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151.
D. Kucharski G. Kirchner H.-C. Lim F. Koidl 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
The nanosatellite BLITS (Ball Lens In The Space) demonstrates a successful design of the new spherical lens type satellite for Satellite Laser Ranging (SLR). The spin parameters of the satellite were calculated from more than 1000 days of SLR data collected from 6 High Repetition Rate (HRR) systems: Beijing, Changchun, Graz, Herstmonceux, Potsdam, Shanghai. 相似文献
152.
L. S. Anderson-Huang 《Space Science Reviews》1998,85(1-2):203-213
The chromosphere-corona transition region of the Sun enjoys both simplicities of character and complexities of character which
result from its very thin geometrical extent. The simplicities derive from the reasonably clear view of the energy balance
(both observationally and theoretically), while the complexities derive from both the proximity of the not-so-clearly viewed
regions below and above, and the almost certain convolutions and perhaps discontinuities in the three dimensional geometry
of the transition sheet. While observational resolution and spectral information has improved greatly in recent years, the
problems associated with a single vantage point, the Earth and its environs, have not gone away. To understand the transition
region we must resolve structures radially and temporally as well as in the plane of the sky.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
153.
AHP中判断矩阵元素最优估计值的误差分析 总被引:1,自引:1,他引:0
在AHP模型中,请一组专家对某一属性进行评价,通过适当的数学处理方法,可得判断矩阵元素的最优估计值,并根据残差来确定所求估计值是否达到精度要求,若不符合精度要求则需返还给专家进行重新评估。这是AHP中构造判断矩阵的一种新方法。 相似文献
154.
155.
Jørgen Christensen-Dalsgaard 《Space Science Reviews》1998,85(1-2):19-36
The ‘standard’ solar model is based on a number of simplifying assumptions and depends on knowledge of the physical properties
of matter in the Sun. Given these assumptions, the constraint that the model have the observed surface luminosity provides
an estimate of the initial solar helium abundance. From helioseismic analyses further information can be obtained about the
present composition, including a fairly precise measure of the envelope helium abundance and an estimate of the hydrogen profile
in the radiative interior. It must be emphasized, however, that these inferences may suffer from systematic error arising
from incomplete knowledge about the equation of state and opacity of the solar interior.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
156.
Robert H. Nichols Jr. 《Space Science Reviews》2000,92(1-2):113-122
Variations in the abundances of short-lived radionuclides such as 26Al (τ1/2 ≈ 0.74 Ma) and 53Mn (τ1/2 ≈ 3.7 Ma) in meteoritic solids may be used to infer relative formation intervals of these solids in the nebula at precisions
of less than 1 Ma. In a strict chronometric interpretation of the isotopic variations, whereby criteria such as spatial and
temporal isotopic homogeneity and closed system isotopic evolution are met, solid formation occurred in the nebula for at
least several million years. This is longer than some theoretical and astronomical estimates for the duration of the active
nebula. The evidence for live 41Ca (τ1/2 ≈ 0.10 Ma) in meteoritic inclusions further indicates that the onset of solid formation occurred quite early, perhaps within
a few hundred thousand years after the onset of the collapse of the sun's parent molecular cloud. Failure of the chronometric
interpretation may arise for a variety of reasons, including but not limited to, the late, inhomogeneous injection of material
from a nearby stellar source or the local production of short-lived radionuclides by an energetic particle irradiation, e. g., from T Tauri (X-wind) or galactic cosmic ray sources. Although some isotopic evidence exists that the criteria required
for a strict chronometric interpretation are not met by each of the short-lived chronometers, there is no compelling reason
to shorten the interval of solid formation in the nebula to less than 1 Ma.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
157.
158.
S. Bingert P. Zacharias H. Peter B.V. Gudiksen 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2010
The structure and dynamics of a box in a stellar corona can be modeled employing a 3D MHD model for different levels of magnetic activity. Depending on the magnetic flux through the surface the nature of the resulting coronal structures can be quite different. We investigate a model of an active region for two sunspots surrounded by magnetic field patches comparable in magnetic flux to the sunspots. The model results in emission from the model corona being concentrated in loop structures. In Gudiksen and Nordlund (2005) the loops seen in EUV and X-ray emission outline the magnetic field, following the general paradigm. However, in our model, where the magnetic field is far from a force-free state, the loops seen in X-ray emission do not follow the magnetic field lines. This result is of interest especially for loops as found in areas where the magnetic field emerging from active regions interacts with the surrounding network. 相似文献
159.
G.P. Wu G.L. Huang Y. Huang D.Y. Wang 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(6):984-987
Based upon the most efficient electron acceleration near the midplane of 3D non-neutral driven reconnecting current sheet (RCS) and the electrostatic wave excitation by the drift Maxwellian distribution of electrons in Vlasov simulation, we assume that the electrostatic waves mainly propagate opposite to the reconnecting electric field and investigated how these waves affect the electron acceleration. The main results are: (1) when the electron’s velocity equals to the phase speed of the waves, they will be trapped and have the different accelerating characteristics from the untrapped electrons through solving the momentum equations of electrons analytically; (2) the test particle simulations further prove that the number of the energetic electrons decreases with the increasing intensity of unstable waves, and the distribution of the energetic electrons takes on the double power-law. 相似文献
160.
Jie Chen Henrik Lundstedt Hongqi Zhang 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2010
In this paper, the twist values of ‘S’-shape transequatorial loops (TLs) from 1991 to 2001 are calculated, GOES soft X-ray flares dataset of the active regions connected by these TLs are investigated. The result shows the twist value of the TLs has a weak relation with the flare flux. There is no clear correlation between the twist value and the distance between the footpoint of TLs and location of flare in the corresponding active regions. 相似文献