全文获取类型
收费全文 | 2896篇 |
免费 | 440篇 |
国内免费 | 307篇 |
专业分类
航空 | 1483篇 |
航天技术 | 1406篇 |
综合类 | 292篇 |
航天 | 462篇 |
出版年
2024年 | 5篇 |
2023年 | 57篇 |
2022年 | 70篇 |
2021年 | 133篇 |
2020年 | 132篇 |
2019年 | 122篇 |
2018年 | 156篇 |
2017年 | 120篇 |
2016年 | 102篇 |
2015年 | 98篇 |
2014年 | 192篇 |
2013年 | 156篇 |
2012年 | 189篇 |
2011年 | 222篇 |
2010年 | 172篇 |
2009年 | 218篇 |
2008年 | 214篇 |
2007年 | 147篇 |
2006年 | 146篇 |
2005年 | 155篇 |
2004年 | 93篇 |
2003年 | 89篇 |
2002年 | 68篇 |
2001年 | 58篇 |
2000年 | 55篇 |
1999年 | 51篇 |
1998年 | 50篇 |
1997年 | 55篇 |
1996年 | 37篇 |
1995年 | 40篇 |
1994年 | 66篇 |
1993年 | 37篇 |
1992年 | 40篇 |
1991年 | 36篇 |
1990年 | 32篇 |
1989年 | 17篇 |
1988年 | 7篇 |
1987年 | 3篇 |
1986年 | 1篇 |
1984年 | 2篇 |
排序方式: 共有3643条查询结果,搜索用时 328 毫秒
101.
We present preliminary results from high resolution observations obtained with the Michelson Doppler Imager (MDI) instrument
on the SOHO of two large solar flares of 14 July 2000 and 24 November 2000. We show that rapid variations of the line-of-sight
magnetic field occured on a time scale of a few minutes during the flare explosions. The reversibility/irreversibility of
the magnetic field of both active regions is a very good tool for understanding how the magnetic energy is released in these
flares. The observed sharp increase of the magnetic energy density at the time of maximum of the solar flare could involve
an unknown component which deposited supplementary energy into the system.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
102.
张德荣 《沈阳航空工业学院学报》2005,22(3):65-69
太阳和木星的自转是不均匀的,纬度愈高,自转愈慢。据此,作者推测液态外地核的自转,也存在类似的不均匀性,而这种不均匀自转将对地壳板块运动产生影响。利用磁流体力学理论,阐明这类星球自转的不均匀性,是磁制动的不均匀性引起的。研究了磁制动对地壳板块运动影响的途径及表现方式,并举出实例证明这些表现方式的确存在,从而证明磁制动是影响地壳板块运动的一个极为重要的因素。 相似文献
103.
104.
在光晶格钟运行时,不停起伏的杂散磁场会引入一阶塞曼频移和二阶塞曼频移,从而影响光晶格钟的频率不稳定度。此外,突变的磁场可能导致激光频率参考到钟跃迁频率的伺服闭环过程发生不可恢复的失锁,从而阻碍光钟的持续运行。在实验中,光钟进行频率闭环锁定前,通常通过控制三维线圈对光钟主腔中心原子处的杂散磁场进行补偿。首先使用三维磁强计,对真空主腔附近的磁场进行监测和记录,以分析杂散磁场对光钟性能的影响。然后利用正态分布模型和二项分布模型等,对光钟频率伺服锁定过程的阿伦偏差进行仿真拟合。在引入实际磁场监测数据的基础上,模拟光钟频率的伺服锁定过程,分析其仿真结果可以得出:减小杂散磁场起伏和控制磁场漂移,在提高冷镱原子光钟的短期稳定性和长期稳定性方面具有重要意义。 相似文献
105.
电大尺寸散射体的RCS计算方法研究 总被引:1,自引:0,他引:1
为了更加有效的求解电大目标散射计算问题,在避免谐振区效应情况下获得复杂目标的隐身雷达散射截面(RCS)特性,引用混合场积分方程(CFIE),在快速算法的求解迭代过程中采用共轭梯度算法(CG)的收敛技术,能够稳定的求解电大尺寸的RCS。计算和分析了金属球双站RCS和金属立方体双站RCS,并和精确计算、相关参考文献进行了比较,证明了方法的正确性,计算结果稳定,在工程实际上有较大的应用价值。 相似文献
106.
陶瓷纤维梯度增强活塞的梯度方程研究 总被引:2,自引:1,他引:2
功能梯度材料零件具有单质材料零件无法比拟的理化性能优势,然而由于材料分布复杂以及对功能梯度材料本身性能研究不充分,使性能分析存在很多困难。论文应用复合材料热性能理论,采用有限元分析软件ADINA,分析陶瓷纤维梯度增强活塞(材料梯度方程的参数不同)的温度分布和应力分布,结果表明陶瓷纤维梯度层可以明显改变活塞温度分布,缓和由于热膨胀系数不匹配,在陶瓷纤维增强层与活塞本体交界处产生的应力。根据计算结果拟合出温度峰值、整体应力峰值和层间应力峰值与方程系数之间的曲线,并加以验证。 相似文献
107.
108.
Alexeev Igor I. Belenkaya Elena S. Bobrovnikov Sergey Yu. Kalegaev Vladimir V. 《Space Science Reviews》2003,107(1-2):7-26
A magnetohydrodynamic model of the solar wind flow is constructed using a kinematic approach. It is shown that a phenomenological
conductivity of the solar wind plasma plays a key role in the forming of the interplanetary magnetic field (IMF) component
normal to the ecliptic plane. This component is mostly important for the magnetospheric dynamics which is controlled by the
solar wind electric field. A simple analytical solution for the problem of the solar wind flow past the magnetosphere is presented.
In this approach the magnetopause and the Earth's bow shock are approximated by the paraboloids of revolution. Superposition
of the effects of the bulk solar wind plasma motion and the magnetic field diffusion results in an incomplete screening of
the IMF by the magnetopause. It is shown that the normal to the magnetopause component of the solar wind magnetic field and
the tangential component of the electric field penetrated into the magnetosphere are determined by the quarter square of the
magnetic Reynolds number. In final, a dynamic model of the magnetospheric magnetic field is constructed. This model can describe
the magnetosphere in the course of the severe magnetic storm. The conditions under which the magnetospheric magnetic flux
structure is unstable and can drive the magnetospheric substorm are discussed. The model calculations are compared with the
observational data for September 24–26, 1998 magnetic storm (Dst
min=−205 nT) and substorm occurred at 02:30 UT on January 10, 1997.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
109.
Yuri N. Kulikov Helmut Lammer Herbert I. M. Lichtenegger Thomas Penz Doris Breuer Tilman Spohn Rickard Lundin Helfried K. Biernat 《Space Science Reviews》2007,129(1-3):207-243
Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation,
heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary
atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect
of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun
arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal
balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic
chemical reactions and cooling by IR-radiating molecules like CO2, NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures
obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen
and high Jeans’ escape rates for heavier species like H2, He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO2, N2 and H2O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various
non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian
magnetosphere against solar wind induced ion pick up erosion. We find that the early martian magnetic field could decrease
the ion-related non-thermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost
its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the
young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations
for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount
of ∼250 bar of O+ ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial
ocean (TO (1 TO ∼1.39×1024 g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and
compare our findings with the results of preceding studies. 相似文献
110.