全文获取类型
收费全文 | 60876篇 |
免费 | 422篇 |
国内免费 | 1128篇 |
专业分类
测绘学 | 2085篇 |
大气科学 | 3659篇 |
地球物理 | 11461篇 |
地质学 | 25840篇 |
海洋学 | 4513篇 |
天文学 | 10333篇 |
综合类 | 2248篇 |
自然地理 | 2287篇 |
出版年
2022年 | 488篇 |
2021年 | 708篇 |
2020年 | 755篇 |
2019年 | 826篇 |
2018年 | 6340篇 |
2017年 | 5458篇 |
2016年 | 4162篇 |
2015年 | 843篇 |
2014年 | 1493篇 |
2013年 | 2058篇 |
2012年 | 2566篇 |
2011年 | 4537篇 |
2010年 | 3752篇 |
2009年 | 4240篇 |
2008年 | 3604篇 |
2007年 | 4279篇 |
2006年 | 1787篇 |
2005年 | 1088篇 |
2004年 | 1211篇 |
2003年 | 1194篇 |
2002年 | 988篇 |
2001年 | 810篇 |
2000年 | 681篇 |
1999年 | 430篇 |
1998年 | 458篇 |
1997年 | 474篇 |
1996年 | 337篇 |
1995年 | 358篇 |
1994年 | 335篇 |
1993年 | 281篇 |
1992年 | 284篇 |
1991年 | 290篇 |
1990年 | 337篇 |
1989年 | 272篇 |
1988年 | 258篇 |
1987年 | 260篇 |
1986年 | 191篇 |
1985年 | 301篇 |
1984年 | 302篇 |
1983年 | 295篇 |
1982年 | 274篇 |
1981年 | 269篇 |
1980年 | 282篇 |
1979年 | 203篇 |
1978年 | 242篇 |
1977年 | 204篇 |
1976年 | 183篇 |
1975年 | 184篇 |
1974年 | 171篇 |
1973年 | 206篇 |
排序方式: 共有10000条查询结果,搜索用时 15 毫秒
991.
A. K. Pandey K. Upadhyay K. Ogura Ram Sagar V. Mohan H. Mito H. C. Bhatt B. C. Bhatt 《Monthly notices of the Royal Astronomical Society》2005,358(4):1290-1308
UBVRI CCD photometry in a wide field around two young open clusters, NGC 663 and 654, has been carried out. Hα and polarimetric observations for the cluster NGC 654 have also been obtained. We use the photometric data to construct colour–colour and colour–magnitude diagrams, from which we can investigate the reddening, age, mass and evolutionary states of the stellar contents of the these clusters. The reddening across the cluster regions is found to be variable. There is evidence for anomalous reddening law in both clusters; however, more infrared and polarimetric data are needed to conclude about the reddening law. Both clusters are situated at about a distance of 2.4 kpc. Star formation in both clusters is found to be a continuous process. In the case of NGC 663, star formation seems to have taken place sequentially, in the sense that formation of low-mass stars precedes the formation of most massive stars. Whereas, in the case of NGC 654, formation of low-mass stars did not cease after the formation of most massive stars in the cluster. 相似文献
992.
V. T. Doroshenko S. G. Sergeev Yu. S. Efimov S. Nazarov V. I. Pronik E. A. Sergeeva G. A. Sivtsov 《Astrophysics》2007,50(1):40-53
Observations with a matrix photometer are reported. The stellar magnitudes in the BVRcIc bands are estimated for 80 comparison
stars in the neighborhoods of 10 galaxies with active nuclei: 2 Seyfert galaxies, 4 quasars, and 4 BL Lac objects. The stellar
magnitudes of the observed stars range from 11 to 19m.5. For stars with magnitudes of 14–15m the typical photometric errors are 0m.011, 0m.008, 0m.006, and 0m.007 in the B, V, R, and I bands, respectively. The BVRI magnitudes for most of these stars were not known previously. 14′
× 14′ finding charts for these stars are included. These results can be used for differential BVRI photometry of active galactic
nuclei.
__________
Translated from Astrofizika, Vol. 50, No. 1, pp. 57–72 (February 2007). 相似文献
993.
Mikhail V. Medvedev 《Astrophysics and Space Science》2007,307(1-3):245-250
It has recently been realized that the Weibel instability plays a major role in the formation and dynamics of astrophysical
shocks of gamma-ray bursts and supernovae. Thanks to technological advances in the recent years, experimental studies of the
Weibel instability are now possible in laser-plasma interaction devices. We, thus, have a unique opportunity to model and
study astrophysical conditions in laboratory experiments – a key goal of the Laboratory Astrophysics program. Here we briefly
review the theory of strong non-magnetized collisionless GRB and SN shocks, emphasizing the crucial role of the Weibel instability
and discuss the properties of radiation emitted by (isotropic) electrons moving through the Weibel-generated magnetic fields,
which is referred to as the jitter radiation. We demonstrate that the jitter radiation field is anisotropic with respect to
the direction of the Weibel current filaments and that its spectral and polarization characteristics are determined by microphysical
plasma parameters. We stress that the spectral analysis can be used for accurate diagnostics of the plasma conditions in laboratory
experiments and in astrophysical GRB and SN shocks. 相似文献
994.
