全文获取类型
收费全文 | 6088篇 |
免费 | 662篇 |
国内免费 | 502篇 |
专业分类
航空 | 3074篇 |
航天技术 | 1728篇 |
综合类 | 445篇 |
航天 | 2005篇 |
出版年
2024年 | 17篇 |
2023年 | 52篇 |
2022年 | 121篇 |
2021年 | 188篇 |
2020年 | 136篇 |
2019年 | 123篇 |
2018年 | 229篇 |
2017年 | 214篇 |
2016年 | 219篇 |
2015年 | 187篇 |
2014年 | 284篇 |
2013年 | 297篇 |
2012年 | 303篇 |
2011年 | 355篇 |
2010年 | 380篇 |
2009年 | 436篇 |
2008年 | 374篇 |
2007年 | 295篇 |
2006年 | 220篇 |
2005年 | 239篇 |
2004年 | 174篇 |
2003年 | 205篇 |
2002年 | 223篇 |
2001年 | 210篇 |
2000年 | 134篇 |
1999年 | 152篇 |
1998年 | 127篇 |
1997年 | 117篇 |
1996年 | 102篇 |
1995年 | 141篇 |
1994年 | 113篇 |
1993年 | 69篇 |
1992年 | 80篇 |
1991年 | 44篇 |
1990年 | 45篇 |
1989年 | 56篇 |
1988年 | 29篇 |
1987年 | 25篇 |
1986年 | 26篇 |
1985年 | 81篇 |
1984年 | 62篇 |
1983年 | 50篇 |
1982年 | 48篇 |
1981年 | 89篇 |
1980年 | 26篇 |
1979年 | 18篇 |
1978年 | 17篇 |
1977年 | 18篇 |
1976年 | 15篇 |
1972年 | 14篇 |
排序方式: 共有7252条查询结果,搜索用时 0 毫秒
991.
A three-dimensional (3-D) global hybrid simulation is carried out for the generation and structure of magnetic reconnection in the magnetosheath due to interaction of an interplanetary Tangential Discontinuity (TD) with the bow shock and magnetosphere. Runs are performed for solar wind TDs possessing different initial half-widths. As the TD propagates through the bow shock toward the magnetopause, it is greatly narrowed by a two-step compression processes, a "shock compression' followed by a subsequent ``convective compression'. In cases with a relatively thin solar wind TD, 3-D patchy reconnection is initiated in the transmitted TD, forming magnetosheath flux ropes. Multiple components of ion particles are present in the velocity distribution in the magnetosheath merging, accompanied by ion heating. For cases with a relatively wide initial TD, a dominant single X-line appears in the subsolar magnetosheath after the transmitted TD is narrowed. A shock analysis is performed for the detailed structure of magnetic reconnection in the magnetosheath. Rotational Discontinuity (RD)/Time-Dependent Intermediate Shock (TDIS) are found to dominate the reconnection layer, which and some weak slow shocks are responsible for the ion heating and acceleration. 相似文献
992.
Orbital experimental researches on crystal growth of Mn-doped GaSb and Bi2Se0.21Te2.79 are briefly summarized. The space experiments were completed in September of 2007 on broad the Foton-M3 satellite of Russia. Ground-based researches on the solidification behaviors of Al-Al3Ni, Al-Al2Cu, Ag-Cu eutectic, Al-Pb monotectic and Cu-Co peritectic alloys in a 50-meter-high drop tube were investigated. New experimental results on the ultrasonic field and the temperature recycling induced to chiral symmetry breaking of NaClO3 crystal also were reported in the present paper. 相似文献
993.
刘杨 濮祖荫 谢伦 郭瑞龙 王晓钢 肖池阶 史全岐 DUNLOP M BOGDANOVA Y V MOORE T E RUSSELL C T LINDQVIST P A TORBERT R B POLLOCK C ZHAO Cong 《空间科学学报》2018,38(2):147-168
利用MMS观测数据,对磁层顶通量绳内离子惯性尺度(di)的结构进行分析研究.结果发现,许多不同尺度(约1di至数十di)的通量绳内都存在具有di尺度的电流 j m,其方向在磁层顶局地坐标系的-M方向,即与磁层顶查普曼-费拉罗电流同向,由电子在+M方向的运动( v em)携带.这些电流结构具有以下特征:磁鞘与磁层成分混合,磁场为开放形态;离子去磁化,电子与磁场冻结;N方向(即垂直于磁层顶电流片方向)的电场 E n显著增大,幅度达到约20mV·m-1,并伴有明显的尖峰状起伏,该增强和尖峰状起伏的电场对应于霍尔电场.分析表明,电流、电子与离子运动的偏离以及霍尔电场之间遵从广义欧姆定律,三者密切关联.进一步对磁层顶磁重联的探测数据进行分析发现,在很多重联区内也存在与通量绳内相似的结构,其尺度约为di量级,其中霍尔电场 E N、电流 j M和电子速度 v eM均与通量绳内对应物理量的方向相同且幅度相近.基于上述观测事实,采用经典FTE通量绳模型,对通量绳内电流、电子运动和霍尔电场的起源进行了初步探讨,认为其来源于磁层顶无碰撞磁重联区内的相应结构,并且后者在离子尺度通量绳的形成过程中起到重要作用. 相似文献
994.
