全文获取类型
收费全文 | 18808篇 |
免费 | 2694篇 |
国内免费 | 3673篇 |
专业分类
测绘学 | 770篇 |
大气科学 | 1975篇 |
地球物理 | 2221篇 |
地质学 | 9031篇 |
海洋学 | 1797篇 |
天文学 | 6894篇 |
综合类 | 879篇 |
自然地理 | 1608篇 |
出版年
2024年 | 60篇 |
2023年 | 198篇 |
2022年 | 484篇 |
2021年 | 515篇 |
2020年 | 555篇 |
2019年 | 661篇 |
2018年 | 520篇 |
2017年 | 546篇 |
2016年 | 551篇 |
2015年 | 652篇 |
2014年 | 961篇 |
2013年 | 1010篇 |
2012年 | 1093篇 |
2011年 | 1205篇 |
2010年 | 1188篇 |
2009年 | 1683篇 |
2008年 | 1503篇 |
2007年 | 1527篇 |
2006年 | 1441篇 |
2005年 | 1299篇 |
2004年 | 1152篇 |
2003年 | 1006篇 |
2002年 | 877篇 |
2001年 | 777篇 |
2000年 | 677篇 |
1999年 | 595篇 |
1998年 | 536篇 |
1997年 | 292篇 |
1996年 | 271篇 |
1995年 | 256篇 |
1994年 | 203篇 |
1993年 | 195篇 |
1992年 | 142篇 |
1991年 | 92篇 |
1990年 | 87篇 |
1989年 | 77篇 |
1988年 | 73篇 |
1987年 | 26篇 |
1986年 | 34篇 |
1985年 | 32篇 |
1984年 | 28篇 |
1983年 | 19篇 |
1982年 | 20篇 |
1981年 | 9篇 |
1980年 | 14篇 |
1979年 | 3篇 |
1978年 | 5篇 |
1977年 | 15篇 |
1954年 | 3篇 |
1875年 | 1篇 |
排序方式: 共有10000条查询结果,搜索用时 31 毫秒
101.
102.
宁波盆地地下揭示的一套包含暗色膏硝质泥岩、泥质白云岩在内的紫红、灰紫色泥岩、棕褐色砂砾岩、细砂岩和玻屑凝灰岩的地层,均称方岩组,内含膏盐并具油色显示。对其时代有早、晚白垩世和早第三纪之认识,笔者从70~90年代地质工作中所获化石分析认为,虽然宁波盆地这一层位含化石不丰,但从分布及数量上比较,相对占优势的应该是孢粉和植物化石,其时代意见也较为一致,指示为早白垩世。 相似文献
103.
104.
冰雹云雷达回波自动识别系统 总被引:2,自引:0,他引:2
利用CAPPI资料对立体风暴进行识别,计算并提供出实用的风暴结构参数,采用矩心踊跃法和矩不变量法相结合对单体风暴和混合性风暴回波进行跟踪;最小二第线性外推预报;根据WSD-88D的冰雹算法,在风暴结构基础上本文建立了Windows98操作平台上冰雹识别系统,经单站1年11次强对流天气过程的资料检验,结果表明:雹云识别精度达82%。系统建立了大量人机对话框以方便用户,增加实用性及推广性。 相似文献
105.
T.D. Thoroughgood V.S. Dhillon S.P. Littlefair T.R. Marsh D.A. Smith 《Monthly notices of the Royal Astronomical Society》2001,327(4):1323-1333
We present spectroscopy of the eclipsing recurrent nova U Sco. The radial velocity semi-amplitude of the primary star was found to be from the motion of the wings of the He ii λ 4686-Å emission line. By detecting weak absorption features from the secondary star, we find its radial velocity semi-amplitude to be . From these parameters, we obtain a mass of for the white dwarf primary star and a mass of for the secondary star. The radius of the secondary is calculated to be , confirming that it is evolved. The inclination of the system is calculated to be , consistent with the deep eclipse seen in the light-curves. The helium emission lines are double-peaked, with the blueshifted regions of the disc being eclipsed prior to the redshifted regions, clearly indicating the presence of an accretion disc. The high mass of the white dwarf is consistent with the thermonuclear runaway model of recurrent nova outbursts, and confirms that U Sco is the best Type Ia supernova progenitor currently known. We predict that U Sco is likely to explode within ∼700 000 yr. 相似文献
106.
