全文获取类型
收费全文 | 351篇 |
免费 | 50篇 |
国内免费 | 11篇 |
专业分类
航空 | 73篇 |
航天技术 | 257篇 |
综合类 | 13篇 |
航天 | 69篇 |
出版年
2023年 | 8篇 |
2022年 | 8篇 |
2021年 | 6篇 |
2020年 | 14篇 |
2019年 | 13篇 |
2018年 | 12篇 |
2017年 | 4篇 |
2016年 | 2篇 |
2015年 | 7篇 |
2014年 | 20篇 |
2013年 | 25篇 |
2012年 | 23篇 |
2011年 | 30篇 |
2010年 | 18篇 |
2009年 | 24篇 |
2008年 | 35篇 |
2007年 | 21篇 |
2006年 | 14篇 |
2005年 | 21篇 |
2004年 | 16篇 |
2003年 | 6篇 |
2002年 | 8篇 |
2001年 | 14篇 |
2000年 | 13篇 |
1999年 | 6篇 |
1998年 | 5篇 |
1997年 | 4篇 |
1996年 | 5篇 |
1995年 | 8篇 |
1994年 | 11篇 |
1993年 | 3篇 |
1992年 | 2篇 |
1991年 | 1篇 |
1990年 | 1篇 |
1989年 | 2篇 |
1988年 | 1篇 |
1987年 | 1篇 |
排序方式: 共有412条查询结果,搜索用时 515 毫秒
291.
292.
B.W. Joshua J.O. Adeniyi B.W. Reinisch I.A. Adimula A.O. Olawepo O.A. Oladipo S.J. Adebiyi 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2014
The effects of some geomagnetic storms on the F2 layer peak parameters over Ilorin, Nigeria (Lat. 8:53°N, Long. 4.5°E, dip angle, −2.96°) have been investigated. Our results showed that the highest intensity of the noon bite-out occurred during the March equinox and lowest during the June Solstice on quiet days. Quiet day NmF2 disturbances which appeared as a pre-storm enhancement, but not related to the magnetic storm event that followed were observed at this station. These enhancements were attributed to the modification of the equatorial electric field as a result of injection of the Auroral electric field to the low and equatorial ionosphere. For disturbed conditions, the morphology of the NmF2 on quiet days is altered. Daytime and nighttime NmF2 and hmF2 enhancements were recorded at this station. Decreases in NmF2 were also observed during the recovery periods, most of which appeared during the post-noon period, except the storm event of May 28–29. On the average, enhancements in NmF2 (i.e. Positive phases) are the prominent features of this station. Observations from this study also indicate that Dst, Ap and Kp which have been the most widely used indices in academic research in describing the behavior of geomagnetic storms, are not sufficient for storm time analysis in the equatorial and low latitude ionosphere. 相似文献
293.
K.-I. Nishikawa J. Niemiec M. Medvedev B. Zhang P. Hardee A. Nordlund J. Frederiksen Y. Mizuno H. Sol M. Pohl D.H. Hartmann M. Oka G.J. Fishman 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
Using our new 3-D relativistic particle-in-cell (PIC) code parallelized with MPI, we investigated long-term particle acceleration associated with a relativistic electron–positron jet propagating in an unmagnetized ambient electron–positron plasma. The simulations were performed using a much longer simulation system than our previous simulations in order to investigate the full nonlinear stage of the Weibel instability and its particle acceleration mechanism. Cold jet electrons are thermalized and ambient electrons are accelerated in the resulting shocks. Acceleration of ambient electrons leads to a maximum ambient electron density three times larger than the original value as predicted by hydrodynamic shock compression. In the jet (reverse) shock behind the bow (forward) shock the strongest electromagnetic fields are generated. These fields may lead to time dependent afterglow emission. In order to calculate radiation from first principles that goes beyond the standard synchrotron model used in astrophysical objects we have used PIC simulations. Initially we calculated radiation from electrons propagating in a uniform parallel magnetic field to verify the technique. We then used the technique to calculate emission from electrons in a small simulation system. From these simulations we obtained spectra which are consistent with those generated from electrons propagating in turbulent magnetic fields with red noise. This turbulent magnetic field is similar to the magnetic field generated at an early nonlinear stage of the Weibel instability. A fully developed shock within a larger simulation system may generate a jitter/synchrotron spectrum. 相似文献
294.
