全文获取类型
收费全文 | 2222篇 |
免费 | 217篇 |
国内免费 | 233篇 |
专业分类
测绘学 | 879篇 |
大气科学 | 95篇 |
地球物理 | 251篇 |
地质学 | 684篇 |
海洋学 | 191篇 |
天文学 | 48篇 |
综合类 | 207篇 |
自然地理 | 317篇 |
出版年
2024年 | 3篇 |
2023年 | 23篇 |
2022年 | 69篇 |
2021年 | 66篇 |
2020年 | 84篇 |
2019年 | 69篇 |
2018年 | 51篇 |
2017年 | 88篇 |
2016年 | 97篇 |
2015年 | 115篇 |
2014年 | 110篇 |
2013年 | 137篇 |
2012年 | 173篇 |
2011年 | 152篇 |
2010年 | 137篇 |
2009年 | 114篇 |
2008年 | 135篇 |
2007年 | 113篇 |
2006年 | 110篇 |
2005年 | 96篇 |
2004年 | 98篇 |
2003年 | 88篇 |
2002年 | 57篇 |
2001年 | 60篇 |
2000年 | 59篇 |
1999年 | 55篇 |
1998年 | 68篇 |
1997年 | 32篇 |
1996年 | 38篇 |
1995年 | 28篇 |
1994年 | 20篇 |
1993年 | 34篇 |
1992年 | 27篇 |
1991年 | 15篇 |
1990年 | 14篇 |
1989年 | 11篇 |
1988年 | 7篇 |
1987年 | 7篇 |
1986年 | 1篇 |
1985年 | 2篇 |
1984年 | 1篇 |
1982年 | 1篇 |
1981年 | 1篇 |
1980年 | 2篇 |
1979年 | 1篇 |
1978年 | 1篇 |
1976年 | 1篇 |
1954年 | 1篇 |
排序方式: 共有2672条查询结果,搜索用时 15 毫秒
1.
Janis Britals 《Celestial Mechanics and Dynamical Astronomy》1992,54(4):305-316
It is shown in this paper how to build a canonical transformation of variables, so that the eccentric anomaly becomes the new independent variable. In the case of eccentric elliptical orbits it changes the equations of motion so, that they can be integrated analytically to any order of approximation comparatively easy. 相似文献
2.
We model the subnebulae of Jupiter and Saturn wherein satellite accretion took place. We expect each giant planet subnebula to be composed of an optically thick (given gaseous opacity) inner region inside of the planet’s centrifugal radius (where the specific angular momentum of the collapsing giant planet gaseous envelope achieves centrifugal balance, located at rCJ ∼ 15RJ for Jupiter and rCS ∼ 22RS for Saturn) and an optically thin, extended outer disk out to a fraction of the planet’s Roche-lobe (RH), which we choose to be ∼RH/5 (located at ∼150 RJ near the inner irregular satellites for Jupiter, and ∼200RS near Phoebe for Saturn). This places Titan and Ganymede in the inner disk, Callisto and Iapetus in the outer disk, and Hyperion in the transition region. The inner disk is the leftover of the gas accreted by the protoplanet. The outer disk may result from the nebula gas flowing into the protoplanet during the time of giant planet gap-opening (or cessation of gas accretion). For the sake of specificity, we use a solar composition “minimum mass” model to constrain the gas densities of the inner and outer disks of Jupiter and Saturn (and also Uranus). Our model has Ganymede at a subnebula temperature of ∼250 K and Titan at ∼100 K. The outer disks of Jupiter and Saturn have constant temperatures of 130 and 90 K, respectively.Our model has Callisto forming in a time scale ∼106 years, Iapetus in 106-107 years, Ganymede in 103-104 years, and Titan in 104-105 years. Callisto takes much longer to form than Ganymede because it draws materials from the extended, low density portion of the disk; its accretion time scale is set by the inward drift times of satellitesimals with sizes 300-500 km from distances ∼100RJ. This accretion history may be consistent with a partially differentiated Callisto with a ∼300-km clean ice outer shell overlying a mixed ice and rock-metal interior as suggested by Anderson et al. (2001), which may explain the Ganymede-Callisto dichotomy without resorting to fine-tuning poorly known model parameters. It is also possible that particulate matter coupled to the high specific angular momentum gas flowing through the gap after giant planet gap-opening, capture of heliocentric planetesimals by the extended gas disk, or ablation of planetesimals passing through the disk contributes to the solid content of the disk and lengthens the time scale for Callisto’s formation. Furthermore, this model has Hyperion forming just outside Saturn’s centrifugal radius, captured into resonance by proto-Titan in the presence of a strong gas density gradient as proposed by Lee and Peale (2000). While Titan may have taken significantly longer to form than Ganymede, it still formed fast enough that we would expect it to be fully differentiated. In this sense, it is more like Ganymede than like Callisto (Saturn’s analog of Callisto, we expect, is Iapetus). An alternative starved disk model whose satellite accretion time scale for all the regular satellites is set by the feeding of planetesimals or gas from the planet’s Roche-lobe after gap-opening is likely to imply a long accretion time scale for Titan with small quantities of NH3 present, leading to a partially differentiated (Callisto-like) Titan. The Cassini mission may resolve this issue conclusively. We briefly discuss the retention of elements more volatile than H2O as well as other issues that may help to test our model. 相似文献
3.
