全文获取类型
收费全文 | 33007篇 |
免费 | 5803篇 |
国内免费 | 7903篇 |
专业分类
测绘学 | 2595篇 |
大气科学 | 6825篇 |
地球物理 | 8129篇 |
地质学 | 16033篇 |
海洋学 | 3913篇 |
天文学 | 1382篇 |
综合类 | 3613篇 |
自然地理 | 4223篇 |
出版年
2024年 | 175篇 |
2023年 | 572篇 |
2022年 | 1482篇 |
2021年 | 1756篇 |
2020年 | 1391篇 |
2019年 | 1650篇 |
2018年 | 1797篇 |
2017年 | 1644篇 |
2016年 | 1929篇 |
2015年 | 1675篇 |
2014年 | 2062篇 |
2013年 | 1923篇 |
2012年 | 1868篇 |
2011年 | 1945篇 |
2010年 | 2062篇 |
2009年 | 1922篇 |
2008年 | 1788篇 |
2007年 | 1685篇 |
2006年 | 1313篇 |
2005年 | 1240篇 |
2004年 | 941篇 |
2003年 | 946篇 |
2002年 | 905篇 |
2001年 | 942篇 |
2000年 | 1083篇 |
1999年 | 1484篇 |
1998年 | 1189篇 |
1997年 | 1130篇 |
1996年 | 1038篇 |
1995年 | 911篇 |
1994年 | 787篇 |
1993年 | 713篇 |
1992年 | 565篇 |
1991年 | 450篇 |
1990年 | 330篇 |
1989年 | 311篇 |
1988年 | 270篇 |
1987年 | 150篇 |
1986年 | 143篇 |
1985年 | 95篇 |
1984年 | 99篇 |
1983年 | 75篇 |
1982年 | 65篇 |
1981年 | 58篇 |
1980年 | 41篇 |
1979年 | 34篇 |
1978年 | 11篇 |
1977年 | 11篇 |
1976年 | 6篇 |
1958年 | 30篇 |
排序方式: 共有10000条查询结果,搜索用时 15 毫秒
981.
Relationship between biogeochemical features of biogenic elements and flocculation in the Changjiang Estuary 总被引:1,自引:3,他引:1
RelationshipbetweenbiogeochemicalfeaturesofbiogenicelementsandflocculationintheChangjiangEstuary¥LinYi'an;TangRenyou;LiYan;Do... 相似文献
982.
TheeffectsofimmobilizationonphysiologyandultrastructureofunicellularalgaPlatymonassubcordiformis¥ZhangXuecheng;WuXiaonanandLi... 相似文献
983.
Theconcentrationanddistributionofdimethylsulfideinthemarineatmosphericboundarylayerneartheequator¥LiXingsheng;LiZhe;F.Parungo... 相似文献
984.
非线性效应对浅水水波变形的影响 总被引:3,自引:0,他引:3
本文采用波数矢量无旋和波能守恒方程建立了一个考虑非线性作用的浅水水波变形数值模型,模型中采用Battjes关系与波数矢量无旋,波能守恒方程一起来求解波浪在浅水中变形的波浪要素,在波能守恒方程中考虑了底摩擦的影响。利用本文提出的数值模型对一个斜坡浅滩水域波浪折射绕射现象进行了验证,验证计算中用一个非线性经验弥散关系近似浅水水波变形的非线性效应并与用线性弥散关系的计算结果进行了比较,结果说明使用非线性 相似文献
985.
银河系的形成与演化是天体物理学研究的重大前沿课题,银河系的化学演化在其中更具有极其重要的地位。随着观测资料的不断积累和理论工作的不断深入,银河系化学演化的研究取得了一系列进展。在观测方面,从太阳附近区域,整个银盘,银晕和核球等方面简要回顾了银河系化学演化模型主要观测约束的近期结果;在化学演化模型方面,回顾了银河系化学演化研究的发展历程和近期进展,并对未来的研究进行了展望。 相似文献
986.
987.
