全文获取类型
收费全文 | 27629篇 |
免费 | 5311篇 |
国内免费 | 9563篇 |
专业分类
测绘学 | 450篇 |
大气科学 | 831篇 |
地球物理 | 3151篇 |
地质学 | 28124篇 |
海洋学 | 1632篇 |
天文学 | 5193篇 |
综合类 | 1645篇 |
自然地理 | 1477篇 |
出版年
2024年 | 130篇 |
2023年 | 469篇 |
2022年 | 880篇 |
2021年 | 1048篇 |
2020年 | 989篇 |
2019年 | 1229篇 |
2018年 | 1033篇 |
2017年 | 1196篇 |
2016年 | 1301篇 |
2015年 | 1362篇 |
2014年 | 1909篇 |
2013年 | 1763篇 |
2012年 | 2099篇 |
2011年 | 2106篇 |
2010年 | 2007篇 |
2009年 | 2263篇 |
2008年 | 2093篇 |
2007年 | 2196篇 |
2006年 | 2040篇 |
2005年 | 1739篇 |
2004年 | 1642篇 |
2003年 | 1440篇 |
2002年 | 1235篇 |
2001年 | 1216篇 |
2000年 | 1193篇 |
1999年 | 994篇 |
1998年 | 916篇 |
1997年 | 747篇 |
1996年 | 676篇 |
1995年 | 523篇 |
1994年 | 463篇 |
1993年 | 367篇 |
1992年 | 299篇 |
1991年 | 232篇 |
1990年 | 163篇 |
1989年 | 150篇 |
1988年 | 115篇 |
1987年 | 54篇 |
1986年 | 61篇 |
1985年 | 36篇 |
1984年 | 27篇 |
1983年 | 19篇 |
1982年 | 18篇 |
1981年 | 7篇 |
1980年 | 16篇 |
1979年 | 4篇 |
1978年 | 9篇 |
1977年 | 18篇 |
1954年 | 5篇 |
1875年 | 1篇 |
排序方式: 共有10000条查询结果,搜索用时 175 毫秒
71.
本文简述了沙柳河南区有色金属矿床的基本特征。通过对成矿热液及成矿物质的来源与性质的研究,认为该矿床的成因类型为火山沉积—接触交代改造叠加型,进而探讨了该矿床的成矿模式。 相似文献
72.
M.R. Burleigh J.P. Pye S.W. Poulton K.B. Sohl P.J. Wheatley G.A. Wynn 《Monthly notices of the Royal Astronomical Society》2001,325(4):1458-1462
During re-processing and analysis of the entire ROSAT Wide Field Camera (WFC) pointed observations data base, we discovered a serendipitous, off-axis detection of the cataclysmic variable SW UMa at the onset of its 1997 October superoutburst. Although long outbursts in this SU UMa-type system are known to occur every ∼ 450 d, none had ever been previously observed in the extreme ultra-violet (EUV) by ROSAT . The WFC observations began just ≈13 hr after the optical rise was detected. With a peak count rate of ∼ 4.5 count s−1 in the S1 filter, SW UMa was temporarily the third brightest object in the sky in this waveband. Over the next ≈19 hr the measured EUV flux dropped to < 2 count s−1 , while the optical brightness remained essentially static at m v ∼11 . Similar behaviour has also been recently reported in the EUV light curve of the related SU UMa-type binary OY Car during superoutburst, as reported by Mauche & Raymond. In contrast, U Gem-type dwarf novae show no such early EUV dip during normal outbursts. Therefore, this feature may be common in superoutbursts of SU UMa-like systems. We expand on ideas first put forward by Osaki and Mauche & Raymond and offer an explanation for this behaviour by examining the interplay between the thermal and tidal instabilities that affect the accretion discs in these systems. 相似文献
73.