Numerical methods are usually used for the computation of ephemerides with perturbations for the precise orbital determination of an artificial satellite. But their numerical stability will be encountered in a long arc. In this case the use the improved Encke special perturbation methods has been suggested. The results of this paper show that Encke's method does indeed have a certain effectiveness, but cannot yet completely resolve the numerical stability, and the more efficient method is to use the energy integral or its variational relation to control the growth of the along-track error in general numerical calculations so that the aim of stabilization can be achieved. 相似文献
4.
5.
激光粒度仪的广泛应用带来了与历史数据的对比问题,因此需要建立激光粒度仪与早期分析结果之间的关系。根据江苏海岸潮滩沉积物样品的激光粒度仪和移液管-筛析法分析,对粒度参数、粒度组分等进行了对比,对两种方法的差异进行了分析。结果表明,对于江苏潮滩沉积物粒度参数中平均粒径的激光粒度仪与移液管-筛析分析结果之间有良好的线性关系;筛分法测得的粗颗粒物质较激光法偏少,而移液管法法测得的细颗粒物质较激光法偏多;将样品分类之后再进行两种方法所获粒度参数的回归分析,相关性得以提高,说明不同粒度组成的沉积物对分析结果的对比有不同的影响。两种方法之间的换算关系不仅与研究区域有关,而且与沉积物本身的粒度组成有关。 相似文献
6.
1.0GPa和常温至1100 ℃条件下角闪石斜长片麻岩的V_p变化:实验测量与理论计算 总被引:3,自引:0,他引:3
在1.0GPa、常温至1100℃条件下测量了角闪石斜长片麻岩的纵波速度(Vp),并统计了不同温度实验产物中各种矿物的体积百分含量。结果显示,1.0GPa下,角闪石斜长片麻岩的Vp首先随温度升高(室温至700℃)缓慢降低约6%,然后(700—850℃)快速降低约6%,再(850~950℃)转而急剧升高15%~25%,最后(T〉950℃)又快速下降。实验产物分析表明在高温高压下α-石英-β石英相变和岩石部分熔融是岩石Vp异常变化的主要因素。由取样产物的矿物含量和弹性参数,计算了各温度条件下岩石的Vp得出与实验测量相同的波速-温度变化趋势,即Vp随温度升高先缓慢降低,接着快速降低后又急剧升高,最后又快速减小。实验测量和理论计算对比研究表明,通过高温高压下岩石中的物相变化观测结果进行岩石波速的计算,是检验岩石弹性波速测量结果和研究地球内部地震波结构的一种有效方法。 相似文献
7.
提出一种基于BP神经网络的结构破损诊断方法,该方法以结构破损前后柔度的变化作为破损诊断网络输入,为了解决由于系统响应样本数据空间分布不均匀对网络收敛速度及网络诊断影响问题,对网络训练样本采用广义空间格点进行了交换,模拟算例及应用实例均表明,本文方法能准确诊断结构破损位置与破坏程度,是一种有效的结构破损诊断方法. 相似文献
8.
9.
Li Yucheng 《海洋学报(英文版)》1996,15(2):261-272
Thewavetransformationandbreakingphenomenainshallowwater¥LiYucheng(1.DalianUniversityofTechnology,Dalian116023,China)Abstract:... 相似文献
10.