全文获取类型
收费全文 | 70984篇 |
免费 | 1401篇 |
国内免费 | 657篇 |
专业分类
测绘学 | 1714篇 |
大气科学 | 5029篇 |
地球物理 | 14220篇 |
地质学 | 25232篇 |
海洋学 | 6179篇 |
天文学 | 16332篇 |
综合类 | 208篇 |
自然地理 | 4128篇 |
出版年
2022年 | 396篇 |
2021年 | 699篇 |
2020年 | 777篇 |
2019年 | 830篇 |
2018年 | 1895篇 |
2017年 | 1759篇 |
2016年 | 2240篇 |
2015年 | 1319篇 |
2014年 | 2179篇 |
2013年 | 3768篇 |
2012年 | 2277篇 |
2011年 | 3118篇 |
2010年 | 2605篇 |
2009年 | 3504篇 |
2008年 | 3255篇 |
2007年 | 3045篇 |
2006年 | 2876篇 |
2005年 | 2353篇 |
2004年 | 2253篇 |
2003年 | 2110篇 |
2002年 | 1927篇 |
2001年 | 1801篇 |
2000年 | 1717篇 |
1999年 | 1379篇 |
1998年 | 1471篇 |
1997年 | 1387篇 |
1996年 | 1101篇 |
1995年 | 1142篇 |
1994年 | 962篇 |
1993年 | 874篇 |
1992年 | 855篇 |
1991年 | 760篇 |
1990年 | 856篇 |
1989年 | 717篇 |
1988年 | 650篇 |
1987年 | 814篇 |
1986年 | 663篇 |
1985年 | 856篇 |
1984年 | 922篇 |
1983年 | 862篇 |
1982年 | 831篇 |
1981年 | 707篇 |
1980年 | 663篇 |
1979年 | 607篇 |
1978年 | 604篇 |
1977年 | 552篇 |
1976年 | 540篇 |
1975年 | 499篇 |
1974年 | 506篇 |
1973年 | 468篇 |
排序方式: 共有10000条查询结果,搜索用时 15 毫秒
961.
Models of giant gaseous protoplanets calculated by DeCampli and Cameron (1979) indicate that iron and probably other minerals in the interior of a planet would be in the liquid state during part of the protoplanet evolution. Liquid drops in a protoplanet would grow by coalescence much as cloud drops in the Earth's atmosphere grow to rain drops. We have modeled this process by using the stochastic collection equation (Slattery, 1978) for various initial conditions. In all of the cases considered, the growth time (to centimeter-sized droplets) is much shorter than the time, as estimated by detailed evolutionary calculations, that the drops are in the liquid state. Brownian collection is effective in quickly coalescing tiny liquid droplets to an average radius of about 0.005 cm with very few drops remaining with radii less than 0.001 cm. For radii larger than 0.005 cm gravitational collection is dominant. Since the particles are rapidly swept from interstellar grain sizes to much larger sizes, the opacity in the cloud layer is expected to drop sharply following melting of the grains. 相似文献
962.
We searched for a variation with heliographic latitude of the solar limb effect by comparing the relative wavelengths of weak and strong Fraunhofer lines. The blue shifts associated with the limb effect appear 9%±5% larger in the polar radius vector than in an equatorial radius vector at cos = 0.5. This should perhaps be interpreted as an increase with latitude of either solar convection or of convective overshoot. Recent observations of poleward meridional flows of 30m s–1 should be corrected for this limb effect variation. This correction increases this flow velocity to 70 m s–1. A search for a similar variation in plages and in network boundaries had negative results, the variation being +1%±5% and -1%±6% respectively.Now at the Multiple Mirror Telescope Observatory, University of Arizona, Tucson, Ariz. 85721, U.S.A. The MMTO is jointly operated by the University of Arizona and the Smithsonian Institution.The Sacramento Peak Observatory is operated by the Association of Universities for Research in Astronomy, Inc. under contract AST 78-17292 with the National Science Foundation. 相似文献
963.
