全文获取类型
收费全文 | 15819篇 |
免费 | 2904篇 |
国内免费 | 3754篇 |
专业分类
测绘学 | 247篇 |
大气科学 | 914篇 |
地球物理 | 2509篇 |
地质学 | 10596篇 |
海洋学 | 1179篇 |
天文学 | 3939篇 |
综合类 | 825篇 |
自然地理 | 2268篇 |
出版年
2024年 | 87篇 |
2023年 | 260篇 |
2022年 | 653篇 |
2021年 | 682篇 |
2020年 | 607篇 |
2019年 | 717篇 |
2018年 | 610篇 |
2017年 | 567篇 |
2016年 | 588篇 |
2015年 | 717篇 |
2014年 | 758篇 |
2013年 | 823篇 |
2012年 | 862篇 |
2011年 | 870篇 |
2010年 | 783篇 |
2009年 | 1171篇 |
2008年 | 989篇 |
2007年 | 1164篇 |
2006年 | 1176篇 |
2005年 | 1009篇 |
2004年 | 946篇 |
2003年 | 947篇 |
2002年 | 823篇 |
2001年 | 701篇 |
2000年 | 672篇 |
1999年 | 604篇 |
1998年 | 596篇 |
1997年 | 406篇 |
1996年 | 295篇 |
1995年 | 271篇 |
1994年 | 269篇 |
1993年 | 201篇 |
1992年 | 208篇 |
1991年 | 93篇 |
1990年 | 92篇 |
1989年 | 88篇 |
1988年 | 51篇 |
1987年 | 40篇 |
1986年 | 26篇 |
1985年 | 12篇 |
1984年 | 10篇 |
1983年 | 4篇 |
1982年 | 3篇 |
1981年 | 5篇 |
1980年 | 2篇 |
1979年 | 8篇 |
1977年 | 2篇 |
1954年 | 9篇 |
排序方式: 共有10000条查询结果,搜索用时 15 毫秒
41.
42.
43.
The steady-state population of bodies resulting from a collisional cascade depends on how material strength varies with size. We find a simple expression for the power-law index of the population, given a power law that describes how material strength varies with size. This result is extended to the case relevant for the asteroid belt and Kuiper belt, in which the material strength is described by 2 separate power laws—one for small bodies and one for larger bodies. We find that the power-law index of the small body population is unaffected by the strength law for the large bodies, and vice versa. Simple analytical expressions describe a wave that is superimposed on the large body population because of the transition between the two power laws describing the strength. These analytical results yield excellent agreement with a numerical simulation of collisional evolution. These results will help to interpret observations of the asteroids and KBOs, and constrain the strength properties of those objects. 相似文献
44.
疏散星团在天文学和天体物理学研究中有着多方面的重要性。近年来在观测和理论工作上都取得了显著的进展。综述了疏散星团的研究现状,对成员判别、基本参数确定、团与恒星的演化、团的结构和动力学进行了详细评述。 相似文献
45.
Makoto Ideta 《Astrophysics and Space Science》2003,284(2):531-534
Dynamical evolution of N-body bars embedded in spherical and prolate dark matter halos is investigated. In particular, the configuration such that
galactic disks are placed in the plane perpendicular to the equatorial plane of the prolate halos is considered. Such a configuration
is frequently found in cosmological simulations. N-body disks embedded in a fixed external halo potential were simulated, so that the barred structure was formed via dynamical
instability in initially cool disks. In the subsequent evolution, bars in prolate halos dissolved gradually with time, while
the bar pattern in spherical halos remained almost unchanged until the end of simulations. The e-folding time of bars suggest
that they could be destroyed in a time smaller than a Hubble time.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
46.
Emilio Donoso Ana O'Mill Diego G. Lambas 《Monthly notices of the Royal Astronomical Society》2006,369(1):479-484
We analyse a high-redshift sample (0.4 < z < 0.5) of luminous red galaxies (LRGs) extracted from the Sloan Digital Sky Survey data release 4 and their surrounding structures to explore the presence of alignment effects of these bright galaxies with neighbour objects. In order to avoid projection effects, we compute photometric redshifts for galaxies within 3 h −1 Mpc in projection of LRGs and calculate the relative angle between the LRG major axis and the direction to neighbours within 1000 km s−1 . We find a clear signal of alignment between LRG orientations and the distribution of galaxies within 1.5 h −1 Mpc. The alignment effects are present only for the red population of tracers; LRG orientation is uncorrelated to the blue population of neighbour galaxies. These results add evidence to the alignment effects between primaries and satellites detected at low redshifts. We conclude that such alignments were already present at z ∼ 0.5. 相似文献
47.
48.
Distances to nine dark globules are determined by a method using optical ( VRI ) and near-infrared (near-IR) ( JHK ) photometry of stars projected towards the field containing the globules. In this method, we compute intrinsic colour indices of stars projected towards the direction of the globule by dereddening the observed colour indices using various trial values of extinction A V and a standard extinction law. These computed intrinsic colour indices for each star are then compared with the intrinsic colour indices of normal main-sequence stars and a spectral type is assigned to the star for which the computed colour indices best match with the standard intrinsic colour indices. Distances ( d ) to the stars are determined using the A V and absolute magnitude ( MV ) corresponding to the spectral types thus obtained. A distance versus extinction plot is made and the distance at which A V undergoes a sharp rise is taken to be the distance to the globule. All the clouds studied in this work are in the distance range 160–400 pc. The estimated distances to dark globules LDN 544, LDN 549, LDN 567, LDN 543, LDN 1113, LDN 1031, LDN 1225, LDN 1252 and LDN 1257 are 180 ± 35, 200 ± 40, 180 ± 35, 160 ± 30, 350 ± 70, 200 ± 40, 400 ± 80, 250 ± 50 and 250 ± 50 pc, respectively. Using the distances determined, we have estimated the masses of the globules and the far-IR luminosity of the IRAS sources associated with them. The mass of the clouds studied are in the range 10–200 M⊙ . 相似文献
49.
Agostino Renda Daisuke Kawata Yeshe Fenner Brad K. Gibson 《Monthly notices of the Royal Astronomical Society》2005,356(3):1071-1078
The chemical evolution history of a galaxy hides clues about how it formed and has been changing through time. We have studied the chemical evolution history of the Milky Way (MW) and Andromeda (M31) to find which are common features in the chemical evolution of disc galaxies as well as which are galaxy-dependent. We use a semi-analytic multizone chemical evolution model. Such models have succeeded in explaining the mean trends of the observed chemical properties in these two Local Group spiral galaxies with similar mass and morphology. Our results suggest that while the evolution of the MW and M31 shares general similarities, differences in the formation history are required to explain the observations in detail. In particular, we found that the observed higher metallicity in the M31 halo can be explained by either (i) a higher halo star formation efficiency (SFE), or (ii) a larger reservoir of infalling halo gas with a longer halo formation phase. These two different pictures would lead to (i) a higher [O/Fe] at low metallicities, or (ii) younger stellar populations in the M31 halo, respectively. Both pictures result in a more massive stellar halo in M31, which suggests a possible correlation between the halo metallicity and its stellar mass. 相似文献
50.