全文获取类型
收费全文 | 554篇 |
免费 | 13篇 |
国内免费 | 35篇 |
专业分类
大气科学 | 85篇 |
地球物理 | 5篇 |
地质学 | 8篇 |
海洋学 | 2篇 |
天文学 | 495篇 |
综合类 | 3篇 |
自然地理 | 4篇 |
出版年
2023年 | 1篇 |
2022年 | 1篇 |
2021年 | 4篇 |
2020年 | 1篇 |
2019年 | 5篇 |
2018年 | 1篇 |
2017年 | 6篇 |
2016年 | 2篇 |
2015年 | 6篇 |
2014年 | 9篇 |
2013年 | 7篇 |
2012年 | 7篇 |
2011年 | 6篇 |
2010年 | 7篇 |
2009年 | 45篇 |
2008年 | 25篇 |
2007年 | 48篇 |
2006年 | 54篇 |
2005年 | 45篇 |
2004年 | 55篇 |
2003年 | 30篇 |
2002年 | 49篇 |
2001年 | 35篇 |
2000年 | 43篇 |
1999年 | 39篇 |
1998年 | 36篇 |
1997年 | 3篇 |
1996年 | 4篇 |
1995年 | 3篇 |
1994年 | 6篇 |
1993年 | 2篇 |
1992年 | 2篇 |
1991年 | 4篇 |
1990年 | 2篇 |
1989年 | 3篇 |
1986年 | 1篇 |
1985年 | 1篇 |
1984年 | 1篇 |
1982年 | 1篇 |
1979年 | 1篇 |
1978年 | 1篇 |
排序方式: 共有602条查询结果,搜索用时 125 毫秒
141.
142.
Andrei Lobanov 《Astrophysics and Space Science》2007,311(1-3):263-267
Compact relativistic jets in active galactic nuclei offer an effective tool for investigating the physics of nuclear regions
in galaxies. The emission properties, dynamics, and evolution of jets in AGN are closely connected to the characteristics
of the central supermassive black hole, accretion disk and broad-line region in active galaxies. Recent results from studies
of the nuclear regions in several active galaxies with prominent outflows are reviewed in this contribution. 相似文献
143.
Annalisa Celotti 《Astrophysics and Space Science》2005,300(1-3):23-30
This contribution focuses on the evidence for a bimodality in the luminosity believed to be associated with the accretion
process in AGN. In particular, it will be stressed that this behavior does seem to be present in an analogous way both in
radio-loud and radio-quiet AGN, as inferred from samples selected in an independent way. The found bimodality can be naturally
– although not uniquely – interpreted in the frame of the ADIOS solution for radiative inefficient accretion flows. The (so
far) qualitative analogy with the behavior of XRB provides an interesting perspective to find a unique framework for the accretion
and jet production in accreting black hole systems. 相似文献
144.
M. Yu. Piotrovich Yu. N. Gnedin N. A. Silant'ev T. M. Natsvlishvili S. D. Buliga 《Astronomische Nachrichten》2015,336(10):1013-1016
Magnetic fields in an accretion disk around the central black hole can modify the size of the innermost stable circular orbit (ISCO) and can produce a difference to the classical Novikov‐Thorne radius. We estimated the ISCO magnetic field strength from the polarimetric observations of the accretion‐disk radiation. This estimate is obtained taking into account the effect of the Faraday rotation of the polarization plane at the distance of the mean free path of photons between successive electron scattering events. We present the new method for estimating the ISCO radius in the accretion disk, i.e. in the nearest vicinity of a central black hole. Our estimates confirmed the Frolov, Shoom & Tzounis (2014) and Ranea‐Sandoval & Garcia (2015) conclusion that the magnetic field in the accretion disk decreases the size of the innermost stable circular orbit. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
145.
