全文获取类型
收费全文 | 16576篇 |
免费 | 326篇 |
国内免费 | 122篇 |
专业分类
测绘学 | 360篇 |
大气科学 | 1133篇 |
地球物理 | 3314篇 |
地质学 | 6392篇 |
海洋学 | 1529篇 |
天文学 | 3339篇 |
综合类 | 66篇 |
自然地理 | 891篇 |
出版年
2022年 | 172篇 |
2021年 | 269篇 |
2020年 | 257篇 |
2019年 | 316篇 |
2018年 | 665篇 |
2017年 | 579篇 |
2016年 | 626篇 |
2015年 | 318篇 |
2014年 | 592篇 |
2013年 | 861篇 |
2012年 | 660篇 |
2011年 | 822篇 |
2010年 | 762篇 |
2009年 | 901篇 |
2008年 | 785篇 |
2007年 | 755篇 |
2006年 | 664篇 |
2005年 | 499篇 |
2004年 | 495篇 |
2003年 | 438篇 |
2002年 | 433篇 |
2001年 | 326篇 |
2000年 | 341篇 |
1999年 | 242篇 |
1998年 | 271篇 |
1997年 | 236篇 |
1996年 | 178篇 |
1995年 | 191篇 |
1994年 | 168篇 |
1993年 | 160篇 |
1992年 | 116篇 |
1991年 | 136篇 |
1990年 | 137篇 |
1989年 | 109篇 |
1988年 | 126篇 |
1987年 | 146篇 |
1986年 | 126篇 |
1985年 | 162篇 |
1984年 | 162篇 |
1983年 | 154篇 |
1982年 | 143篇 |
1981年 | 128篇 |
1980年 | 144篇 |
1979年 | 134篇 |
1978年 | 131篇 |
1977年 | 113篇 |
1976年 | 91篇 |
1975年 | 95篇 |
1974年 | 104篇 |
1973年 | 94篇 |
排序方式: 共有10000条查询结果,搜索用时 15 毫秒
161.
O. Engvold 《Solar physics》1980,67(2):351-355
Observed H brightness versus size of emission substructures of quiescent prominences are compared with values predicted from thermodynamical models. The measured size of an emission element of a given brightness is substantially less than the theoretical value.Two possible causes for the discrepancy are suggested: (1) The partial filling of a recording aperture, due to the prominence fine structure, may affect the measurements seriously. Caution is therefore urged against using face values of observed brightness vs ratios in model calculations in cases of partly optically thick lines. (2) Changes of individual fine structure elements on a time scale of a few minutes implies that the prominence plasma may be in a non-stationary radiative state. 相似文献
162.
163.
164.
165.
Thomas E. Corbin 《Celestial Mechanics and Dynamical Astronomy》1980,22(1):25-34
Systematic reductions of nineteenth century observations to the system of the FK4 are discussed. Reductions made on a nightly basis are described and compared with the results obtained through the use of conventional tables. The series of observations made at the Paris Observatory from 1837 to 1881 was used to compare the two methods, and a combined system of 24 000 FK4, FK4 Sup and AGK 3R positions and proper motions provided the reference stars. The results show that for Uranus the mean error of a single observation in right ascension is ±1..33 when tables are used for the reductions, and ±1.12 when nightly reductions are made, while in declination the corresponding mean errors are ±0.88 and ±0.80. The observations of Neptune show an even greater difference between the two methods; the mean errors for the tabular and nightly reductions are ±1.57 and ±1.09 in right ascension and ±0.88 and ±0.75 in declination. Secular rates in the (0–C)'s of Uranus of –0.029/year in right ascension and ±0.030/year in declination are present when the observations are reduced with tables. These rates are reduced to –0.007/year and +0.015/year, respectively, when nightly reductions are made.Presented at the Symposium Star Catalogues, Positional Astronomy and Celestial Mechanics, held in honor of Paul Herget at the U.S. Naval Observatory, Washington, November 30, 1978. 相似文献
166.
167.
O. Demircan 《Astrophysics and Space Science》1977,47(2):459-488
Kopal's new iterative method for analysing partially eclipsing binary light curves in the frequency domain has been put into a form suitable for applications, and explicit forms for basic expressions developed. To facilitate the computations in practice, the required newS
m
-functions, which are expressed in terms ofJ
,
0
-integrals, have been extensively tabulated by making use of hypergeometric series. The automated method has been tested successfully on the light curves of Persei (Algol). Short information on the system and the revised sets of elements including a new determination of the limb-darkening coefficient in the ultraviolet have been presented. 相似文献
168.
C. D'uston J. M. Bosqued F. Cambou V. V. Temny G. N. Zastenker O. L. Vaisberg E. G. Eroshenko 《Solar physics》1977,51(1):217-229
Solar wind and interplanetary magnetic field data were obtained by the PROGNOZ 1 and PROGNOZ 2 satellites during the period following the August 4, 1972 (0621 UT) solar flare. A thermalized plasma was recorded one hour after the shock followed two hours later by the plasma piston with a bulk velocity higher than 1700 km s-1. The comparison between the PROGNOZ and PIONEER 9 solar wind data shows an attenuation of the plasma properties with the deflection from the flare's meridian. 相似文献
169.
G. E. O. Giacaglia 《Celestial Mechanics and Dynamical Astronomy》1977,15(2):191-215
The equations of motion of an artificial satellite are given in nonsingular variables. Any term in the geopotential is considered as well as luni-solar perturbations up to an arbitrary power ofr/r, r being the geocentric distance of the disturbing body. Resonances with tesseral harmonics and with the Moon or Sun are also considered. By neglecting the shadow effect, the disturbing function for solar radiation is also developed in nonsingular variables for the long periodic perturbations. Formulas are developed for implementation of the theory in actual computations. 相似文献
170.
The correlation between the polar cap geomagnetic variations (H-traces) and the changes of the azimuthal (YSE) and vertical (ZSE) components of the interplanetary magnetic field (IMF) during undisturbed periods is examined. It is shown that peak-to-peak correlation between YSE and geomagnetic horizontal component variations may be generally observed in the daytime cusp region, independently of the magnitude and polarity of the ZSE. The existence of the DP3 disturbances associated with the northward component ZSE > 0 is confirmed. It is shown that the disturbances due to the vertical component of the IMF dominate in the region near the pole. In so far as the southward component of the IMF generates both polar cap disturbances and geomagnetic substorms, the disturbances in the region near the pole, associated with ZSE < 0, may be regarded as a precursor of a substorm. On this basis a new index of the polar cap magnetic activity PCL, characterizing the changeability of the magnetic field is proposed. It is shown that the increase of the PCL index is followed in 1–2 hr by a substorm in 70% of events considered. 相似文献