全文获取类型
收费全文 | 78855篇 |
免费 | 1150篇 |
国内免费 | 597篇 |
专业分类
测绘学 | 1873篇 |
大气科学 | 5256篇 |
地球物理 | 14555篇 |
地质学 | 31095篇 |
海洋学 | 6699篇 |
天文学 | 16951篇 |
综合类 | 289篇 |
自然地理 | 3884篇 |
出版年
2022年 | 458篇 |
2021年 | 748篇 |
2020年 | 864篇 |
2019年 | 959篇 |
2018年 | 4045篇 |
2017年 | 3744篇 |
2016年 | 3141篇 |
2015年 | 1125篇 |
2014年 | 1877篇 |
2013年 | 3215篇 |
2012年 | 2875篇 |
2011年 | 4790篇 |
2010年 | 4232篇 |
2009年 | 4933篇 |
2008年 | 4153篇 |
2007年 | 4664篇 |
2006年 | 2603篇 |
2005年 | 2039篇 |
2004年 | 1941篇 |
2003年 | 2014篇 |
2002年 | 1773篇 |
2001年 | 1406篇 |
2000年 | 1316篇 |
1999年 | 1114篇 |
1998年 | 1111篇 |
1997年 | 1079篇 |
1996年 | 928篇 |
1995年 | 868篇 |
1994年 | 821篇 |
1993年 | 700篇 |
1992年 | 658篇 |
1991年 | 669篇 |
1990年 | 723篇 |
1989年 | 587篇 |
1988年 | 571篇 |
1987年 | 638篇 |
1986年 | 600篇 |
1985年 | 779篇 |
1984年 | 789篇 |
1983年 | 763篇 |
1982年 | 733篇 |
1981年 | 649篇 |
1980年 | 668篇 |
1979年 | 586篇 |
1978年 | 565篇 |
1977年 | 535篇 |
1976年 | 499篇 |
1975年 | 506篇 |
1974年 | 482篇 |
1973年 | 517篇 |
排序方式: 共有10000条查询结果,搜索用时 919 毫秒
141.
The photometric U orbital variations of the symbiotic binary AG Peg, caused by occultation of a bright gaseous region by the
M giant in this system, are used to determine the geometry of this region whose existence is explained in the framework of
the colliding winds model. The emission of the bright region varies and a particular value of its mean density of 2–3 1010 cm-3 has been derived. The causes for the irregular variations of the light in the orbital minimum and maximum are discussed.
It is also obtained, when the mass-loss rate of the hot companion of the system decreases to about 5 10-10
Ms
⊙ yr-1, this bright region will disappear.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
142.
Theoretical line ratios involving 2s
2
S - 3p
2
P, 2p
2
P - 3s
2
S, and 2p
2
S - 3d
2
D transitions inCiv between 312 and 420 Å are presented. A comparison of these with solar active region observational data obtained during a rocket flight by the Solar EUV Rocket Telescope and Spectrograph (SERTS) reveals good agreement between theory and experiment, with discrepancies that average only 22%. This provides experimental support for the accuracy of the atomic data adopted in the line ratio calculations, and also resolves discrepancies found previously when the theoretical results were compared with solar data from the S082A instrument on boardSkylab. The potential usefulness of theCIV line ratios as electron temperature diagnostics for the solar transition region is briefly discussed. 相似文献
143.
J.C. Vega Beltrán W.W. Zeilinger A. Pizzella E.M. Corsini F. Bertola J.G. Funes J.E. Beckman 《Astrophysics and Space Science》2001,276(2-4):1201-1210
In this paper we present the kinematics of the gas and/or the stars of a sample of 20 disc galaxies. We investigate whether there is any relation between the kinematics of the gas and stars and the classical morphological type of the galaxies in the sample. We deduce that, in most of the late-type spirals we have studied, the stars and the ionized gas are moving with virtually circular velocity, except when the spectroscopic slit crosses a bar region. On the other hand, we found in the central parts of early-type disc galaxies a wider variety of different behaviour of stars and gas. We find many possible factors that complicate the classification of the kinematical properties of the galaxies by their morphological type: the presence of counter-rotations (star vs. stars or star vs. gas), misalignment between the different kinematic components present in the galaxy, the presence of a bar structure and its orientation with respect to the line of nodes of the galaxy, and interactions and mergers or external accretion processes are some of the problems we find in the study of the kinematics of a galaxy. 相似文献
144.
