全文获取类型
收费全文 | 1681篇 |
免费 | 28篇 |
国内免费 | 49篇 |
专业分类
测绘学 | 3篇 |
大气科学 | 9篇 |
地球物理 | 55篇 |
地质学 | 155篇 |
海洋学 | 47篇 |
天文学 | 1463篇 |
综合类 | 9篇 |
自然地理 | 17篇 |
出版年
2024年 | 4篇 |
2023年 | 5篇 |
2022年 | 7篇 |
2021年 | 11篇 |
2020年 | 3篇 |
2019年 | 13篇 |
2018年 | 7篇 |
2017年 | 7篇 |
2016年 | 8篇 |
2015年 | 20篇 |
2014年 | 16篇 |
2013年 | 26篇 |
2012年 | 29篇 |
2011年 | 25篇 |
2010年 | 23篇 |
2009年 | 143篇 |
2008年 | 101篇 |
2007年 | 163篇 |
2006年 | 146篇 |
2005年 | 133篇 |
2004年 | 126篇 |
2003年 | 130篇 |
2002年 | 115篇 |
2001年 | 106篇 |
2000年 | 92篇 |
1999年 | 101篇 |
1998年 | 113篇 |
1997年 | 15篇 |
1996年 | 13篇 |
1995年 | 11篇 |
1994年 | 4篇 |
1993年 | 8篇 |
1992年 | 4篇 |
1991年 | 2篇 |
1990年 | 7篇 |
1989年 | 7篇 |
1988年 | 4篇 |
1987年 | 4篇 |
1984年 | 1篇 |
1983年 | 1篇 |
1981年 | 4篇 |
排序方式: 共有1758条查询结果,搜索用时 31 毫秒
91.
Yun Xu Xin-Wu Cao Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai Graduate School of Chinese Academy of Sciences Beijing 《中国天文和天体物理学报》2007,7(1):63-70
1 INTRODUCTION Most bright active galactic nuclei (AGNs) exhibit broad emission lines, with full width at half maximum (FWHM ≥ 103 km s?1) (Peterson et al. 1999). Some type 1 AGNs could have very broad emission lines (FWHM≥ 20 000 km s?1). Type 2 AGNs s… 相似文献
92.
Accretion disks orbiting black holes power high-energy systems such as X-ray binaries and Active Galactic Nuclei. Observations
are providing increasingly detailed quantitative information about such systems. This data has been interpreted using standard
toy-models that rely on simplifying assumptions such as regular flow geometry and a parameterized stress. Global numerical
simulations offer a way to investigate the basic physical dynamics of accretion flows without these assumptions and, in principle,
lead to a genuinely predictive theory. In recent years we have developed a fully three-dimensional general relativistic magnetohydrodynamic
simulation code that evolves time-dependent inflows into Kerr black holes. Although the resulting global simulations of black
hole accretion are still somewhat simplified, they have brought to light a number of interesting results. These include the
formation of electro-magnetically dominated jets powered by the black hole’s rotation, and the presence of strong stresses
in the plunging region of the accretion flow. The observational consequences of these features are gradually being examined.
Increasing computer power and increasingly sophisticated algorithms promise a bright future for the computational approach
to black hole accretion. 相似文献
93.
94.
95.
A. Juhász T. Prusti P. Ábrahám C. P. Dullemond 《Monthly notices of the Royal Astronomical Society》2007,374(4):1242-1252
We investigate the long-term optical–infrared variability of SV Cep and explain it in the context of an existing UX Ori (UXOR) model. A 25-month monitoring programme was completed with the Infrared Space Observatory in the 3.3–100 μm wavelength range. Following a careful data reduction, the infrared light curves were correlated with the variations of SV Cep in the V band. A remarkable correlation was found between the optical and the far-infrared light curves. In the mid-infrared regime, the amplitude of variations is lower, with a hint for a weak anti-correlation with the optical changes. In order to interpret the observations, we modelled the spectral energy distribution of SV Cep assuming a self-shadowed disc with a puffed-up inner rim, using a two-dimensional radiative transfer code. We found that modifying the height of the inner rim, the wavelength dependence of the long-term optical–infrared variations is well reproduced, except the mid-infrared domain. The origin of variation of the rim height might be fluctuation in the accretion rate in the outer disc. In order to model the mid-infrared behaviour, we tested adding an optically thin envelope to the system, but this model failed to explain the far-infrared variability. Infrared variability is a powerful tool to discriminate between models of the circumstellar environment. The proposed mechanism of variable rim height may not be restricted to UXOR stars, but might be a general characteristic of intermediate-mass young stars. 相似文献
96.
R. G. Martin S. H. Lubow J. E. Pringle M. C. Wyatt 《Monthly notices of the Royal Astronomical Society》2007,378(4):1589-1600
There is evidence for the existence of massive planets at orbital radii of several hundred au from their parent stars where the time-scale for planet formation by core accretion is longer than the disc lifetime. These planets could have formed close to their star and then migrated outwards. We consider how the transfer of angular momentum by viscous disc interactions from a massive inner planet could cause significant outward migration of a smaller outer planet. We find that it is in principle possible for planets to migrate to large radii. We note, however, a number of effects which may render the process somewhat problematic. 相似文献
97.
Results from simultaneous spectral and photometric monitoring of the Herbig Ae star CQ Tau in the neighborhood of the Hα and
resonance sodium doublet Na I D lines are presented. It is shown that the inner structure of the accretion disk of CQ Tau
is nonuniform and consists of two regions with quite different kinematic characteristics. Region I is characterized by relative
stability and a smooth long-term variation in the velocity of the gas along the line of sight. Region II is distinguished
by the highest velocities and a variability in their maximum values over time scales from a few days to 700 days. The dust
clouds which produse the star’s brightness minima may also be the source of cold gas and contribute to the observed spectral
variability. We assume that region I of the disk coincides with the accretion disk of the star. The kinematic differences
in region II may be caused by dissipation of circumstellar dust clouds which, moving in elongated orbits, are able to approach
the star quite closely.
__________
Translated from Astrofizika, Vol. 50, No. 1, pp. 39–55 (February 2007). 相似文献
98.
99.
100.
C. Brocksopp J. C. A. Miller-Jones R. P. Fender B. W. Stappers 《Monthly notices of the Royal Astronomical Society》2007,378(3):1111-1117
XTE J1748−288 is a black hole X-ray transient which went into outburst in 1998 June. The X-ray light curves showed canonical morphologies, with minor variations on the 'fast rise exponential decay' profile. The radio source, however, reached an unusually high flux density of over 600 mJy. This high radio flux was accompanied by an exceptional (>20 per cent) fractional linear polarization, the variability of which was anticorrelated with the flux density. We use this variability to discuss possible depolarization mechanisms and to predict the underlying behaviour of the (unresolved) core/jet components. 相似文献