We present archival Rossi X-ray Timing Explorer ( RXTE ) and simultaneous Advanced Satellite for Cosmology and Astrophysics ( ASCA ) data of the eclipsing low mass X-ray binary (LMXB) X 1822−371. Our spectral analysis shows that a variety of simple models can fit the spectra relatively well. Of these models, we explore two in detail through phase-resolved fits. These two models represent the case of a very optically thick and a very optically thin corona. While systematic residuals remain at high energies, the overall spectral shape is well approximated. The same two basic models are fitted to the X-ray light curve, which shows sinusoidal modulations interpreted as absorption by an opaque disc rim of varying height. The geometry we infer from these fits is consistent with previous studies: the disc rim reaches out to the tidal truncation radius, while the radius of the corona (approximated as spherical) is very close to the circularization radius. Timing analysis of the RXTE data shows a time-lag from hard to soft consistent with the coronal size inferred from the fits. Neither the spectra nor the light curve fits allow us to rule out either model, leaving a key ingredient of the X 1822−371 puzzle unsolved. Furthermore, while previous studies were consistent with the central object being a 1.4 M⊙ neutron star, which has been adopted as the best guess scenario for this system, our light curve fits show that a white dwarf or black hole primary can work just as well. Based on previously published estimates of the orbital evolution of X 1822−371, however, we suggest that this system contains either a neutron star or a low mass (≲2.5 M⊙ ) black hole and is in a transitional state of duration shortward of 107 yr. 相似文献
74.
75.
Sonja Vrielmann Axel D. Schwope 《Monthly notices of the Royal Astronomical Society》2001,322(2):269-279
We present a new mapping algorithm, the Accretion Stream Mapping (ASM), which uses the full phase-coverage of a light curve to derive spatially resolved intensity distributions along the accretion stream in magnetic cataclysmic variables of AM Herculis type (polars). The surface of the accretion stream is approximated as a 12-sided (duodecadon-shaped) tube. After successfully testing this method on artificial data we applied it to emission-line light curves of H β , H γ and He ii λ 4686 of the bright eclipsing polar HU Aqr. We find hydrogen and helium line emission bright in the threading region of the stream where the stream couples on to magnetic field lines. It is particularly interesting that the stream is bright on the irradiated side facing the white dwarf, which highlights the interplay of collisional and radiative excitation/ionization. 相似文献
76.
M.M. Montgomery 《Monthly notices of the Royal Astronomical Society》2001,325(2):761-766
We compare analytical expressions of precession rates from apsidal (positive) superhumps in close binary systems with numerical disc simulation results and observed values. In the analytical expressions, we include both the dynamical effects on the precession of the disc and effects caused by pressure forces that have been theorized to provide a retrograde effect (i.e. slowing) on the prograde disc precession. We establish new limits on density wave pitch angle to a normalized disc sound speed 60≥Ωorb d tan i / c >2.214 . Using average values for the density wave pitch angle i and speed of sound c , we find good correlation between numerical simulations and the analytical expression for the apsidal superhump period excess, which includes both the prograde and retrograde effects, for mass ratios of 0.025≤ q ≤0.33 . We also show good correlations with the four known eclipsing systems, OY Car, Z Cha, HT Cas, and WZ Sge. Our analytical expression for apsidal superhump period excess as a function of orbital period is consistent with the trend found in observed systems. 相似文献
77.
78.
In many areas of engineering practice, applied loads are not uniformly distributed but often concentrated towards the centre of a foundation. Thus, loads are more realistically depicted as distributed as linearly varying or as parabola of revolution. Solutions for stresses in a transversely isotropic half‐space caused by concave and convex parabolic loads that act on a rectangle have not been derived. This work proposes analytical solutions for stresses in a transversely isotropic half‐space, induced by three‐dimensional, buried, linearly varying/uniform/parabolic rectangular loads. Load types include an upwardly and a downwardly linearly varying load, a uniform load, a concave and a convex parabolic load, all distributed over a rectangular area. These solutions are obtained by integrating the point load solutions in a Cartesian co‐ordinate system for a transversely isotropic half‐space. The buried depth, the dimensions of the loaded area, the type and degree of material anisotropy and the loading type for transversely isotropic half‐spaces influence the proposed solutions. An illustrative example is presented to elucidate the effect of the dimensions of the loaded area, the type and degree of rock anisotropy, and the type of loading on the vertical stress in the isotropic/transversely isotropic rocks subjected to a linearly varying/uniform/parabolic rectangular load. Copyright © 2002 John Wiley & Sons, Ltd. 相似文献
79.
80.
IntroductionThe area of eastern Liaoning is an importantmetal and nonmetal metallogenetic district in China,and the Liaohe group is one of the most importantstrata that hosts Pb, Zn, Au, B and Mg etcstratabound deposits. Up to now many geo1ogistssuch as Z… 相似文献