全文获取类型
收费全文 | 1563篇 |
免费 | 149篇 |
国内免费 | 160篇 |
专业分类
航空 | 481篇 |
航天技术 | 1028篇 |
综合类 | 73篇 |
航天 | 290篇 |
出版年
2024年 | 3篇 |
2023年 | 40篇 |
2022年 | 24篇 |
2021年 | 78篇 |
2020年 | 39篇 |
2019年 | 51篇 |
2018年 | 59篇 |
2017年 | 37篇 |
2016年 | 33篇 |
2015年 | 34篇 |
2014年 | 108篇 |
2013年 | 89篇 |
2012年 | 91篇 |
2011年 | 126篇 |
2010年 | 104篇 |
2009年 | 118篇 |
2008年 | 122篇 |
2007年 | 83篇 |
2006年 | 55篇 |
2005年 | 95篇 |
2004年 | 52篇 |
2003年 | 31篇 |
2002年 | 47篇 |
2001年 | 35篇 |
2000年 | 42篇 |
1999年 | 23篇 |
1998年 | 38篇 |
1997年 | 35篇 |
1996年 | 27篇 |
1995年 | 28篇 |
1994年 | 39篇 |
1993年 | 19篇 |
1992年 | 26篇 |
1991年 | 18篇 |
1990年 | 15篇 |
1989年 | 5篇 |
1988年 | 2篇 |
1987年 | 1篇 |
排序方式: 共有1872条查询结果,搜索用时 196 毫秒
1.
航天应用的液体火箭发动机及燃烧型加热器燃烧室室压高、燃料流量大、温度低、有重复启动需求,实现安全可靠点火的难度较大。针对这些需求,研究了一种采用高背压设计的电弧等离子体点火器。实验研究了Ar,N2气体工质在高进气压力下的伏安特性,发现N2在宽压力范围内适用于点火。发射光谱分析表明,在高达数MPa的进气压力下,Ar,N2等离子体射流电子密度符合局部热力学平衡判据(LTE判据),点火能量集中。N2等离子体整体温度低于Ar,但阳极喷口附近温度高于Ar,N2等离子体射流火焰长,卷吸沿程空气造成射流平均温度偏低,但有助于低温液体推进剂的蒸发混合和强化点火。等离子体射流引起了臭氧和氮氧化物的形成,具有促进点火和化学反应的作用。背压提高引起电源输出电压升高,提高供气压力和电流,有助于点火器在高背压环境中稳定电压。燃烧型空气加热器燃烧室的点火实验发现,采用N2等离子体喷注面中心点火,可以在短时间内完成酒精-空气和酒精-液氧-空气的点火,最高燃烧室室压接近5MPa时,点火器仍能稳定工作,多次使用电极烧蚀不明显,在液体火箭发动机的重复可靠点火方面具有很好的应用前景。 相似文献
2.
Mingying Huo Giovanni Mengali Alessandro A. Quarta 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2018,61(10):2617-2627
Propellantless continuous-thrust propulsion systems, such as electric solar wind sails, may be successfully used for new space missions, especially those requiring high-energy orbit transfers. When the mass-to-thrust ratio is sufficiently large, the spacecraft trajectory is characterized by long flight times with a number of revolutions around the Sun. The corresponding mission analysis, especially when addressed within an optimal context, requires a significant amount of simulation effort. Analytical trajectories are therefore useful aids in a preliminary phase of mission design, even though exact solution are very difficult to obtain. The aim of this paper is to present an accurate, analytical, approximation of the spacecraft trajectory generated by an electric solar wind sail with a constant pitch angle, using the latest mathematical model of the thrust vector. Assuming a heliocentric circular parking orbit and a two-dimensional scenario, the simulation results show that the proposed equations are able to accurately describe the actual spacecraft trajectory for a long time interval when the propulsive acceleration magnitude is sufficiently small. 相似文献
3.
为了研究冰冻天体表面撞击坑的形成与演化,开展了水冰的超高速撞击成坑实验。使用二级轻气炮发射1.0 mm直径的球形弹丸,以3 km/s、5 km/s和7 km/s速度对圆柱状冰块进行撞击。弹丸材料包括聚碳酸酯和不锈钢两种,冰块温度为253 K。实验观察到了不同弹丸和不同速度条件下,冰块中撞击坑的形貌特征。对撞击坑直径、深度和剖面形状进行了测量,并与文献中铝弹丸对水冰的撞击坑进行了比较分析。获得了水冰撞击坑特征随撞击参数的变化规律,结果表明:撞击坑直径和深度的主导机制不同,坑深主要由弹丸侵彻作用形成,而坑径主要由冰块的剥落所致;坑深比坑径具有更强的对于弹丸密度的依赖性,高密度弹丸撞击坑直径具有比低密度弹丸更强的对于撞击速度的依赖性;撞击坑体积与撞击能量成正比,高密度弹丸形成的撞击坑直径表现出“能量缩比”行为,而低密度弹丸形成的撞击坑直径表现出“动量缩比”行为。 相似文献
4.
《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2020,65(11):2551-2558
The whistler-mode chorus waves are one of the most important plasma waves in the Earth’s magnetosphere. Generally, the amplitude of whistler-mode chorus waves prefers to strengthen when the energetic fluxes of anisotropic electrons increase outside the plasmapause. This characteristic is commonly associated with the geomagnetic storms or substorms. However, the relationship between the solar wind dynamic pressure (Psw) and the long-time variation of chorus waves during the quiet period of the geomagnetic activity still needs more detailed investigations. In this paper, based on MMS observations, we present a chorus event just observed in the inner side of magnetopause without obvious geomagnetic storms or substroms. Interestingly, during this time interval, some Psw fluctuations were recorded. Both the amplitudes and frequencies of chorus waves changed as a response to the variation in Psw. It proved that the enhancement of Psw increases the energetic electrons fluxes, which provides free energies for the chorus amplification. Furthermore, the wave growth rates calculated using linear theory increases and the central frequency of the chorus waves shifts to a higher frequency when the Psw enhancement is greater, which are also consistent well with the observations. The results provide a direct evidence that the Psw play an important role in the long-time variation of whistler-mode chorus waves inside the magnetopause. 相似文献
5.
