全文获取类型
收费全文 | 665篇 |
免费 | 35篇 |
国内免费 | 20篇 |
专业分类
航空 | 299篇 |
航天技术 | 305篇 |
综合类 | 26篇 |
航天 | 90篇 |
出版年
2024年 | 1篇 |
2023年 | 25篇 |
2021年 | 5篇 |
2020年 | 17篇 |
2019年 | 17篇 |
2018年 | 14篇 |
2017年 | 2篇 |
2016年 | 3篇 |
2015年 | 4篇 |
2014年 | 48篇 |
2013年 | 19篇 |
2012年 | 18篇 |
2011年 | 25篇 |
2010年 | 18篇 |
2009年 | 35篇 |
2008年 | 60篇 |
2007年 | 60篇 |
2006年 | 32篇 |
2005年 | 31篇 |
2004年 | 12篇 |
2003年 | 18篇 |
2002年 | 8篇 |
2001年 | 44篇 |
2000年 | 13篇 |
1999年 | 13篇 |
1998年 | 26篇 |
1997年 | 2篇 |
1996年 | 17篇 |
1995年 | 15篇 |
1994年 | 86篇 |
1993年 | 17篇 |
1992年 | 3篇 |
1991年 | 3篇 |
1990年 | 3篇 |
1989年 | 2篇 |
1984年 | 4篇 |
排序方式: 共有720条查询结果,搜索用时 234 毫秒
471.
The differences between the composition of Galactic cosmic rays and that of the interstellar medium are manifold, and they
contain a wealth of information about the varying processes that created them. These differences reveal much about the initial
mixing of freshly synthesized matter, the chemistry and differentiation of the interstellar medium, and the mechanisms and
environment of ion injection and acceleration. Here we briefly explore these processes and show how they combine to create
the peculiar, but potentially universal, composition of the cosmic rays and how measurements of the composition can provide
a unique measure of the mixing ratio of the fresh supernova ejecta and the old interstellar medium in this initial phase of
interstellar mixing.
In particular, we show that the major abundance differences between the cosmic rays and the average interstellar medium can
all result from cosmic ray ion injection by sputtering and scattering from fast refractory oxide grains in a mix of fresh
supernova ejecta and old interstellar material. Since the bulk of the Galactic supernovae occur in the cores of superbubbles,
the bulk of the cosmic rays are accelerated there out of such a mix. We show that the major abundance differences all imply
a mixing ratio of the total masses of fresh supernova ejecta and old interstellar material in such cores is roughly 1 to 4.
That means that the metallicity of ∼3 times solar, since the ejecta has a metallicity of ∼8 times that of the present interstellar
medium. 相似文献
472.
刘思俊 《西安航空技术高等专科学校学报》2005,23(4):17-18
正确地指导好高职高专在校生的专升本,是每位老师应尽的责任和义务。笔从近几年高职高专在校生专升本的实际出发,分析探讨了高职高专在校生专升本可能遇到的困难和问题,以及如何正确引导学生克服困难,找出解决这些问题的思路和方法。 相似文献
473.
J. S. Kaastra A. M. Bykov S. Schindler J. A. M. Bleeker S. Borgani A. Diaferio K. Dolag F. Durret J. Nevalainen T. Ohashi F. B. S. Paerels V. Petrosian Y. Rephaeli P. Richter J. Schaye N. Werner 《Space Science Reviews》2008,134(1-4):1-6
We present the work of an international team at the International Space Science Institute (ISSI) in Bern that worked together
to review the current observational and theoretical status of the non-virialised X-ray emission components in clusters of
galaxies. The subject is important for the study of large-scale hierarchical structure formation and to shed light on the
“missing baryon” problem. The topics of the team work include thermal emission and absorption from the warm-hot intergalactic
medium, non-thermal X-ray emission in clusters of galaxies, physical processes and chemical enrichment of this medium and
clusters of galaxies, and the relationship between all these processes. One of the main goals of the team is to write and
discuss a series of review papers on this subject. These reviews are intended as introductory text and reference for scientists
wishing to work actively in this field. The team consists of sixteen experts in observations, theory and numerical simulations. 相似文献
474.
Yanxia Zhang Yongheng Zhao Dan Gao 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(12):1949-1954
With the availability of multi-wavelength, multi-scale and multi-epoch astronomical catalogues, the number of features to describe astronomical objects has increases. The better features we select to classify objects, the higher the classification accuracy is. In this paper, we have used data sets of stars and quasars from near-infrared band and radio band. Then best-first search method was applied to select features. For the data with selected features, the algorithm of decision table was implemented. The classification accuracy is more than 95.9%. As a result, the feature selection method improves the effectiveness and efficiency of the classification method. Moreover the result shows that decision table is robust and effective for discrimination of celestial objects and used for preselecting quasar candidates for large survey projects. 相似文献
475.
当前万维网服务发现机制并没有考虑消费者对服务质量的需求,消费者需要花很多时间来选择满足自己服务质量的服务.采取了一个QoS (Quality of Service)过滤器,采用服务质量属性量化方法和一个服务质量匹配算法来选取符合消费者服务质量要求的服务,并把服务存储在本地缓存中.这种方法考虑到消费者对服务质量的要求,减少访问远程发现服务器的次数,加快了服务发现速度.通过对本地服务添加标注和关键字来支持消费者服务的个性化. 相似文献
476.