Kyle T. Alfriend Srinivas R. Vadali Hanspeter Schaub 《Celestial Mechanics and Dynamical Astronomy》2001,81(1-2):57-62
Satellites flying in formation is a concept being pursued by the Air Force and NASA. Potential periodic formation orbits have been identified using Hill's (or Clohessy Wiltshire) equations. Unfortunately the gravitational perturbations destroy the periodicity of the orbits and control will be required to maintain the desired orbits. Since fuel will be one of the major factors limiting the system lifetime it is imperative that fuel consumption be minimized. To maximize lifetime we not only need to find those orbits which require minimum fuel we also need for each satellite to have equal fuel consumption and this average amount needs to be minimized. Thus, control of the system has to be addressed, not just control of each satellite. In this paper control of the individual satellites as well as the constellation is addressed from an astrodynamics perspective. 相似文献
107.
Benedetta Ciardi † rea Ferrara 《Monthly notices of the Royal Astronomical Society》2001,324(3):648-652
We calculate the expected mid-infrared (MIR) molecular hydrogen line emission from the first objects in the Universe. As a result of their low masses, the stellar feedback from massive stars is able to blow away their gas content and collect it into a cooling shell where H2 rapidly forms and IR roto-vibrational (as for example the rest-frame 2.12 μm) lines carry away a large fraction (up to 10 per cent) of the explosion energy. The fluxes from these sources are in the range 10−21 –10−17 erg s−1 cm−2 . The highest number counts are expected in the 20-μm band, where about 105 sources deg−2 are predicted at the limiting flux of 3×10−18 erg s−1 cm−2 . Among the planned observational facilities, we find that the best detection perspectives are offered by the Next Generation Space Telescope ( NGST ), which should be able to reveal about 200 first objects in one hour observation time at its limiting flux in the above band. Therefore, mid-IR instruments appear to represent perfect tools to trace star formation and stellar feedback in the high ( z ≳5) redshift Universe. 相似文献
108.
Davide Lazzati Rosalba Perna Gabriele Ghisellini 《Monthly notices of the Royal Astronomical Society》2001,325(4):L19-L23
The recent detection of a transient absorption feature in the X-ray prompt emission of GRB 990705 showed the importance of such observations in the understanding of gamma-ray bursts and their progenitors. We investigate the time dependence of photoionization edges during the prompt emission of bursts in different environments. We show that their variability can be used to infer the density and geometry of the surrounding medium, giving important clues to unveil the nature of the burst progenitor. 相似文献
109.
Hong Lin Zhang Douglas H. Sampson 《Monthly notices of the Royal Astronomical Society》2001,322(3):433-437
Calculations are made of the resonance contribution to electron-impact excitation of H-like 13 C and Li-like 23 Na, 25 Mg, 27 Al and 29 Si to the upper hyperfine levels that produce millimetre (mm) lines of likely astrophysical interest. The resonance contribution is found to be very important for these Li-like ions, considerably more important than for Li-like 57 Fe considered previously. However, resonances are found to be rather unimportant for H-like 13 C. The effect of radiative decay on the resonance contribution is found to be insignificant in all of the present calculations. 相似文献
110.
R. Papoular 《Monthly notices of the Royal Astronomical Society》2005,362(2):489-497
A model is proposed for the formation of water ice mantles on grains in interstellar clouds. This occurs by direct accretion of monomers from the gas, be they formed by gas or surface reactions. The formation of the first monolayer requires a minimum extinction of interstellar radiation, sufficient to lower the grain temperature to the point where thermal evaporation of monomers is just offset by monomer accretion from the gas. This threshold is mainly determined by the adsorption energy of water molecules on the grain material; for hydrocarbon material, chemical simulation places this energy between 0.5 and 2 kcal mol−1 , which sets the (true) visible extinction threshold at a few magnitudes. However, realistic distributions of matter in a cloud will usually add to this an unrelated amount of cloud core extinction, which can explain the large dispersion of observed (apparent) thresholds. Once the threshold is crossed, all available water molecules in the gas are quickly adsorbed, because the grain cools down and the adsorption energy on ice is higher than on bare grain. The relative thickness of the mantle, and, hence, the slope of τ3 ( A v ) depend only on the available water vapour, which is a small fraction of the oxygen abundance. Chemical simulation was also used to determine the adsorption sites and energies of O and OH on hydrocarbons and study the dynamics of formation of water molecules by surface reactions with gaseous H atoms, as well as their chances to stick in situ. 相似文献