145.
The results of an investigation of three peculiar objects in the Cygnus region are given. One of them was already known to be a Herbig-Haro object. In accordance with its observational characteristics, the second object is, in all probability, a T Tauri star. The physical character of the last object is not yet entirely clear, but from the properties of its emission in the near infrared range it is probably also a T Tauri star. The proper motions of the objects have been measured. It is shown that all three objects are members of a tight system of the Trapezium type and evidently are the results of the successive fragmentation of an original protostellar body. 相似文献
146.
Polarimetric observations of the light scattered by dust have been carried out at Pic-du-Midi Observatory with the 2 m telescope
in June and September–October 1996, and at Haute-Provence Observatory with the 0.80 m telescope in April 1997. They cover
a total number of 11 nights and a large (6.9°–47.7°) phase angle range. The spatial resolution allows to underline structures
in the coma, as well in the brightness images as in the polarization maps, with a correlation between the regions of bright
structures and the regions of higher polarization. A clear difference appears between the sunward and antisunward side, with
higher polarization on the antisunward side. The phase angle coverage allows us to obtain a polarimetric phase curve for the
whole coma and to compare it with other cometary phase curves. The degree of polarization is higher for Hale-Bopp than for
the comets previously observed.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
147.
N.C. Hambly A.C. Davenhall M.J. Irwin H.T. MacGillivray 《Monthly notices of the Royal Astronomical Society》2001,326(4):1315-1327
In this, the third in a series of three papers concerning the SuperCOSMOS Sky Survey, we describe the astrometric properties of the data base. We describe the algorithms employed in the derivation of the astrometric parameters of the data, and demonstrate their accuracies by comparison with external data sets using the first release of data, the South Galactic Cap survey. We show that the celestial coordinates, which are tied to the International Celestial Reference Frame via the Tycho–2 reference catalogue, are accurate to better than ±0.2 arcsec at J , R ∼19,18 , rising to ±0.3 arcsec at J , R ∼22,21 , with positional-dependent systematic effects from bright to faint magnitudes at the ∼0.1-arcsec level. The proper motion measurements are shown to be accurate to typically ±10 mas yr−1 at J , R ∼19,18 , rising to ±50 mas yr−1 at J , R ∼22,21 , and are tied to zero using the extragalactic reference frame. We show that the zero-point errors in the proper motions are ≤1 mas yr−1 for R >17 , and are no larger than ∼10 mas yr−1 for R <17 mas yr−1 . 相似文献
148.
M. V. Sazhin V. E. Zharov T. A. Kalinina 《Monthly notices of the Royal Astronomical Society》2001,323(4):952-964
Parallax measurements allow distances to celestial objects to be determined. Together with measurements of their position on the celestial sphere, they give a full three-dimensional picture of the location of the objects relative to the observer. The distortion of the parallax value of a distant source affected by weak microlensing is considered. This means that the weak microlensing leads to distortion of the distance scale. The gravitational deflection causes a retrograde apparent motion of the image, which is revealed as a negative parallax. It is shown that the distortions may significantly change the parallax values when they amount to several microseconds of arc. In particular, at this level many measured values of parallaxes should be negative. 相似文献
149.
The new calculations of the Oiv temperature-sensitive EUV line ratios are presented and compared with previous results. 相似文献
150.
Anastassios E. Petropoulos James M. Longuski 《Celestial Mechanics and Dynamical Astronomy》1994,60(4):431-454
An exact analysis of the coverage obtained by spacecraft using cross-track scanning and nadir-centered conical imaging, under imposed viewing obliqueness and resolution requirements, is presented. In addition to exact expressions for the area acquired and the area acquisition rate, envelope theory is introduced to obtain the boundary of the imaged area. These expressions are relatively compact, allowing rapid machine computation. The effects of the sun phase angle, and of imaging system limitations are also examined. The Galileo mission encounter with Callisto is used as a numerical example, from which certain general conclusions are drawn regarding optimal imaging trajectories. 相似文献