295.
296.
磁场影响葡萄糖氧化酶活性的研究 总被引:5,自引:0,他引:5
以尼龙网作载体,用戊二醛交联将区区糖氧化酶(GOD)固定装成酶柱并联结于流动体系中,采用流动注射分光光度法研究磁场对固定化GOD催化活性的影响。结果表明,在0℃、5℃、45℃下以1.0×10^-2mol.L^-1的葡萄糖为底物及55℃下以0.1mol^-1的葡萄糖为底物时,0.22T静有显著提高固定化GOD的反应速度,且磁场效应与底物浓度及磁场作用时间有关。用动力学方法考察了不同强度的磁场对溶解G 相似文献
297.
M.V. Alania R. Modzelewska A. Wawrzynczak 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2010
We develop a three-dimensional (3-D) model of the 27-day variation of galactic cosmic-ray (GCR) intensity with a spatial variation of the solar wind velocity. A consistent, divergence-free interplanetary magnetic field is derived by solving the corresponding Maxwell equations with a variable solar wind speed, which reproduces in situ observed experimental data for the time interval to be analyzed (24 August 2007–28 February 2008). We perform model calculations for the GCR intensity using the variable solar wind and the corresponding magnetic field. Results are compatible with experimental data; the correlation coefficient between our model predictions and observed 27-day GCR variation is 0.80 ± 0.05. 相似文献
298.
Naoya Maeda Satoko Takasaki Hideaki Kawano Shinichi Ohtani P.M.E. Décréau J.G. Trotignon S.I. Solovyev D.G. Baishev Kiyohumi Yumoto 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
By applying the cross-phase method and the amplitude-ratio method to magnetic field data obtained from two ground stations located close to each other, we can determine the frequency of the field line resonance (FLR), or the field line eigenfrequency, for the field line running through the midpoint of the two stations. From thus identified FLR frequency we can estimate the equatorial plasma mass density (ρ) by using the T05s magnetospheric field model [Tsyganenko, N.A., Sitnov, M.I. Modeling the dynamics of the inner magnetosphere during strong geomagnetic storms, J. Geophys. Res. 110, A03208, 2005] and the equation of Singer et al. [Singer, H.J., Southwood, D.J., Walker, R.J., Kivelson, M.G. Alfven wave resonances in a realistic magnetospheric magnetic field geometry, J. Geophys. Res. 86 (A6) 4589–4596, 1981]. 相似文献
299.
300.
We investigate the properties of interplanetary inhomogeneities generating long-lasting mid-latitude Pc1, 2 geomagnetic pulsations. The data from the Wind and IMP 8 spacecrafts, and from the Mondy and Borok midlatitude magnetic observatories are used in this study. The pulsations under investigation develop in the maximum and early recovery phase of magnetic storms. The pulsations have amplitudes from a few tens to several hundred pT andlast more than seven hours. A close association of the increase (decrease) in solar wind dynamic pressure (Psw) with the onset or enhancement (attenuation or decay) of these pulsations has been established. Contrary to high-latitude phenomena, there is a distinctive feature of the interplanetary inhomogeneities that are responsible for generation of long-lasting mid-latitude Pc1, 2. It is essential that the effect of the quasi-stationary negative Bz-component of the interplanetary magnetic field on the magnetosphere extends over 4 hours. Only then are the Psw pulses able to excite the above-mentioned type of mid-latitude geomagnetic pulsations. Model calculations show that in the cases under study the plasmapause can form in the vicinity of the magnetic observatory. This implies that the existence of an intense ring current resulting from the enhanced magnetospheric convection is necessary for the Pc1, 2 excitation. Further, the existence of the plasmapause above the observation point (as a waveguide) is necessary for long-lasting Pc1 waves to arrive at the ground. 相似文献