995.
文章利用AUTODYN软件对铝合金球形弹丸正撞击双层墙防护结构进行了仿真研究,比较了双层墙防护结构中铝合金材料和复合材料防护屏的防护性能。结果表明:在相同的面密度和构型下,双层墙防护结构中铝合金防护屏的防护效果优于复合材料防护屏。 相似文献
996.
利用2003-2016年期间子午工程海南站(19.5°N,109.1°E)数字测高仪观测到的电离层等离子体漂移数据,分析了高低两种太阳活动条件下纬向和垂直向漂移对近磁静、中等磁扰和强磁扰三种地磁活动水平的响应特性.结果表明:日间纬向漂移各季节均以西向为主,随地磁活动无明显变化,白天日出附近和夜间漂移在各季节均以东向为主,随地磁活动增强而减弱,减弱程度在分季最大,在夏季最小;日间垂直漂移在零值附近变化,且不受地磁活动和季节影响,日落附近漂移仅在分季受到地磁活动的抑制,午夜前垂直漂移在分季受到抑制,在冬季因强磁扰而反向,夏季无明显规律,子夜至日出后垂直漂移在各季节随地磁活动增强而减小.与赤道区Jicamarca相比,两地漂移对地磁活动的响应相近,但在幅度和相位上存在差异,这可能是两地区的地理位置、背景电场和风场结构等不同造成的. 相似文献
997.
ASF网格是提高增强型罗兰(Enhanced Long Range Navigation,eLoran)系统精度的重要方法。根据所在网格四个顶点的附加二次时延(Added Secondary Factor,ASF)值通过网格应用算法得到待测试点的ASF值,一定程度上比公式计算的ASF值更准确。在计算过程中,用户四个顶点ASF值的测量误差会传递给用户,同时内插算法本身也会引入误差,此时内插算法的选择尤为重要。本文通过仿真、分析比较几种常用的内插算法,得出结论:反距离插值算法引入的误差最大,双线应插值算法引入的误差最小,而且误差呈现一定层次感,网格从内到外误差逐渐减小。 相似文献
998.
The five main types of antisunward propagating energetic fluxes (particles and emission) may be thought of as well established to date, the effects of which lead to a particilar character of disturbance in the near-terrestrial environment (the Earth's magnetosphere, ionosphere and atmosphere). The strongest global restructuring of the magnetosphere and ionosphere is caused by fluxes of relatively dense n of 1-70 cm-3 at the Earth's orbit) Solar Wind (SW) quasi-neutral, low-energy (E < 10 keV) plasma which cause magnetospheric and ionospheric storms lasting 24 hours or longer. For that reason, main attention is given to their study at the initial stage of research. The physical essence of the method of predicting disturbances in the near-terrestrial space environment, the amplitude of which can be expressed in, for example, the Kp index units, involves:(1) identifying all the most geo-effective SW streams of type, (2) determing their sources on the solar disk,and (3) quantifying the correlations between the characteristics of their solar sources with a maximum value of the Kp-index that is caused by the concerned type of SW stream. Semi-phenomenological relations have been obtained, which relate parameters of type SW stream sources to characteristics of geomagnetic storms:storm commencement, the time at which the storm intensity reaches its maximum values, the storm duration,as well as to the storm amplitude expressed in terms of geomagnetic indeces. 相似文献
999.
Input data of the system are two-dimensional images and one-dimensional distributions of total and polarized solar emission at 5.2 cm wavelength obtained with SSRT. Together with photoheliograms, magnetograms, Hα-filtergrams and characteristics of active regions received from other sources, they form the initial database. The first stage includes superimposing the images, identifying microwave sources with active regions, assigning NOAA numbers to the sources, and determining for each active region the heliolatitude, extent, and inclination angle of the group's axis to the equator. These data are used to calculate the boundaries of longitude zones for each active region. A next stage involves determining the brightness temperatures of microwave sources less than the polarization distribution, the degree of polarization, and microwave emission flux, as well as calculating the parameters of microwave sources. Each parameter is assigned its own value of the weight factor, and the sum of values is used to draw the conclusion about the flare occurrence probability in each active region and on the Sun in general. 相似文献
1000.