Ruben J. Diaz Horacio Dottori Evencio Mediavilla Maria Aguero Damian Mast 《New Astronomy Reviews》2006,49(10-12):547
We present a scientific case approached through high quality 3D NIR spectroscopy performed with CIRPASS, attached to the Gemini South telescope. A binary mass concentration at the nucleus of the galaxy M 83 was suggested by Thatte et al. [A&A 364 (2000) L47] and Mast et al. [BAAA 45 (2002) 98. Astroph#0505264] determined the possible position of the hidden secondary mass concentration with 2D H-alpha kinematics. The preliminary results of the NIR study presented here are based in almost 1500 spectra centered in the wavelength 1.3 μm, with a spectral resolving power of 3200. They allow us to unveil, with 0.36″ (6.4 pc) sampling and subarcsecond resolution, the velocity field in a region of 13″ × 9″ around the optical nucleus. We confirm that the optical nucleus is not located at the most important center of symmetry of the ionized gas velocity field. The largest black hole that could fit to the circular motion in this kinematic center should have a mass not larger than 3 × 106(sin i)−1 M solar masses. 相似文献
146.
147.
J. R. Touma S. Tremaine M. V. Kazandjian 《Monthly notices of the Royal Astronomical Society》2009,394(2):1085-1108
We show that the algorithm proposed by Gauss to compute the secular evolution of gravitationally interacting Keplerian rings extends naturally to softened gravitational interactions. The resulting tool is ideal for the study of the secular dynamical evolution of nearly Keplerian systems such as stellar clusters surrounding black holes in galactic nuclei, cometary clouds or planetesimal discs. We illustrate its accuracy, efficiency and versatility on a variety of configurations. In particular, we examine a secularly unstable system of counterrotating discs, and follow the unfolding and saturation of the instability into a global, uniformly precessing, lopsided ( m = 1) mode. 相似文献
148.
149.
M. D. Colling P. F. Roche R. E. Mason 《Monthly notices of the Royal Astronomical Society》2009,394(4):2043-2049
We report spatially resolved variations in the 3.4-μm hydrocarbon absorption feature and the 3.3-μm polycyclic aromatic hydrocarbon (PAH) emission band in the Circinus galaxy over the central few arcsec. The absorption is measured towards warm emitting dust associated with Coronal line regions to the east and west of the nucleus. There is an absorption optical depth τ3.4 μm ∼ 0.1 in the core which decreases to the west and increases to the east. This is consistent with increased extinction out to ∼40 pc east of the core, supported by the Coronal emission line intensities which are significantly lower to the east than the west. PAH emission is measured to be symmetrically distributed out to ±4 arcsec, outside the differential extinction region. The asymmetry in the 3.4-μm absorption band reflects that seen in the 9.7-μm silicate absorption band reported by Roche et al., and the ratio of the two absorption depths remains approximately constant across the central regions, with τ3.4 μm /τ9.7 μm ∼ 0.06 ± 0.01 . This indicates well-mixed hydrocarbon and silicate dust populations, with no evidence for significant changes near the nucleus. 相似文献
150.
C. Vignali F. Pozzi J. Fritz A. Comastri C. Gruppioni E. Bellocchi F. Fiore M. Brusa R. Maiolino M. Mignoli F. La Franca L. Pozzetti G. Zamorani A. Merloni 《Monthly notices of the Royal Astronomical Society》2009,395(4):2189-2195
We present multiwavelength observations (from optical to submillimetre, including Spitzer and Submillimetre Common-User Bolometer Array) of H2XMMJ 003357.2−120038 (also GD 158_19), an X-ray selected, luminous narrow-line (type 2) quasar at z = 1.957 selected from the HELLAS2XMM survey. Its broad-band properties can be reasonably well modelled assuming three components: a stellar component to account for the optical and near-infrared (IR) emission; an active galactic nucleus (AGN) component (i.e. dust heated by an accreting active nucleus), dominant in the mid-IR, with an optical depth at 9.7 along the line of sight (close to the equatorial plane of the obscuring matter) of τ(9.7) = 1 and a full covering angle of the reprocessing matter (torus) of 140° and a far-IR starburst component (i.e. dust heated by star formation) to reproduce the wide bump observed longward of 70 .
The derived star formation rate is ≈1500 M⊙ yr−1 . The overall modelling indicates that GD 158_19 is a high-redshift X-ray luminous, obscured quasar with coeval powerful AGN activity and intense star formation. It is probably caught before the process of expelling the obscuring gas has started, thus quenching the star formation. 相似文献
The derived star formation rate is ≈1500 M