Turbulent fluctuations have been investigated in the internal boundary layer (IBL) which forms after a dry-to-wet surface transition. The IBL is defined as that part of the atmospheric surface layer where the influence of the downstream surface is noticeable. The results of the application of three different quadrant analysis techniques are presented. The three techniques, in increasing order of the amount of information supplied, provide:
- the diurnal variation of quadrant contribution (C i), number fraction (T i) and conditional average (% MathType!MTEF!2!1!+-% feaafeart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXafv3ySLgzGmvETj2BSbqefm0B1jxALjhiov2D% aebbfv3ySLgzGueE0jxyaibaiiYdd9qrFfea0dXdf9vqai-hEir8Ve% ea0de9qq-hbrpepeea0db9q8as0-LqLs-Jirpepeea0-as0Fb9pgea% 0lrP0xe9Fve9Fve9qapdbaqaaeGacaGaaiaabeqaamaabaabcaGcba% GaeyykJeUabm4DayaafaGabm4CayaafaGaeyOkJe-aaSbaaSqaaiaa% dMgaaeqaaaaa!4215!\[\langle w's'\rangle _i \], with s = T or q) of vertical sensible and latent heat fluxes,
- the quadrant contribution and number of samples of different sizes depending on the relative magnitude of each sample, and
- the distribution of the nondimensional probability density function.
995.
N. Ya. Sotnikova 《Astrophysics》1996,39(2):141-152
Computer programs developed to study large-scale, transient gas structures in galaxies are described and test results are given. Gas-dynamic quantities are determined on the basis of a three-dimensional algorithm using so-called "smoothed particle hydrodynamics" (SPH). Preliminary calculations were made to simulate the formation of a gas ring around a spheroidal galaxy when it absorbs a low-mass, gas-rich companion, as well due to gas accretion during the flyby of a spiral galaxy of comparable mass. The evolution of tidal gas tails of disk galaxies is investigated.Translated from Astrofizika, Vol. 39, No. 2, pp. 265–284, April–June, 1996. 相似文献
996.
Richard A. Serafin 《Celestial Mechanics and Dynamical Astronomy》1996,65(4):389-398
We deal here with the efficient starting points for Kepler's equation in the special case of nearly parabolic orbits. Our approach provides with very simple formulas that allow calculating these points on a scientific vest-pocket calculator. Moreover, srtarting with these points in the Newton's method we can calculate a root of Kepler's equation with an accuracy greater than 0.001 in 0–2 iterations. This accuracy holds for the true anomaly || 135° and |e – 1| 0.01. We explain the reason for this effect also.Dedicated to the memory of Professor G.N. Duboshin (1903–1986). 相似文献
997.
An H filament eruption on November 5, 1992 was fully observed in H with the Hida Flare Monitoring Telescope, while Yohkoh's Soft X-ray Telescope observed the pre- and post-eruption evolution of the coronal magnetic fields. From the H data, including the red and blue wings, we have reconstructed the rise of the filament, including trajectory, velocity, and acceleration. In combination with the Yohkoh data this reconstruction suggests that the filament had several interactions with other coronal magnetic fields during the eruption. The Yohkoh data also shows pre-eruption changes in the coronal fields and several post-eruption bright coronal structures. The pre-eruption changes are interpreted as a partial opening of the corona, indicating that it is not necessary to have a complete opening of the corona in order for a filament to erupt and we discuss the several possible contributions from emerging flux. The post-event bright coronal structures are compared with theory and with a cleaner filament eruption event on July 31, 1992. These comparisons suggest that, although there are many similarities, it is hard to completely reconcile the observations with the existing theory. 相似文献
998.
We have obtained images in solar coronal emission lines under high sky-background conditions by making precise differential measurements between the coronal emission line and the near-by continuum, which is primarily due to scattered light from the solar disk. Chopping between the two wavelengths was performed at 100 kHz to avoid artifacts from fast-flying dust particles and other aerosols, and also from seeing effects. The differential signal was detected with a novel CCD camera that demodulates signals up to 100 kHz. These preliminary observations show coronal emission at the 0.2% level of the scattered-light background and pave the way to efficient and precise imaging of coronal emission features under less than ideal coronal-sky conditions.Operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. 相似文献
999.
The problem to compute the magnetic field above the chromosphere using data of the vector = B
t/Bt that gives the projected field direction can be solved with different approximations. The field of direction vectors is, however, not the only field accessible to observations. The Stokes parameters, which are components of the radiation tensor, can be measured at each point of the image plane. The directions of the eigenvectors of the radiation tensor define two mutually orthogonal systems of integral curves in the image plane. These families of curves have singular points, which are generally of different type than those of the vector field. When the morphology of H chromospheric fibrils are used to infer the topology of the magnetic field, a similar problem is met, suggesting that singular points should also be present there. 相似文献
1000.
The purpose of this paper is to find correlation between OI 6300 Å line intensity with solar and ionospheric parameters. A critical study have been made and the following important results are obtained:
相似文献
(i) | Solar flare index plays more important role for the emissions of 6300 Å line than other solar parameters. |
(ii) | Intensity of 6300 Å line increases linearly with the increase of solar flare index. |
(iii) | Virtual height plays more important role than critical frequency for the emission of 6300 Å line-intensity. |
(iv) | Possible explanation of this type of variation is also presented. |