全文获取类型
收费全文 | 435篇 |
免费 | 44篇 |
国内免费 | 113篇 |
专业分类
测绘学 | 9篇 |
大气科学 | 17篇 |
地球物理 | 114篇 |
地质学 | 212篇 |
海洋学 | 62篇 |
天文学 | 90篇 |
综合类 | 67篇 |
自然地理 | 21篇 |
出版年
2023年 | 2篇 |
2022年 | 1篇 |
2021年 | 2篇 |
2020年 | 1篇 |
2019年 | 3篇 |
2018年 | 8篇 |
2017年 | 10篇 |
2016年 | 5篇 |
2015年 | 2篇 |
2014年 | 3篇 |
2013年 | 6篇 |
2011年 | 23篇 |
2010年 | 16篇 |
2009年 | 25篇 |
2008年 | 26篇 |
2007年 | 28篇 |
2006年 | 32篇 |
2005年 | 27篇 |
2004年 | 38篇 |
2003年 | 49篇 |
2002年 | 34篇 |
2001年 | 27篇 |
2000年 | 18篇 |
1999年 | 10篇 |
1998年 | 14篇 |
1997年 | 16篇 |
1996年 | 11篇 |
1995年 | 12篇 |
1994年 | 10篇 |
1993年 | 21篇 |
1992年 | 26篇 |
1991年 | 19篇 |
1990年 | 10篇 |
1989年 | 15篇 |
1988年 | 4篇 |
1987年 | 2篇 |
1986年 | 5篇 |
1985年 | 1篇 |
1983年 | 5篇 |
1981年 | 2篇 |
1979年 | 2篇 |
1978年 | 5篇 |
1977年 | 5篇 |
1975年 | 2篇 |
1974年 | 1篇 |
1970年 | 1篇 |
1933年 | 2篇 |
1927年 | 3篇 |
1924年 | 2篇 |
排序方式: 共有592条查询结果,搜索用时 15 毫秒
31.
32.
The XMM-Newton X-ray observatory was launched at the end of 1999 and it is still successfully operated. In addition to the
X-ray instruments, the payload carries a small telescope, the Optical Monitor, which provides simultaneous imaging and spectroscopic
observations in the optical and UV ranges. In this report we review the status of the OM and its main achievements after 10
years of operations. We also introduce the XMM-OM Serendipitous Ultra-violet Source Survey (SUSS) Catalogue. 相似文献
33.
We are conducting a systematic study of a carefully selected sampleof nearby E/S0 galaxies and Sa bulges using the unique
panoramic integral-fieldspectrograph SAURON, mounted at the WHT. The goal of the SAURON projectis to fully map the gaseous/stellar
kinematics and the stellar populations of a representative sample of 80 early-type galaxies up to 1 Re,probing different environments
(clusters, field). These data, used in combination with existing ground-based and HST observations, and fed to the theoretical
machinery we have developed, will allow to determine theintrinsic dynamical structure of the galaxies. We will also measure
the masses of central black holes, relate the internal dynamics to the ageand metallicity of the stellar populations, and
establish the historyof metal enrichment as a function of Hubble type and environment. Some brief results on two targets observed
during the SAURON campaign will serve as an illustration of the unique and high quality data we are currently gathering.
This revised version was published online in September 2006 with corrections to the Cover Date. 相似文献
34.
35.
碳水化合物的组合合成是一项新兴技术,该技术可以在短时间内合成大量用于进行生物活性筛选的寡糖及拟糖物。液相与固相合成技术可以极大地加快药物研究与开发进程。作者针对该技术在碳水化合物合成方面的研究进展情况进行讨论。 相似文献
36.
