全文获取类型
收费全文 | 43701篇 |
免费 | 1504篇 |
国内免费 | 1203篇 |
专业分类
测绘学 | 1219篇 |
大气科学 | 3564篇 |
地球物理 | 9876篇 |
地质学 | 16311篇 |
海洋学 | 3719篇 |
天文学 | 8643篇 |
综合类 | 425篇 |
自然地理 | 2651篇 |
出版年
2022年 | 297篇 |
2021年 | 494篇 |
2020年 | 462篇 |
2019年 | 505篇 |
2018年 | 1564篇 |
2017年 | 1429篇 |
2016年 | 1345篇 |
2015年 | 901篇 |
2014年 | 1176篇 |
2013年 | 1993篇 |
2012年 | 2008篇 |
2011年 | 2214篇 |
2010年 | 1682篇 |
2009年 | 2156篇 |
2008年 | 1832篇 |
2007年 | 1878篇 |
2006年 | 1829篇 |
2005年 | 2195篇 |
2004年 | 2297篇 |
2003年 | 1823篇 |
2002年 | 1176篇 |
2001年 | 912篇 |
2000年 | 863篇 |
1999年 | 687篇 |
1998年 | 720篇 |
1997年 | 708篇 |
1996年 | 582篇 |
1995年 | 563篇 |
1994年 | 480篇 |
1993年 | 421篇 |
1992年 | 420篇 |
1991年 | 395篇 |
1990年 | 465篇 |
1989年 | 377篇 |
1988年 | 357篇 |
1987年 | 442篇 |
1986年 | 346篇 |
1985年 | 431篇 |
1984年 | 531篇 |
1983年 | 452篇 |
1982年 | 453篇 |
1981年 | 404篇 |
1980年 | 422篇 |
1979年 | 360篇 |
1978年 | 347篇 |
1977年 | 341篇 |
1976年 | 311篇 |
1975年 | 296篇 |
1974年 | 313篇 |
1973年 | 342篇 |
排序方式: 共有10000条查询结果,搜索用时 0 毫秒
181.
182.
183.
O.?V.?YushkovaEmail author A.?L.?Gavrik V.?N.?Marchuk V.?V.?Yushkov V.?M.?Smirnov M.?A.?Laptev B.?V.?Chernyshev I.?N.?Dutyshev V.?P.?Lebedev A.?V.?Medvedev A.?A.?Petrukovich 《Solar System Research》2018,52(4):287-300
An overview of radiophysical investigations of the lunar soil and plasma shell by active radar detection with the use of spacecraft is presented. The possibility is analyzed of conducting bistatic measurements using the Irkutsk Incoherent Scattering Radar and the onboard radar system RLK-L which is being developed for the orbital station of the Luna-Resurs mission. 相似文献
184.
L. Trafton 《Icarus》1985,63(3):374-405
We report the results of monitoring Saturn's H2 quadrupole and CH4 band absorptions outside of the equatorial zone over one-half of Saturn's year. This interval covers most of the perihelion half of Saturn's elliptical orbit, which happens to be approximately bounded by the equinoxes. Marked long-term changes occur in the CH4 absorption accompanied by weakly opposite changes in the H2 absorption. Around the 1980 equinox, the H2 and CH4 absorptions in the northern hemisphere appear to be discontinuous with those in the southern hemisphere. This discontinuity and the temporal variation of the absorptions are evidence for seasonal changes. The absorption variations can be attributed to a variable haze in Saturn's troposphere, responding to changes in temperature and insolation through the processes of sublimation and freezing. Condensed or frozen CH4 is very unlikely to contribute any haze. The temporal variation of the absorption in the strong CH4 bands at south temperate latitudes is consistent with a theoretically expected phase lag of 60° between the tropopause temperature and the seasonally variable insolation. We model the vertical haze distribution of Saturn's south temperature latitudes during 1971–1977 in terms of a distribution having a particle scale height equal to a fraction of the atmospheric scale height. The results are a CH4/H2 mixing ratio of (4.2 ± 0.4) × 10?3, a haze particle albedo of , and a range of variation in the particle to gas scale-height ratio of 0.6 ± 0.2. The haze was lowest near the time of maximum temperature. We also report spatial measurements of the absorption in the 6450 Å NH3 band made annually since the 1980 equinox. A 20 ± 4% increase in the NH3 absorption at south temperate latitudes has occurred since 1973–1976 and the NH3 absorption at high northern latitudes has increased during spring. Increasing insolation, and the resulting net sublimation of NH3 crystals, is probably the cause. Significant long-term changes apparently extend to the deepest visible parts of Saturn's atmosphere. An apparently anomalous ortho-para H2 ratio in 1978 suggests that the southern temperate latitudes experienced an unusual upwelling during that time. This may have signaled a rise in the radiative-convective boundary from deep levels following maximum tropospheric temperature and the associated maximum radiative stability. This would be further evidence that the deep, visible atmosphere is governed by processes such as dynamics and the thermodynamics of phase changes, which have response times much shorter than the radiative time constant. 相似文献
185.