V. A. Kalmykov 《Physical Oceanography》1996,7(2):91-97
Zakharov's equation is applied to study numerically the evolution of wave amplitudes. It is demonstrated that, owing to Krasitskii's
new kernel functions, the system of surface waves remains Hamiltonian, in contrast to the former approaches used by Yuen,
Lake, and Zakharov. If surface waves are wind-generated, they grow and become stochastic. If the effect of the waves on the
wind is considered, then the wave amplitude evolution, similar to the no-wind case, continues to be recurrent.
Translated by Vladimir A. Puchkin. 相似文献
995.
J. A. Docobo V. S. Tamazian N. D. Melikian M. H. Eritsian A. A. Karapetian 《Astrophysics》2000,43(2):162-169
The results of photometric and polarimetric observations of the star Μ Cep at Byurakan Observatory are presented. Some interesting
correlations between the parameters of the star’s brightness variation and the degree of polarization of the light are obtained.
It is suggested that the recorded rapid changes in the degree of polarization may result from Μ Cep being a double star.
Translated from Astrofizika, Vol. 43, No. 2, pp. 219-228, April–June, 2000. 相似文献
996.
N. A. Andreeva Yu. L. Zyskin O. R. Kalekin Yu. I. Neshpor A. A. Stepanyan V. P. Fomin N. N. Chalenko V. G. Shitov 《Astronomy Letters》2000,26(4):199-203
We present two-year-long observations of the flux of very-high-energy (~1012 eV) gamma rays from the active galactic nucleus Mk 501 performed with a Cherenkov detector at the Crimean Astrophysical Observatory. A gamma-ray flux from the object was shown to exist at confidence levels of 11 and 7 standard deviations for 1997 and 1998, respectively. The flux varied over a wide range. The mean flux at energies >1012 eV, as inferred from the 1997 and 1998 data, is (5.0±0.6)×10?11 and (3.7±0.6)×10?11 cm?2 s?1, respectively. The errors are the sum of statistical observational and modeling errors. The mean power released in the form of gamma rays is ~2×1043 erg s?1 sr?1. 相似文献
997.
Based on CCD spectra obtained with the PFES echelle spectrometer of the 6-m telescope, we have determined for the first time the effective temperature T eff=5900 K, surface gravity logg=0.0, and detailed chemical composition of the faint star identified with the infrared source IRAS 23304+6147 by the model-atmosphere method. Its metallicity indicates that the object belongs to the old Galactic disk (the mean abundance of the iron-group elements V, Cr, and Fe for IRAS 23304+6147 is [X/H]=?0.61 dex). The stellar atmosphere exhibits an enhancement of carbon and nitrogen, [C/Fe]=+0.98, [N/Fe]=+1.36, and C/O>1. Significant overabundances of lanthanides were detected: the mean [X/Fe]=+1.04 for La, Ce, Pr, Nd, and Eu. The elemental abundances suggest that the atmospheric chemical composition of IRAS 23304+6147 was modified mainly by nucleosynthesis followed by mixing. By modeling the object's spectrum, we revealed absorption features at the positions of well-known absorption diffuse interstellar bands (DIBs). An analysis of radial-velocity and intensity measurements for these DIBs leads us to conclude that, for IRAS 23304+6147, the DIBs originate mostly in its circumstellar dust envelope expanding at a velocity of about 20 km s?1. Molecular C2 Swan emission bands were detected in the object's spectrum, which also originate in the circumstellar envelope. There is a close match between the object's atmospheric effective temperatures determined independently by the model-atmosphere method and by modeling its optical and infrared energy distribution, within the accuracy of the methods. 相似文献
998.
We study the relaxation of a compressible plasma to an equilibrium with flow. The constraints of conservation of mass, energy,
angular momentum, cross-helicity and relative magnetic helicity are imposed. Equilibria corresponding to the energy extrema
while conserving these invariants for parallel flows yield three classes of solutions and one of them with an increasing radial
density profile, relevant to solar flux tubes is presented. 相似文献
999.
1000.
Yu. V. Glagolevskij A. V. Shavrina J. Sylvestre G. A. Chountonov Ya. V. Pavlenko V. R. Khalak 《Astrophysical Bulletin》2009,64(2):166-175
Surface helium and silicon distribution of a He-weak CP star HD21699 was examined using the spectra obtained at different phases of the star’s rotational period. The abundance of helium over the whole surface is weak, but in the magnetic polar regions it is strong, apparently due to the impact of stellar wind. Silicon accumulates in the region with a horizontal alignment of the magnetic lines, as follows from the theory. The abundance of helium and silicon increases with depth. Moreover, the boundary of the abundance variation is very sharp and its depth practically does not change with the rotational period phase. Accounting for the stratification of chemical elements considerably changes the deduced temperature distribution with depth as well as the form of the hydrogen line profile. 相似文献