全文获取类型
收费全文 | 20687篇 |
免费 | 2202篇 |
国内免费 | 2411篇 |
专业分类
测绘学 | 6847篇 |
大气科学 | 2531篇 |
地球物理 | 3603篇 |
地质学 | 4497篇 |
海洋学 | 1762篇 |
天文学 | 1293篇 |
综合类 | 2068篇 |
自然地理 | 2699篇 |
出版年
2024年 | 98篇 |
2023年 | 232篇 |
2022年 | 744篇 |
2021年 | 924篇 |
2020年 | 899篇 |
2019年 | 1014篇 |
2018年 | 645篇 |
2017年 | 1000篇 |
2016年 | 907篇 |
2015年 | 938篇 |
2014年 | 1094篇 |
2013年 | 1390篇 |
2012年 | 1295篇 |
2011年 | 1184篇 |
2010年 | 911篇 |
2009年 | 1133篇 |
2008年 | 1197篇 |
2007年 | 1431篇 |
2006年 | 1273篇 |
2005年 | 1050篇 |
2004年 | 984篇 |
2003年 | 808篇 |
2002年 | 674篇 |
2001年 | 603篇 |
2000年 | 462篇 |
1999年 | 424篇 |
1998年 | 384篇 |
1997年 | 274篇 |
1996年 | 223篇 |
1995年 | 228篇 |
1994年 | 206篇 |
1993年 | 167篇 |
1992年 | 100篇 |
1991年 | 80篇 |
1990年 | 64篇 |
1989年 | 58篇 |
1988年 | 51篇 |
1987年 | 28篇 |
1986年 | 24篇 |
1985年 | 13篇 |
1984年 | 15篇 |
1982年 | 9篇 |
1981年 | 6篇 |
1980年 | 6篇 |
1977年 | 13篇 |
1976年 | 4篇 |
1973年 | 4篇 |
1972年 | 4篇 |
1971年 | 5篇 |
1954年 | 7篇 |
排序方式: 共有10000条查询结果,搜索用时 78 毫秒
21.
22.
论社会共同价值观 总被引:1,自引:0,他引:1
刘正球 《广东海洋大学学报》2003,23(2):49-56
社会共同价值观是社会共同体之所以能存在和发展的凝聚力、它指导社会共同体及其成员的前进方向、它还规范和约束社会共同体成员的思想和行动以形成社会共同体的合力。社会共同价值观是在一定历史时期的特定社会共同体中各社会阶层的社会成员普遍认同并持有的价值观。社会共同价值观具有普遍性、结构性、稳定性等特征 ,具有凝聚功能、导向功能和规约功能。社会共同价值观具有理论体系的形式、文化形式、社会心理的形式等存在形式 相似文献
23.
It has been found that the near-infrared flux variations of Seyfert galaxies satisfy relations of the form Fi ≈α i j +β i j Fj , where Fi , Fj are the fluxes in filters i and j ; and α i , j , β i , j are constants. These relations have been used to estimate the constant contributions of the non-variable underlying galaxies. The paper attempts a formal treatment of the estimation procedure, allowing for the possible presence of a third component, namely non-variable hot dust. In an analysis of a sample of 38 Seyfert galaxies, inclusion of the hot dust component improves the model fit in approximately half the cases. All derived dust temperatures are below 300 K, in the range 540–860 K or above 1300 K. A noteworthy feature is the estimation of confidence intervals for the component contributions: this is achieved by bootstrapping. It is also pointed out that the model implies that such data could be fruitfully analysed in terms of principal components. 相似文献
24.