We describe a forward-fitting method that has been developed to reconstruct hard X-ray images of solar flares from the Ramaty
High-Energy Solar Spectroscopic Imager (RHESSI), a Fourier imager with rotation-modulated collimators that was launched on
5 February 2002. The forward-fitting method is based on geometric models that represent a spatial map by a superposition of
multiple source structures, which are quantified by circular gaussians (4 parameters per source), elliptical gaussians (6
parameters), or curved ellipticals (7 parameters), designed to characterize real solar flare hard X-ray maps with a minimum
number of geometric elements. We describe and demonstrate the use of the forward-fitting algorithm. We perform some 500 simulations
of rotation-modulated time profiles of the 9 RHESSI detectors, based on single and multiple source structures, and perform
their image reconstruction. We quantify the fidelity of the image reconstruction, as function of photon statistics, and the
accuracy of retrieved source positions, widths, and fluxes. We outline applications for which the forward-fitting code is
most suitable, such as measurements of the energy-dependent altitude of energy loss near the limb, or footpoint separation
during flares.
Supplementary material to this paper is available in electronic form at http://dx.doi.org/10.1023/A:1022469811115 相似文献
37.
K. Groß U. Micksch TIPTEQ Research Group Seismics Team 《Geophysical Journal International》2008,172(2):565-571
We describe results of an active-source seismology experiment across the Chilean subduction zone at 38.2°S. The seismic sections clearly show the subducted Nazca plate with varying reflectivity. Below the coast the plate interface occurs at 25 km depth as the sharp lower boundary of a 2–5 km thick, highly reflective region, which we interpret as the subduction channel, that is, a zone of subducted material with a velocity gradient with respect to the upper and lower plate. Further downdip along the seismogenic coupling zone the reflectivity decreases in the area of the presumed 1960 Valdivia hypocentre. The plate interface itself can be traced further down to depths of 50–60 km below the Central Valley. We observe strong reflectivity at the plate interface as well as in the continental mantle wedge. The sections also show a segmented forearc crust in the overriding South American plate. Major features in the accretionary wedge, such as the Lanalhue fault zone, can be identified. At the eastern end of the profile a bright west-dipping reflector lies perpendicular to the plate interface and may be linked to the volcanic arc. 相似文献
38.
Ahmet Ruhi Mermut 《山地科学学报》2009,(2):I0002-I0002
Soils, the Earth's Critical Zone, play a vital and fundamental role in the Earth's terrain eco- environment system and human life. Although the concepts of soil/quality and sustainable development have been introduced for decades, we are still failing to understand how well soils function and they need tobe cared and protected. We have been increasingly witnessing and becoming the victim of shrinking forests, 相似文献
39.
40.
The Cassini spacecraft has acquired 25 radar altimeter elevation profiles along Titan's surface as of April 2008, and we have analyzed 18 of these for which there are currently reconstructed ephemeris data. Altimeter measurements were collected at spatial footprint sizes from 6-60 km along ground tracks of length 400-3600 km. The elevation profiles yield topographic information at this resolution with a statistical height accuracy of 35-50 m and kilometer-scale errors several times greater. The data exhibit significant variations in terrain, from flat regions with little topographic expression to very rugged Titanscapes. The bandwidth of the transmitted waveform admits vertical resolution of the terrain height to 35 m at each observed location on the surface. Variations in antenna pointing and changes in surface statistics cause the range-compressed radar echoes to exhibit strong systematic and time-variable biases of hundreds of meters in delay. It is necessary to correct the received echoes for these changes, and we have derived correction algorithms such that the derived echo profiles are accurate at the 100 m level for off-nadir pointing errors of 0.3° and 0.6°, for leading edge and echo centroid estimators, respectively. The leading edge of the echo yields the elevation of the highest points on the surface, which we take to be the peaks of any terrain variation. The mean value of the echo delay is more representative of the mean elevation, so that the difference of these values gives an estimate of any local mountain heights. Finding locations where these values diverge indicates higher-relief terrain. Elevation features are readily seen in the height profiles. Several of the passes show mountains of several hundred m altitude, spread over 10's or even 100's of km in spatial extent, so that slopes are very small. Large expanses of sub-100 m topography are commonplace on Titan, so it is rather smooth in many locations. Other areas exhibit more relief, although the overall observed variation in surface height on any pass is less than about 1 km. Some elevation features correspond to observed changes in brightness in Cassini infrared images, but many do not. Correspondence between the imaging SAR ground tracks and the altimeter paths is limited, so that identifying elevation changes with higher resolution SAR features is premature at present. 相似文献