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排序方式: 共有463条查询结果,搜索用时 375 毫秒
101.
102.
G. A. J. Hussain A. Collier Cameron M. M. Jardine N. Dunstone J. Ramirez Velez H. C. Stempels J.-F. Donati M. Semel G. Aulanier T. Harries J. Bouvier C. Dougados J. Ferreira B. D. Carter W. A. Lawson 《Monthly notices of the Royal Astronomical Society》2009,398(1):189-200
We have produced brightness and magnetic field maps of the surfaces of CV Cha and CR Cha: two actively accreting G- and K-type T Tauri stars in the Chamaeleon I star-forming cloud with ages of 3–5 Myr. Our magnetic field maps show evidence for strong, complex multipolar fields similar to those obtained for young rapidly rotating main-sequence stars. Brightness maps indicate the presence of dark polar caps and low-latitude spots – these brightness maps are very similar to those obtained for other pre-main-sequence and rapidly rotating main-sequence stars.
Only two other classical T Tauri stars have been studied using similar techniques so far: V2129 Oph and BP Tau. CV Cha and CR Cha show magnetic field patterns that are significantly more complex than those recovered for BP Tau, a fully convective T Tauri star.
We discuss possible reasons for this difference and suggest that the complexity of the stellar magnetic field is related to the convection zone; with more complex fields being found in T Tauri stars with radiative cores (V2129 Oph, CV Cha and CR Cha). However, it is clearly necessary to conduct magnetic field studies of T Tauri star systems, exploring a wide range of stellar parameters in order to establish how they affect magnetic field generation, and thus how these magnetic fields are likely to affect the evolution of T Tauri star systems as they approach the main sequence. 相似文献
Only two other classical T Tauri stars have been studied using similar techniques so far: V2129 Oph and BP Tau. CV Cha and CR Cha show magnetic field patterns that are significantly more complex than those recovered for BP Tau, a fully convective T Tauri star.
We discuss possible reasons for this difference and suggest that the complexity of the stellar magnetic field is related to the convection zone; with more complex fields being found in T Tauri stars with radiative cores (V2129 Oph, CV Cha and CR Cha). However, it is clearly necessary to conduct magnetic field studies of T Tauri star systems, exploring a wide range of stellar parameters in order to establish how they affect magnetic field generation, and thus how these magnetic fields are likely to affect the evolution of T Tauri star systems as they approach the main sequence. 相似文献
103.
基于SVAR模型的气温变化对南京市工业经济的影响研究 总被引:7,自引:1,他引:6
目前气象经济学领域探讨气象因子与经济体之间相互动态影响的研究尚不多见,基于此,采用年平均气温序列及工业产值、GDP、劳动力序列,建立多变量的结构向量自回归模型(SVAR模型),通过脉冲响应函数来考察气温对南京市工业经济的动态影响,并用方差分解法揭示其相互影响程度.结果表明总体上气温升高对南京工业有负面影响,但是这种负面作用是趋缓的,平均每年南京工业产值的3.1%受到气温升高带来的负面影响;同时南京工业经济发展对当地气温升高确实存在促进作用,平均每年南京工业经济发展对本地的气温升高的贡献率有4.4%.研究也说明SVAR模型不失为研究气象因子对经济体影响的可行方法. 相似文献
104.
105.
In this paper new orbital elements are given for eleven binaries. For eight of them, WDS 00003–4417 = I 1477, WDS 00106–7313 = I 43 AB, WDS 00366+5609 = A 914, WDS 00519–4343 = I 47, WDS 01315+1521 = BU 506, WDS 01577+4434 = A 1526, WDS 08144–4550 = FIN 113 AB and WDS 08291–4756 = FIN 315 Aa‐Ab, the orbital elements are calculated for the first time. For three of them, WDS 04422+2257 = MCA 16 Aa‐Ab, WDS 08275–5501 = FIN 116 and WDS 14567–6247 = FIN 372, the orbital elements are recalculated. One of the eleven binaries, MCA 16 Aa‐Ab, was discovered by McAlister in 1980 by speckle interferometry and four pairs were discovered by Finsen between 1929 and 1960. For these five pairs, all measured separations are less than 0″.4 and most of the observations were done by using the interferometric techniques. The orbital periods calculated here are between 39 and 270 years. The remaining six pairs were discovered between 1878 and 1926 and most of the observations are visual. They have longer orbital periods, between 384 and 1637 years. In addition to the orbital elements the masses, dynamical parallaxes, absolute magnitudes and ephemerides for the next five years are also given in this paper (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
106.
107.
Bijan Saha 《Astrophysics and Space Science》2007,312(1-2):3-11
We consider a system of nonlinear spinor and a Bianchi type I gravitational fields in presence of viscous fluid. The nonlinear
term in the spinor field Lagrangian is chosen to be λ
F, with λ being a self-coupling constant and F being a function of the invariants I an J constructed from bilinear spinor forms S and P. Self-consistent solutions to the spinor and BI gravitational field equations are obtained in terms of τ, where τ is the volume scale of BI universe. System of equations for τ and ε, where ε is the energy of the viscous fluid, is deduced. This system is solved numerically for some special cases.
相似文献
108.
在山东惠民凹陷渐新统东营组二段发现了浪花介超科尾花介科Recticytherura ualisicosta gen.et sp.nov.--U形脊直尾花介(新属、新种),化石产于该段近底部含生物砂质灰岩中。这是本区乃至渤海湾盆地下第三系尾花介科化石的首次发现。对该新属、新种进行了描述并据铰合构造、尾突、放射毛细管及壳壁构造等特征判断其为海相介形类。与之共生的介形类的组合特征、壳壁的元素组成特征及围岩的碳、氧同位素特征反映了微咸-半咸水的沉积环境,并由古湖泊的扩张和古气候分析认为东营组二段沉积期在惠民凹陷发生了一次短暂海泛。 相似文献
109.
介绍了AT88SC1608IC卡的特征和利用AT2051单片机设计的IC卡读写器的基本原理及编程。该卡片的存储和保密功能强,读写器的成本低,应用广泛。 相似文献
110.
关于下蜀黄土分类新方法及其承载力探讨 总被引:6,自引:0,他引:6
吴自强 《水文地质工程地质》2001,28(6):39-42
下蜀黄土是我国区域性分布的一种特殊性土,是在干旱气候条件下由风力堆积而成。单一地采用塑性指数(Ip)对其进行分类是显进管于简单而不能反映其特征。本文综合其活动性指数及粘粒含量进行分类的新方法,有利于对下蜀黄土进行评价。同时因其粉粒含量超过50%,受“袜度效应”影响,不能简单地套用粘性土公式,笔者总结了以往下蜀土分布地区采用的粘性土,新黄土公式,注意到Ip,Ps与fo,fk的相关性,提出了fo=100βPs 40α经验公式。 相似文献