全文获取类型
收费全文 | 661篇 |
免费 | 91篇 |
国内免费 | 182篇 |
专业分类
测绘学 | 23篇 |
大气科学 | 209篇 |
地球物理 | 62篇 |
地质学 | 235篇 |
海洋学 | 53篇 |
天文学 | 298篇 |
综合类 | 11篇 |
自然地理 | 43篇 |
出版年
2024年 | 4篇 |
2023年 | 3篇 |
2022年 | 15篇 |
2021年 | 11篇 |
2020年 | 21篇 |
2019年 | 22篇 |
2018年 | 16篇 |
2017年 | 16篇 |
2016年 | 21篇 |
2015年 | 18篇 |
2014年 | 30篇 |
2013年 | 28篇 |
2012年 | 22篇 |
2011年 | 46篇 |
2010年 | 40篇 |
2009年 | 56篇 |
2008年 | 53篇 |
2007年 | 60篇 |
2006年 | 46篇 |
2005年 | 66篇 |
2004年 | 43篇 |
2003年 | 40篇 |
2002年 | 44篇 |
2001年 | 37篇 |
2000年 | 25篇 |
1999年 | 21篇 |
1998年 | 42篇 |
1997年 | 11篇 |
1996年 | 16篇 |
1995年 | 15篇 |
1994年 | 16篇 |
1993年 | 9篇 |
1992年 | 5篇 |
1991年 | 2篇 |
1990年 | 1篇 |
1989年 | 4篇 |
1988年 | 4篇 |
1987年 | 1篇 |
1985年 | 1篇 |
1980年 | 1篇 |
1978年 | 2篇 |
排序方式: 共有934条查询结果,搜索用时 15 毫秒
61.
A microscale three-dimensional urban energy balance model for studying surface temperatures 总被引:1,自引:2,他引:1
A microscale three-dimensional (3-D) urban energy balance model, Temperatures of Urban Facets in 3-D (TUF-3D), is developed
to predict urban surface temperatures for a variety of surface geometries and properties, weather conditions, and solar angles.
The surface is composed of plane-parallel facets: roofs, walls, and streets, which are further sub-divided into identical
square patches, resulting in a 3-D raster-type model geometry. The model code is structured into radiation, conduction and
convection sub-models. The radiation sub-model uses the radiosity approach and accounts for multiple reflections and shading
of direct solar radiation. Conduction is solved by finite differencing of the heat conduction equation, and convection is
modelled by empirically relating patch heat transfer coefficients to the momentum forcing and the building morphology. The
radiation and conduction sub-models are tested individually against measurements, and the complete model is tested against
full-scale urban surface temperature and energy balance observations. Modelled surface temperatures perform well at both the
facet-average and the sub-facet scales given the precision of the observations and the uncertainties in the model inputs.
The model has several potential applications, such as the calculation of radiative loads, and the investigation of effective
thermal anisotropy (when combined with a sensor-view model). 相似文献
62.
E. Rizza J. O. Burns M. J. Ledlow F. N. Owen W. Voges & M. Bliton 《Monthly notices of the Royal Astronomical Society》1998,301(2):328-342
We present results from a ROSAT HRI study of 11 distant ( z ∼ 0.2–0.3) Abell clusters. We have performed a morphological analysis to search for and quantify substructure in the clusters. About 70 per cent of the sample shows significant evidence of substructure in the form of centroid shift or obvious X-ray clumps. We examine the clusters for the presence of cooling flows, and determine the physical properties of the ICM by deprojecting the HRI data. Nine of the clusters have central cooling times less than the age of the system, in agreement with fractions determined from nearby, X-ray-bright samples. Additional PSPC results are presented for four clusters in the sample, and ASCA results for six clusters. The temperatures and metallicities for these distant clusters appear to be consistent with nearby clusters of similar richness. 相似文献
63.
