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71.
爆炸影响降水的观测分析 总被引:1,自引:0,他引:1
大气物理研究所三室原理组 《大气科学》1976,(1):62-67
本文对“炮响雨落”的现象进行了实验验证。初步结果表明:在一定云雨条件下,炮击后可能促使未降水积状云产生降水,也可能促使已降水云的降水参量增大,这些变化发生迅速,但维持时间不长。并指出炮击促进云体降水的作用可能是通过改变支托水滴的气流造成的。在适当条件下,通过炮击影响气流的瞬时作用,可能触发云内不稳定能量释放,造成持续下沉,破坏云的发展,从而防止冰雹灾害。 相似文献
72.
一次雹暴的特征随时间演变的分析 总被引:1,自引:0,他引:1
中国科学院兰州高原大气物理研究所雷达组 《大气科学》1976,(2):62-69
冰雹通常由强烈的积雨,即所谓雹暴中形成。在雹暴的整个生命过程中,无论是外观还是内部特征,都在不停地发生着变化。由于这种变化十分激烈和迅速,大冰雹往往就在某一短时间内(通常不超过30分钟)生长并危害农业。加上此时伴随着闪电大风大雨,要观测它甚为困难。因此,人们至今对其演变的许多方面还缺乏详细和确切的的认识。 相似文献
73.
中国科学院大气物理研究所二室模拟组 《大气科学》1977,1(4):247-255
本文用流体模拟实验的方法,研究了我国夏季青藏高原及邻近地区环流的三维结构和成因,主要结果为: 无转动因素时,高原加热作用能引起流体在低层径向地朝高原辐合,在高原上层放射状向周围辐散.高层辐散流体的一部分在高原内部开始下沉,形成高原上空的对流环,在有转动的实验中也观察到.辐散流体中还出现波动. 高原内部经常出现两个对流上升中心,中心附近的温度有较大脉动,两个对流上升区之间有时为下沉运动,构成高原内部独特的对流环. 通过高原中部的南北垂直剖面上,可观察到方向相反的两个对流环,流体在高原中部上升,在南北高原范围内下沉.在高原外部为高原加热引起的下沉运动. 实验表明,包括基本东西风和高原以外热源的环境背景条件,对高原流场有重要作用. 实验结果为解决夏季青藏高原环流的三维结构提供了依据,文中列举了一些说明的现象。 相似文献
74.
中国科学院地质研究所实验地震研究组 《地质科学》1977,12(2):159-171
前言西南地区(指云南、四川西部地区)位于我国南北构造带即南北地震带的南段,是地壳运动剧烈、构造形态复杂、地震活动十分频繁的地区。它西临印度洋板块的俯冲带,东濒古老稳定的四川地台和黔桂古陆,岩层遭到十分强烈的挤压,形成了一系列平行于印度洋板块的巨型褶皱带、深大断裂带及弧形山脉。 相似文献
75.
Technology 《国土资源导刊(湖南)》2007,(11)
青岛266071潜艇;;定深旋回;;控制定深等速直航潜艇操方向舵后将逐渐进入并保持圆周运动,要实现潜艇定深旋回,可同时操纵尾升降舵、首升降舵或者首尾升降舵配合操舵。通过仿真分析各种操纵方案的优劣,得到实现定深旋回的最佳控制方式。Modeling and analysis on the control of submarine's certain depth and gyration motionCHEN Jun-feng, TIAN Wei,CHE Meng-hu (Navy Submarine Academy, Qingdao 266071, China)Submarine will go into and keep the states of circular motion under the contro 相似文献
76.
PAUL GELADI Research Group for Chemometrics University of Ume S- Ume SwedenKIM ESBENSEN Norwegian Computer Center PB Blindern N- Oslo Norway 《地理学报(英文版)》1990,(5)
This is a first foray into the historical start and early years of chemometrics from about 1972 onwards.We have gathered interviews with three originators(Kowalski,Wold and Massart)as well as with aselected group of six other well-known chemometricians who gradually became active in the 1970s(Christie,Clementi,Hopke,Martens,Brown and Deming).The interviews include amongst a host ofsubjective recollections a succinct record of the key historical literature as highlighted by the interviewees'own rankings of‘earliest’and‘best’.A discussion of the most general commonalities in these interviews together with other historicalmaterial is presented in the second part of the paper. 相似文献
77.
Xiang-Jun Lai Yan Li National Astronomical Observatories/ Yunnan Observatory Chinese Academy of Sciences Kunming China Key Laboratory for the Structure Evolution of Celestial Objects China Graduate University of Chinese Academy of Sciences Beijing China. 《中国天文和天体物理学报》2011,(10)
Based on the turbulent convection model (TCM) of Li & Yang, we have studied the characteristics of turbulent convection in the envelopes of 2 and 5M⊙ stars at the red giant branch and asymptotic giant branch phases. The TCM has been successfully applied over the entire convective envelopes, including the convective unstable zone and the overshooting regions. We find that the convective motions become progressively stronger when the stellar models are located farther up along the Hayashi line. In the convect... 相似文献
78.
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
79.
Magnetic fields control the inconstant Sun. The key to understanding solar variability and its direct impact on the Earth rests with understanding all aspects of these magnetic fields. The Advanced Technology Solar Telescope (ATST) has been design specifically for magnetic remote sensing. Its collecting area, spatial resolution, scattered light, polarization properties, and wavelength performance all insure ATST will be able to observe magnetic fields at all heights in the solar atmosphere from photosphere to corona. After several years of design efforts, ATST has been approved by the U.S. National Science Foundation to begin construction with a not to exceed cost cap of approximately $298M. Work packages for major telescope components will be released for bid over the next several months. An application for a building permit has been submitted (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
80.
M. Collados F. Bettonvil L. Cavaller I. Ermolli B. Gelly A. Prez H. Socas‐Navarro D. Soltau R. Volkmer the EST team 《Astronomische Nachrichten》2010,331(6):615-619
In this paper, the present status of the development of the design of the European Solar Telescope is described. The telescope is devised to have the best possible angular resolution and polarimetric performance, maximizing the throughput of the whole system. To that aim, adaptive optics and multi‐conjugate adaptive optics are integrated in the optical path. The system will have the possibility to correct for the diurnal variation of the distance to the turbulence layers, by using several deformable mirrors, conjugated at different heights. The present optical design of the telescope distributes the optical elements along the optical path in such a way that the instrumental polarization induced by the telescope is minimized and independent of the solar elevation and azimuth. This property represents a large advantage for polarimetric measurements. The ensemble of instruments that are planned is also presented (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献