Nikolaus Peter Schmitt Wolfgang Rehm Thomas Pistner Paul Zeller Hermann Diehl Peter Nav 《Aerospace Science and Technology》2007,11(7-8):546-552
The development and first flight tests are described of a short pulse direct measuring UV LIDAR for the measurement of gusts, turbulence and potentially wake vortices. The results of these stage 1 tests confirm that relative wind velocities can be measured with a standard deviation of below 10 m/s even at high altitudes with no appreciable aerosol concentrations. Operating the system under various flight conditions including rain, dense clouds, and clear air up to 24,000 ft was highly successful. Means to push the standard deviation below 1.6 m/s, foremost by increasing the laser output power and the efficiency of the light collecting system, are identified and quantified. Questions of instrument stability are addressed. 相似文献
477.
How to exploit the Sun as a gravitational lens has been studied extensively during the last 20 years, especially by this author (Refs. 1, 2, 3, 4, 5, 6 and 7). In essence, a spacecraft dubbed FOCAL (an acronym for “Fast Outgoing Cyclopean Astronomical Lens”) should be launched in the direction of the sky opposite to the area of the sky we wish to see highly magnified both at radio and other frequencies. After FOCAL reached the minimal focal distance of 550 AU from the Sun, highly magnified radio images of celestial objects located on the opposite side of the Sun will automatically be produced. In this paper we apply the FOCAL mission concept to the goal of exploring the neighborhood of the Alpha Centauri B star, where the nearest exoplanet to the Solar system was recently discovered. We suggest that: 相似文献
478.
Jie Jiang Jingxiu Wang 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(6):874-880
The generation of solar non-axisymmetric magnetic fields is studied based on a linear α2–Ω dynamo model in a rotating spherical frame. The model consists of a solar-like differential rotation, a magnetic diffusivity varied with depth, and three types of α-effects with different locations, i.e. the tachocline, the whole convective zone and the sub-surface. Some comparisons of the critical α-values of axisymmetric (m = 0) and longitude-dependent modes (m = 1,2,3) are presented to show the roles of the magnetic diffusivity in the problem of modes selection. With the changing of diffusivity intensity for the given solar differential rotation system, the dominant mode possibly changes likewise and the stronger the diffusivity is, the easier the non-axisymmetric modes are excited. The influence of the diffusivity and differential rotation on the configurations of the dominant modes are also presented. 相似文献
479.
The James Webb Space Telescope 总被引:4,自引:0,他引:4
Jonathan P. Gardner John C. Mather Mark Clampin Rene Doyon Matthew A. Greenhouse Heidi B. Hammel John B. Hutchings Peter Jakobsen Simon J. Lilly Knox S. Long Jonathan I. Lunine Mark J. Mccaughrean Matt Mountain John Nella George H. Rieke Marcia J. Rieke Hans-Walter Rix Eric P. Smith George Sonneborn Massimo Stiavelli H. S. Stockman Rogier A. Windhorst Gillian S. Wright 《Space Science Reviews》2006,123(4):485-606
The James Webb Space Telescope (JWST) is a large (6.6 m), cold (<50 K), infrared (IR)-optimized space observatory that will be launched early in the next decade into orbit around the second Earth–Sun Lagrange point. The observatory will have four instruments: a near-IR camera, a near-IR multiobject spectrograph, and a tunable filter imager will cover the wavelength range, 0.6 < ; < 5.0 μ m, while the mid-IR instrument will do both imaging and spectroscopy from 5.0 < ; < 29 μ m.The JWST science goals are divided into four themes. The key objective of The End of the Dark Ages: First Light and Reionization theme is to identify the first luminous sources to form and to determine the ionization history of the early universe. The key objective of The Assembly of Galaxies theme is to determine how galaxies and the dark matter, gas, stars, metals, morphological structures, and active nuclei within them evolved from the epoch of reionization to the present day. The key objective of The Birth of Stars and Protoplanetary Systems theme is to unravel the birth and early evolution of stars, from infall on to dust-enshrouded protostars to the genesis of planetary systems. The key objective of the Planetary Systems and the Origins of Life theme is to determine the physical and chemical properties of planetary systems including our own, and investigate the potential for the origins of life in those systems. Within these themes and objectives, we have derived representative astronomical observations.To enable these observations, JWST consists of a telescope, an instrument package, a spacecraft, and a sunshield. The telescope consists of 18 beryllium segments, some of which are deployed. The segments will be brought into optical alignment on-orbit through a process of periodic wavefront sensing and control. The instrument package contains the four science instruments and a fine guidance sensor. The spacecraft provides pointing, orbit maintenance, and communications. The sunshield provides passive thermal control. The JWST operations plan is based on that used for previous space observatories, and the majority of JWST observing time will be allocated to the international astronomical community through annual peer-reviewed proposal opportunities. 相似文献
480.
Arnab Rai Choudhuri 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(6):868-873
Over the last few years, dynamo theorists seem to be converging on a basic scenario as to how the solar dynamo operates. The strong toroidal component of the magnetic field is produced in the tachocline, from where it rises due to magnetic buoyancy to produce active regions at the solar surface. The decay of tilted bipolar active regions at the surface gives rise to the poloidal component, which is first advected poleward by the meridional circulation and then taken below the surface to the tachocline where it can be stretched to produce the toroidal component. The mathematical formulation of this basic model, however, involves the specification of some parameters which are still uncertain. We review these remaining uncertainties which have resulted in disagreements amongst various research groups and have made it impossible to still arrive at something that can be called a standard model of the solar dynamo. 相似文献