186.
A. Le Gall M.A. Janssen A.G. Hayes C. Savage R.D. Lorenz R.L. Kirk S. Wall E.R. Stofan the Cassini Radar Team 《Icarus》2011,213(2):608-624
Large expanses of linear dunes cover Titan’s equatorial regions. As the Cassini mission continues, more dune fields are becoming unveiled and examined by the microwave radar in all its modes of operation (SAR, radiometry, scatterometry, altimetry) and with an increasing variety of observational geometries. In this paper, we report on Cassini’s radar instrument observations of the dune fields mapped through May 2009 and present our key findings in terms of Titan’s geology and climate. We estimate that dune fields cover ∼12.5% of Titan’s surface, which corresponds to an area of ∼10 million km2, roughly the area of the United States. If dune sand-sized particles are mainly composed of solid organics as suggested by VIMS observations (Cassini Visual and Infrared Mapping Spectrometer) and atmospheric modeling and supported by radiometry data, dune fields are the largest known organic reservoir on Titan. Dune regions are, with the exception of the polar lakes and seas, the least reflective and most emissive features on this moon. Interestingly, we also find a latitudinal dependence in the dune field microwave properties: up to a latitude of ∼11°, dune fields tend to become less emissive and brighter as one moves northward. Above ∼11° this trend is reversed. The microwave signatures of the dune regions are thought to be primarily controlled by the interdune proportion (relative to that of the dune), roughness and degree of sand cover. In agreement with radiometry and scatterometry observations, SAR images suggest that the fraction of interdunes increases northward up to a latitude of ∼14°. In general, scattering from the subsurface (volume scattering and surface scattering from buried interfaces) makes interdunal regions brighter than the dunes. The observed latitudinal trend may therefore also be partially caused by a gradual thinning of the interdunal sand cover or surrounding sand sheets to the north, thus allowing wave penetration in the underlying substrate. Altimetry measurements over dunes have highlighted a region located in the Fensal dune field (∼5° latitude) where the icy bedrock of Titan is likely exposed within smooth interdune areas. The hemispherical assymetry of dune field properties may point to a general reduction in the availability of sediments and/or an increase in the ground humidity toward the north, which could be related to Titan’s asymmetric seasonal polar insolation. Alternatively, it may indicate that either the wind pattern or the topography is less favorable for dune formation in Titan’s northern tropics. 相似文献
187.
Mallory S. E. Roberts Crystal L. Brogan Bryan M. Gaensler Jason W. T. Hessels C.-Y. Ng Roger W. Romani 《Astrophysics and Space Science》2005,297(1-4):93-100
A remarkable number of pulsar wind nebulae (PWN) are coincident with EGRET γ-ray sources. X-ray and radio imaging studies of unidentified EGRET sources have resulted in the discovery of at least six new pulsar wind nebulae (PWN). Stationary PWN (SPWN) appear to be
associated with steady EGRET sources with hard spectra, typical for γ-ray pulsars. Their toroidal morphologies can help determine the geometry of the
pulsar which is useful for constraining models of pulsed γ-ray emission. Rapidly moving PWN (RPWN) with more cometary morphologies
seem to be associated with variable EGRET sources in regions where the ambient medium is dense compared to what is typical for the ISM. 相似文献
188.
Abstract— The possibility of volcanism on Mercury has been a topic of discussion since Mariner 10 returned images of half the planet's surface showing widespread plains material. These plains could be volcanic or lobate crater ejecta. An assessment of the mechanics of the ascent and eruption of magma shows that it is possible to have widespread volcanism, no volcanism on the surface whatsoever, or some range in between. It is difficult to distinguish between a lava flow and lobate crater ejecta based on morphology and morphometry. No definite volcanic features have been identified on Mercury. However, known lunar volcanic features cannot be identified in images with similar resolutions and viewing geometries as the Mariner 10 dataset. Examination of high‐resolution, low Sun angle Mariner 10 images reveals several features which are interpreted to be flow fronts; it is unclear if these are volcanic flows or ejecta flows. This analysis implies that a clear assessment of volcanism on Mercury must wait for better data. MESSENGER (MErcury: Surface, Space ENvironment, GEochemistry, Ranging) will take images with viewing geometries and resolutions appropriate for the identification of such features. 相似文献
189.
190.
Samuel Lévêque Bertrand Koehler Oskar von der Lühe 《Astrophysics and Space Science》1996,239(2):305-314
The Very Large Telescope Interferometer [1,13] will be operated in air which will introduce small optical path fluctuations due to internal turbulence [4,6] and dispersion effects. Both may contribute to fringe contrast decrease. Longitudinal dispersion effects can be corrected by inserting an appropriate glass of variable thickness in one arm of the interferometer [3,5,11,12]. This paper presents a new method applied to VLTI in order to select the optimum glass, according to both the observing wavelength and the spectral bandpath, and to calculate its thickness. Results are presented in terms of improvement on the fringe contrast. 相似文献