Advanced material constitutive models are used to describe complex soil behaviour. These models are often used in the solution of boundary value problems under general loading conditions. Users and developers of constitutive models need to methodically investigate the represented soil response under a wide range of loading conditions. This paper presents a systematic procedure for probing constitutive models. A general incremental strain probe, 6D hyperspherical strain probe (HSP), is introduced to examine rate‐independent model response under all possible strain loading conditions. Two special cases of HSP, the true triaxial strain probe (TTSP) and the plane‐strain strain probe (PSSP), are used to generate 3‐D objects that represent model stress response to probing. The TTSP, PSSP and general HSP procedures are demonstrated using elasto‐plastic models. The objects resulting from the probing procedure readily highlight important model characteristics including anisotropy, yielding, hardening, softening and failure. The PSSP procedure is applied to a Neural Network (NN) based constitutive model. It shows that this probing is especially useful in understanding NN constitutive models, which do not contain explicit functions for yield surface, hardening, or anisotropy. Copyright © 2004 John Wiley & Sons, Ltd. 相似文献
25.
Olac Fuentes 《Experimental Astronomy》2001,12(1):21-31
In this article we show how machine learning methods can beeffectively applied to the problem of automatically predictingstellar atmospheric parameters from spectral information, a veryimportant problem in stellar astronomy. We apply feedforwardneural networks, Kohonen's self-organizing maps andlocally-weighted regression to predict the stellar atmosphericparameters effective temperature, surface gravity and metallicityfrom spectral indices. Our experimental results show that thethree methods are capable of predicting the parameters with verygood accuracy. Locally weighted regression gives slightly betterresults than the other methods using the original dataset asinput, while self-organizing maps outperform the other methods when significant amounts of noise are added. We also implemented a heterogeneous ensemble of predictors, combining the results given by the three algorithms. This ensemble yields better results than any of the three algorithms alone, using both the original and the noisy data. 相似文献
26.
着重讨论了网络用户经济效益的内涵以及用户的投入量和产出量,并提出了评价网络用户经济效益的指标体系,包括成本降低率,成本利润增长率、产品开发时间约率、市场占有增长率等系列指标。 相似文献
27.
卫星激光测距的新进展 总被引:6,自引:0,他引:6
扼要综述了近几年国际上卫星激光测距的进展,介绍了国内激光测距网的现状,展望了未来卫星激光测距的发展。 相似文献
28.
N.C. Hambly A.C. Davenhall M.J. Irwin H.T. MacGillivray 《Monthly notices of the Royal Astronomical Society》2001,326(4):1315-1327
In this, the third in a series of three papers concerning the SuperCOSMOS Sky Survey, we describe the astrometric properties of the data base. We describe the algorithms employed in the derivation of the astrometric parameters of the data, and demonstrate their accuracies by comparison with external data sets using the first release of data, the South Galactic Cap survey. We show that the celestial coordinates, which are tied to the International Celestial Reference Frame via the Tycho–2 reference catalogue, are accurate to better than ±0.2 arcsec at J , R ∼19,18 , rising to ±0.3 arcsec at J , R ∼22,21 , with positional-dependent systematic effects from bright to faint magnitudes at the ∼0.1-arcsec level. The proper motion measurements are shown to be accurate to typically ±10 mas yr−1 at J , R ∼19,18 , rising to ±50 mas yr−1 at J , R ∼22,21 , and are tied to zero using the extragalactic reference frame. We show that the zero-point errors in the proper motions are ≤1 mas yr−1 for R >17 , and are no larger than ∼10 mas yr−1 for R <17 mas yr−1 . 相似文献
29.
C. Jordan S.A. Sim A.D. McMurry M. Aruvel 《Monthly notices of the Royal Astronomical Society》2001,326(1):303-312
Observations of ε Eri (K2 V) have been made with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope . The spectra obtained show a number of emission lines which can be used to determine, or place limits on, the electron density and pressure. Values of the electron pressure are required in order to make quantitative models of the transition region and inner corona from absolute line fluxes, and to constrain semi-empirical models of the chromosphere. Using line flux ratios in Si iii and O iv a mean electron pressure of P e = N e T e =4.8×1015 cm−3 K is derived. This value is compatible with the lower and upper limits to P e found from flux ratios in C iii , O v and Fe xii . Some inconsistencies which may be because of small uncertainties in the atomic data used are discussed. 相似文献
30.