Peter A. Thomas 《Monthly notices of the Royal Astronomical Society》1998,299(2):349-356
I review the multiphase cooling flow equations that reduce to a relatively simple form for a wide class of self-similar density distributions described by the single parameter, k , first introduced by Nulsen. It is shown that steady-state cooling flows are not consistent with all possible emissivity profiles, which can therefore be used as a test of the theory. In combination, they provide strong constraints on the temperature profile and mass distribution within the cooling radius. The model is applied to ROSAT HRI data for three rich clusters. At one extreme ( K ∼ 1) these show evidence for cores in the mass distribution of size 110–140 h −1 50 kpc and have temperatures that decline towards the flow centre. At the other ( k ∈ ∞), the mass density and gas temperature both rise sharply towards the flow centre. The former are more consistent with observations which usually show a lower emission-weighted temperature within the cooling flow than from the cluster as a whole. The requirement that the solutions have a temperature gradient that is non-increasing towards the cluster centre limits the matter density gradient to be shallower than ρgrav ∝∼ r −1.2 in the cluster core. 相似文献
64.
We present the first diffraction-limited K-band image of the Red Rectangle with 76 mas resolution, an H-band image with 75 mas resolution, and an RG 715 filter image ( 800 nm wavelength) with 78 mas resolution (corresponding to 25 AU for a distance of 330 pc). The H and K images were reconstructed from 6 m telescope speckle data and the RG 715 image from 2.2 m telescope data using the speckle masking bispectrum method. At all wavelengths the images show a compact, highly symmetric bipolar nebula, suggesting a toroidal density distribution of the circumstellar material. No direct light from the central binary can be seen as it is obscured by a dust disk or circumbinary torus. Our first high-resolution H−K color image of the nebula shows a broad red plateau of H−K≈ 2m in the bright inner regions.The optical and near-infrared images and the available photometric continuum observations in a wide range of ultraviolet to centimeter wavelengths enabled us to model the Red Rectangle in detail using a two-dimensional radiative transfer code. Our model matches both the high-resolution images and the spectral energy distribution of this object very well, making the following picture much more certain. The central close binary system with a total luminosity of 3000 L is embedded in a very dense, compact circumbinary torus which has an average number density nH ≈5×1012 cm−3, an outer radius of the dense inner region of R≈30 AU (91 mas), and a ρ∝r−2 density distribution. The full opening angle of the bipolar outflow cavities in our model is 70°. By comparing the observed and theoretical images, we derived an inclination angle of the torus to the line of sight of 7°±1°.The radiative transfer calculations show that the dust properties in the Red Rectangle are spatially inhomogeneous. The modeling confirms that the idea of large grains in the long-lived disk around the Red Rectangle (Jura et al., 1997 [ApJ, 474, 741]) is quantitatively consistent with the observations. In our models, unusually large, approximately millimeter-sized grains dominate the emission of the compact, massive torus. Models with smaller average grain sizes can possibly be found in future studies, for instance, if it turns out that the radio spectrum is not mainly caused by continuum dust emission. Therefore, the large grains suggested by our models require further confirmation by both new observations and radiative transfer calculations. Assuming a dust-to-gas ratio ρd/ρg of 0.005, the dense torus mass is 0.25 M. The model gives a lower limit of 0.0018 M, for the mass of the large particles, which produce a gray extinction of A≈ 28m, towards the center. A much smaller mass of submicron-sized dust grains is presumably located in the polar outflow cavities, their conical surface layers, and in the outer low-density parts of the torus (where ρ∝r−4, in the region of 30 AUr 2000 AU corresponding to 0.′′09–6′′). 相似文献
65.
The Day Nui Con Voi belt in Vietnam is the southeasternmost part of the Red River shear zone in Asia. It is a narrow high-grade metamorphic core complex consisting of garnet–sillimanite–biotite gneisses, mylonite bands, amphibolite layers and migmatites. Geothermobarometric study of the complex revealed that the peak metamorphism took place under amphibolite-facies conditions of 690−60+30°C and 0.65±0.15 GPa and the subsequent mylonitization occurred under greenschist-facies conditions of 480°C and under 0.3 GPa. Fifteen synkinematic hornblende and biotite separates from gneisses, amphibolites and mylonites were dated with the K/Ar method. Hornblende separates from the Day Nui Con Voi give K–Ar ages of 26.4–28.5 Ma, and the biotite separates do give 24.5–24.7 Ma. Combination of thermobarometric and geochronological data yields the cooling history of 500°C at 28 Ma and 300°C at 24 Ma with a cooling rate of 70–110°C Ma−1, and 23 km post-metamorphic exhumation of the core complex. The first 16 km exhumation from the peak of metamorphism (at probably 31 Ma) to 28 Ma was triggered by the left-lateral strike-slip displacement of the Red River shear zone. 相似文献
66.