摘要: 为了更好地满足航空航天领域中使用的多种嵌入式软件的高可靠性要求,设计一种软件脆弱性自动分析定位的方法.该方法基于程序切片技术,改进现有的前向计算动态切片算法,利用动态程序切片收集程序运行时的动态信息,构造程序切片谱,设定相关统计量统计程序语句的脆弱性可疑度,生成脆弱性定位报告.在发现软件中存在的脆弱性后,该方法对导致此脆弱性的程序代码根源实现了自动分析定位.基于此方法设计开发了软件脆弱性自动定位工具并进行了实例验证分析,实验证明了该方法的有效性. 相似文献
6.
Facundo L. Poblet Francisco Azpilicueta 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2018,61(9):2275-2289
The Earth and the near interplanetary medium are affected by the Sun in different ways. Those processes generated in the Sun that induce perturbations into the Magnetosphere-Ionosphere system are called geoeffective processes and show a wide range of temporal variations, like the 11-year solar cycle (long term variations), the variation of ~27?days (recurrent variations), solar storms enduring for some days, particle acceleration events lasting for some hours, etc.In this article, the periodicity of ~27?days associated with the solar synodic rotation period is investigated. The work is mainly focused on studying the resulting 27-day periodic signal in the magnetic activity, by the analysis of the horizontal component of the magnetic field registered on a set of 103 magnetic observatories distributed around the world. For this a new method to isolate the periodicity of interest has been developed consisting of two main steps: the first one consists of removing the linear trend corresponding to every calendar year from the data series, and the second one of removing from the resulting series a smoothed version of it obtained by applying a 30-day moving average. The result at the end of this process is a data series in which all the signal with periods larger than 30?days are canceled.The most important characteristics observed in the resulting signals are two main amplitude modulations: the first and most prominent related to the 11-year solar cycle and the second one with a semiannual pattern. In addition, the amplitude of the signal shows a dependence on the geomagnetic latitude of the observatory with a significant discontinuity at approx. ±60°.The processing scheme was also applied to other parameters that are widely used to characterize the energy transfer from the Sun to the Earth: F10.7 and Mg II indices and the ionospheric vertical total electron content (vTEC) were considered for radiative interactions; and the solar wind velocity for the non-radiative interactions between the solar wind and the magnetosphere. The 27-day signal obtained in the magnetic activity was compared with the signals found in the other parameters resulting in a series of cross-correlations curves with maximum correlation between 3 and 5?days of delays for the radiative and between 0 and 1?days of delay for the non-radiative parameters. This result supports the idea that the physical process responsible for the 27-day signal in the magnetic activity is related to the solar wind and not to the solar electromagnetic radiation. 相似文献
7.
Junhyeok Jeon Young-Joo Kwon Yong-Sam Lee 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2018,61(8):2116-2123
Observing Venus during the daytime is challenging. However, observational data of Venus during the daytime can be found in history books from East Asian countries such as Korea, China and Japan. In this study, we are focused on data from Korean history book, and using records left in the Joseon wangjo sillok, one of the Korean history books from the Joseon dynasty (CE 1392–1910), tries to prove whether the reported observations were actual observation data. We collected these 4663 records from the Joseon wangjo sillok to determine whether they were actual observations, and to confirm the scientific validity of the records. When we looked at the distribution of observations on a yearly basis, we noticed that there were more observations in the fall and winter, while there were only limited numbers of observations in the spring. This difference in distribution suggests that observations were strongly affected by atmospheric conditions due to the weather. From the 4663 data collected, we found a cycle of about 1.6?years. The cycle of about 1.6?years is assumed to be related to the conjunction cycle of Venus. And, we found a cycle of about 1.0?years. The cycle of about 1.0?years is assumed to reflect the indirect effects of the Asian dust phenomenon. Our research result verified the record as actual observational data. In addition, this result verified that meteorological factors were involved in the recorded astronomical observation data. We think that our data can be helpful to climate studies on the natural sources of key climate-affecting aerosols. 相似文献
8.
9.
Profiles of the visible Fe X (6374 Å) coronal emission line as a function of height above the limb were obtained out to 1.16 solar radii in a coronal hole using the NSO/Sacramento Peak Observatory Coronagraph, Universal Spectrograph and a CCD camera. These are the first coronal line profiles obtained as a function of height in a coronal hole from the ground. Analysis of the line widths suggests a large component of nonthermal broadening which increases with height ranging from 40 to 60 km/s, depending upon the assumed temperature or thermal component of the profile. 相似文献
10.
Although the elemental composition in all parts of the solar photosphere appears to be the same this is clearly not the case
with the solar upper atmosphere (SUA). Spectroscopic studies show that in the corona elemental composition along solar equatorial
regions is usually different from polar regions; composition in quiet Sun regions is often different from coronal hole and
active region compositions and the transition region composition is frequently different from the coronal composition along
the same line of sight. In the following two issues are discussed. The first involves abundance ratios between the high-FIP
O and Ne and the low-FIP Mg and Fe that are important for meaningful comparisons between photospheric and SUA compositions
and the second involves a review of composition and time variability of SUA plasmas at heights of 1.0≤h≤1.5R
⊙. 相似文献