Pei Chong Yuan Xiang-Yan Chen Hua-Lin Zhao Jian-Lin WEN Hai-Kun Li Zheng-Yang 《Chinese Astronomy and Astrophysics》2012
The Antarctic site-testing campaigns have shown that Dome C is an excellent astronomical site on the earth, it is better than any of existing mid-latitude astronomical sites in the world, because of its cold and dry weather, low infrared background radiation, continuously observable time as long as 3–4 months, clear and highly transparent atmosphere, low wind speed, and the absence of dust and light pollution. And in the international astronomical community it is generally believed that Dome A with a higher altitude may be better than Dome C as a potential excellent astronomical site. In the past 3 years, although held by the Center for Antarctic Astronomy of Chinese Academy of Sciences, the site testing at Dome A has preliminarily con?rmed the many advantages of Dome A as an excellent astronomical site, but the data about the atmospheric seeing, which is an important parameter for assessing the site quality for optical observations, have not been obtained until now. Hence, on the basis of a commercial telescope with the diameter of 35 cm, we have made the hardware reformation and software development to have it operate as a DIMM (Differential Image Motion Monitor), which can simultaneously monitor both the seeing and isoplanatic angle at Dome A automatically. At present this instrument has been shipped to Antarctica by the “Xuelong” exploration ship, and will be installed at Dome A, and begin to work in early 2011. Before the shipment, by through the comparative measurements together with an existing seeing monitor at the Xinglong astronomical station, the software, hardware, as well as the installation and adjustment of the instrument, are further veri?ed by testing. 相似文献
988.
989.
Sheng-Ping Gong Yun-Feng Gao Jun-Feng Li School of Aerospace Tsinghua University Beijing China 《中国天文和天体物理学报》2011,(8)
The fuel consumption associated with some interplanetary transfer trajectories using chemical propulsion is not affordable. A solar sail is a method of propulsion that does not consume fuel. Transfer time is one of the most pressing problems of solar sail transfer trajectory design. This paper investigates the time-optimal interplanetary transfer trajectories to a circular orbit of given inclination and radius. The optimal control law is derived from the principle of maximization. An indirect method is used... 相似文献
990.
Vishnu Reddy Juan A. Sanchez Andreas Nathues Nicholas A. Moskovitz Jian-Yang Li Edward A. Cloutis Ken Archer Roy A. Tucker Michael J. Gaffey J. Paul Mann Holger Sierks Ulrich Schade 《Icarus》2012,217(1):153-168
Phase angle and temperature are two important parameters that affect the photometric and spectral behavior of planetary surfaces in telescopic and spacecraft data. We have derived photometric and spectral phase functions for the Asteroid 4 Vesta, the first target of the Dawn mission, using ground-based telescopes operating at visible and near-infrared wavelengths (0.4–2.5 μm). Photometric lightcurve observations of Vesta were conducted on 15 nights at a phase angle range of 3.8–25.7° using duplicates of the seven narrowband Dawn Framing Camera filters (0.4–1.0 μm). Rotationally resolved visible (0.4–0.7 μm) and near-IR spectral observations (0.7–2.5 μm) were obtained on four nights over a similar phase angle range. Our Vesta photometric observations suggest the phase slope is between 0.019 and 0.029 mag/deg. The G parameter ranges from 0.22 to 0.37 consistent with previous results (e.g., Lagerkvist, C.-I., Magnusson, P., Williams, I.P., Buontempo, M.E., Argyle, R.W., Morrison, L.V. [1992]. Astron. Astrophys. Suppl. Ser. 94, 43–71; Piironen, J., Magnusson, P., Lagerkvist, C.-I., Williams, I.P., Buontempo, M.E., Morrison, L.V. [1997]. Astron. Astrophys. Suppl. Ser. 121, 489–497; Hasegawa, S. et al. [2009]. Lunar Planet. Sci. 40. ID 1503) within the uncertainty. We found that in the phase angle range of 0° < α ? 25° for every 10° increase in phase angle Vesta’s visible slope (0.5–0.7 μm) increases 20%, Band I and Band II depths increase 2.35% and 1.5% respectively, and the BAR value increase 0.30. Phase angle spectral measurements of the eucrite Moama in the lab show a decrease in Band I and Band II depths and BAR from the lowest phase angle 13° to 30°, followed by possible small increases up to 90°, and then a dramatic drop between 90° and 120° phase angle. Temperature-induced spectral effects shift the Band I and II centers of the pyroxene bands to longer wavelengths with increasing temperature. We have derived new correction equations using a temperature series (80–400 K) of HED meteorite spectra that will enable interpretation of telescopic and spacecraft spectral data using laboratory calibrations at room temperature (300 K). 相似文献