Scapolite–wollastonite–grossular bearing calc-silicate rocks from the Vellanad area in the Kerala Khondalite Belt (KKB) of Southern India preserve a number of reaction textures which help to deduce their P–T–fluid history. Textures include calcite+plagioclase±quartz symplectites after scapolite, grossular+quartz coronas between wollastonite and plagioclase, grossular coronas between wollastonite and plagioclase+calcite that replace former scapolite, and grossular blebs replacing anorthite+calcite+quartz pseudomorphs of scapolite. Garnet coronas are also observed between clinopyroxene and wollastonite or scapolite or plagioclase. The reactions, apart from those involving clinopyroxene, can be modelled in the simple CaO–Al2O3–SiO2–CO2 system and interpreted using partial reaction grids constructed for the activities of end-members in the analysed phases. The reaction topologies produced are good approximations for the peak as well as retrograde mineral assemblages and reaction textures. For the compositions of the phases present in this study, the medium pressure calc-silicate assemblages are defined by the stable pseudo-invariant points [Qtz], [Mei] and [Grs]. The textural features interpreted using these activity-corrected grids indicate a phase of isobaric cooling from about 835°C to 750°C at 6 kbar in the Vellanad area. This is inconsistent with earlier studies on other lithologies from the KKB, most of which imply a post-peak P–T path involving near-isothermal decompression. However, as the temperatures obtained for the KKB from the calc-silicates are higher than those previously deduced from metapelites and garnet–orthopyroxene assemblages, the phase of near-isobaric cooling reported here is inferred to have proceeded prior to the onset of the decompression documented from studies of other rock types. 相似文献
67.
新生代全球变冷与青藏高原隆升的关系 总被引:8,自引:0,他引:8
文中综合分析可以影响新生代全球变冷的四种原因,提出青藏隆升对新生代大气CO2浓度降低起主导作用,对新生代全球气温的降低起关键控制作用。这种作用是通过青藏高原隆升加剧全球硅酸盐岩和碳酸盐岩的化学风化、有机碳埋藏、植物的光合作用来实现的。而且,青藏高原隆升有可能同洋流改变和行星轨道参数变化于第三纪末至第四纪共同对新生代全球变冷起控制作用。因此,目前首先解决的科学目标应该是:精确刻划青藏高原隆升时代和幅度,并确定青藏高原隆升对新生代全球变冷的贡献,确定一种以青藏高原隆升为主导作用的控制新生代全球变冷的综合模式。 相似文献
68.
69.
We examine the effects of cooling flows on the T X – L Bol relation for a sample of the most X-ray luminous ( L Bol > 1045 erg s−1 ) clusters of galaxies known. Using high-quality ASCA X-ray spectra and ROSAT images we explicitly account for the effects of cooling flows on the X-ray properties of the clusters and show that this reduces the previously noted dispersion in the T X – L Bol relationship. More importantly, the slope of the relationship is flattened from L Bol ∝ T 3 X to approximately L Bol ∝ T 2 X , in agreement with recent theoretical models which include the effects of shocks and pre-heating on the X-ray gas. We find no evidence for evolution in the T X – L Bol relation within z ∼ 0.3. Our results demonstrate that the effects of cooling flows must be accounted for before cosmological parameters can be determined from X-ray observations of clusters. The results presented here should provide a reliable basis for modelling the T X – L Bol relation at high X-ray luminosities. 相似文献
70.
We explore the relationship between the metallicity of the intracluster gas in clusters of galaxies, determined by X-ray spectroscopy, and the presence of cooling flows. Using ASCA spectra and ROSAT images, we demonstrate a clear segregation between the metallicities of clusters with and without cooling flows. On average, cooling-flow clusters have an emission-weighted metallicity a factor ∼ 1.8 times higher than that of non-cooling-flow systems. We suggest that this is caused by the presence of metallicity gradients in the cooling-flow clusters, coupled with the sharply peaked X-ray surface brightness profiles of these systems. Non-cooling-flow clusters have much flatter X-ray surface brightness distributions and are thought to have undergone recent merger events, which may have mixed the central high-metallicity gas with the surrounding less metal-rich material. We find no evidence for evolution in the emission-weighted metallicities of clusters within z ∼ 0.3. 相似文献