A localized force-free current is proposed as a model for the observed coronal loops.An upper limit for the growth rate of kink instabilities in this model is found by solving numerically, in cylinder symmetry, the MHD equation of motion, with the boundary condition = 0 outside the loop.For various current densities a spectrum of kinks is found. These instabilities will disrupt the loops that are long or strongly twisted, on a time scale of a few seconds.The kinks in short or barely twisted loops are too long to fit. 相似文献
964.
We present a simple model for the formation and growth of photochemical aerosols in the atmosphere of Titan. We show that, in general, an optically thick layer of particles in the size range required by models of Titan cannot be obtained at pressures less than about 2 mbar. Since the thin model of Titan's atmosphere requires that the inversion not extend below pressures of 0.11 mbar (D. M. Hunten and J. J. Caldwell, 1978, preprint), it seems to be ruled out by the calculations. 相似文献
965.
The radiative heat flux from 0.1 to 10 bars is estimated on the basis of a “two-cloud” scattering model that fits available spectral data and Pioneer photometry. Deeper than a few bars, the flux is 4.5 W m?2, compared with the 18.8 W m?2 used in an earlier study by Trafton and Stone. A temperature profile is computed, with the H2 pressure-induced opacity; the temperature at 1 bar is found to be 156°K, rather than the commonly accepted 170°K. An additional optical depth of unity at the 0.67-bar level could restore the conventional value; otherwise a considerably cooler atmosphere is a serious possibility. 相似文献
966.
E. M. Drobyshevski 《Earth, Moon, and Planets》1980,23(4):483-491
The hypothesis considering the Jupiter-Sun system as a limiting case of a close binary star implies the initial relative ice abundances in all the Galilean satellites to be essentially equal. The satellites move in the Jovian magnetosphere; thus the unipolar current flowing through their bodies subjected their ices to volumetric electrolysis. Explosions of the electrolysis products resulted in a loss of ices. While Callisto did not explode at all, Ganymede exploded once, Europa twice, and Io two or three times. An analysis of the magnetic field changes needed to create the modern ice abundances in the satellite shows:
- the initial field of Jupiter was ~102 times stronger when compared with the present-day field, and
- the field had to decrease exponentially with τ2| ≈ (0.6?1), which means its relic nature.
967.
Gentileschi ML 《Rivista geografica italiana》1980,87(1):61-74
The author reviews a selection of studies on the behavioral aspects of migration, with emphasis on the process leading up to the decision to migrate. The focus of this review is not on the short-term factors leading to the actual migration decision but on the background factors that lead to the contemplation of migration. The perception by potential migrants of the environment in which they are living as opposed to that of the place to which they might move is considered. (summary in ENG, GER) 相似文献
968.
In the first part, the authors review a group of studies dealing with the identification of regional differences in Italian migratory patterns, especially using the concept of migration field. The second part is devoted to a study of the hierarchical clustering of Italian provinces using 1973 inter-provincial migratory flow data. (summary in ENG, FRE) 相似文献
969.
970.
Green's Theorem is developed for the spherically-symmetric steady-state cosmic-ray equation of transport in interplanetary space. By means of it the momentum distribution functionF
o(r,p), (r=heliocentric distance,p=momentum) can be determined in a regionr
arrbwhen a source is specified throughout the region and the momentum spectrum is specified on the boundaries atr
a
andr
b
. Evaluation requires a knowledge of the Green's function which corresponds to the solution for monoenergetic particles released at heliocentric radiusr
o
, Examples of Green's functions are given for the caser
a
=0,r
b
= and derived for the cases of finiter
a
andr
b
. The diffusion coefficient is assumed of the form = o(p)r
b
. The treatment systematizes the development of all analytic solutions for steady-state solar and galactic cosmic-ray propagation and previous solutions form a subset of the present solutions. 相似文献