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渐近巨星分支恒星 (AGB星 )是一种晚期演化恒星 ,它是恒星作为以核反应释能为发光能源的天体的最后演化阶段。AGB星阶段的恒星具有许多有趣的性质 ,如很大的质量损失率 (因此形成很厚的拱星尘埃气体包层 ) ,光变 ,热脉动 (或He闪耀 ) ,强的红外超量发射 ,分子脉泽发射等 ,弄清AGB星的演化规律是研究恒星演化理论的重要任务。目前人们所知道的AGB星的演化图景是 ,恒星经过漫长的主序演化之后 ,将经过红巨星 (RGB)阶段 ,然后才进入AGB阶段 ,在其演化过程中AGB星的光度和质量损失率要逐渐增大 ,它的光变周期也逐渐变长 ,在其中心星经历了一系列的由He核反应不稳定性引起的热脉动之后 ,它的质量损失很快停止 ,恒星开始向行星状星云 (PN)演化 ,最后行星状星云将会变成一个白矮星 ,这将是许多初始质量不很大的恒星的最终结局。OH/IR星阶段是AGB星演化的一个阶段 ,OH/IR星是那些质量稍大的恒星在AGB阶段后期演化而成的天体。现阶段人们对OH/IR星的具体演化过程还知道得很少。我们利用了球对称包层中的尘埃辐射转移模型来研究OH/IR星的演化性质 ,并且收集了尽量多的具有可靠距离的OH/IR星来研究他们的光度和质量损失率的演化性质。在本文的研究工作中 ,我们主要讨论了OH/IR星在远红外双色图中的分布规律 ,还发现 相似文献
954.
The cometary Leonid meteoroids represent a size range in between largest carbon-richIDPs and the smallest CI meteorites. Their
dustball structure and chemistry offer anopportunity to constrain hierarchical dust accretion inferred from petrologic studies
ofaggregate and cluster IDPs. The Leonid shower meteoroids of known ``comet ejection'ages provide an opportunity to study
space weathering of cometary dust over periodsof up to several hundred years. The meteors and aggregate and cluster IDPs displaycontinuous
thermal modification of organics and volatile element (Na, K-bearing phases), that occur as discrete minerals and amorphous
solids each different response during kinetically controlled ablation. Leonid meteoroids are not excessively Na-rich. The
occurrences of Leonid meteors can now be accurate predicted and combined withknowledge better models for the settling rates,
collections of surviving dust becomea comet nucleus-sampling mission.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
955.
贺兰山地区春季沙尘气溶胶的化学组分和富集因子分析 总被引:29,自引:11,他引:18
春季在贺兰山两侧的内蒙古吉兰泰和宁夏银川机场采集不同沙尘天气条件下的沙尘气溶胶浓度样本,用中子活化分析测定35种元素浓度,揭示了沙尘气溶胶中的元素浓度特征,沙尘天气下沙尘气溶胶中地壳元素含量增加,且含量随沙尘暴强度增强而增大。讨论了作为参考物质的地壳元素的取值及地球化学分类。沙尘气溶胶相对地壳和黄土的富集因子,以亲硫元素和亲沉积层元素为最高。亲地壳元素中的主成分元素在有沙尘天气时,其富集因子也偏高。 相似文献
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炼铜烟灰制取硫酸铜除铁新工艺研究 总被引:1,自引:0,他引:1
研究和比较了各种炼铜烟灰制取硫酸铅除铁工艺,实验结果表明:用氧气或空气氧化配合过氧化法去除炼铜烟灰酸浸液中铁,除铁率90%,过氧化氮氧化深度除铁,除铁率99.8%,溶液中铁含量降至0.01g/L以下。 相似文献
959.
Large degrees of circular polarization at near-infrared wavelengths have been reported in the OMC1 star-forming region. This discovery, in combination with compelling evidence for the existence of non-spherical aligned grains in star formation regions, has prompted us to investigate scattering from spheroidal particles as a possible mechanism for the production of large circular polarization in reflection nebulae. We use a dipole calculation to model the small particle limit and a T -matrix code to treat arbitrarily sized particles. We find that size distributions of perfectly aligned spheroids, with only modest 2:1 axis ratios, are capable of producing circular polarization of up to 50 per cent when scattering unpolarized incident light. This is the case even for dielectric materials, such as 'astronomical silicate', as long as sufficient large particles are included in the size distribution. We consider the effects of particle alignment and find that spinning oblate spheroids should be much more efficient circular polarizers than equivalent prolate spheroids. 相似文献
960.
Takashi Hasegawa † Ken-ichi Wakamatsu ‡ Matthew Malkan ‡ Kazuhiro Sekiguchi John W. Menzies Quentin A. Parker Jun Jugaku Hiroshi Karoji Sadanori Okamura 《Monthly notices of the Royal Astronomical Society》2000,316(2):326-344
The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre ( l =05, b =95, cz =8500 km s−1 ) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 12°×17° area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219.
In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100‐μm flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000 km s−1 . Field galaxies are also distributed centred at 8500 km s−1 . Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0–5000 km s−1 is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Böotes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also. 相似文献
In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100‐μm flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000 km s