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C.J. Rodriguez-Solano U. HugentoblerP. Steigenberger G. Allende-Alba 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
During Sun-Earth eclipse seasons, GPS-IIA satellites perform noon, shadow and post-shadow yaw maneuvers. If the yaw maneuvers are not properly taken into account in the orbit determination process, two problems appear: (1) the observations residuals increase since the modeled position of the satellite’s navigation antenna differs from the true position, and (2) the non-conservative forces like solar radiation pressure or Earth radiation pressure are mismodeled due to the wrong orientation of the satellite’s surfaces in space. 相似文献
754.
《中国航空学报》2016,(2):470-478
Chang'E-3 spacecraft was orbiting the Moon from December 6–14, 2013, and very long baseline interferometry(VLBI) observations were performed to improve the accuracy of its orbit determination. In the process of recording VLBI raw data, 2 bits quantization was implemented.Interesting phenomenon was that signal-to-noise ratio(SNR) of each VLBI station experienced periodical change and had large variation on amplitude while in the Moon's orbit, whereas SNR kept in a stable level after Chang'E-3 landed on the Moon. Influence of varying elevation angle on SNR was analyzed and compensation of 2 bits quantization harmonics to SNR calculation was investigated. Most importantly, telescope system noise temperature increase caused by the Moon was computed along the time of Chang'E-3 orbiting the Moon, and well matched SNR changing trend in terms of correlation coefficients. 相似文献
755.
Roberto Susino Alessandro Bemporad Sergio Dolei Angelos Vourlidas 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
We study the 3-D kinematics of a Coronal Mass Ejection (CME) using data acquired by the LASCO C2 and UVCS instruments on board SOHO, and the COR1 coronagraphs and EUVI telescopes on board STEREO. The event, which occurred on May 20, 2007, was a partial-halo CME associated with a prominence eruption. This is the first CME studied with UVCS data that occurred in the STEREO era. The longitudinal angle between the STEREO spacecrafts was ∼7.7° at that time, and this allowed us to reconstruct via triangulation technique the 3-D trajectory of the erupting prominence observed by STEREO/EUVI. Information on the 3-D expansion of the CME provided by STEREO/COR1 data have been combined with spectroscopic observations by SOHO/UVCS. First results presented here show that line-of-sight velocities derived from spectroscopic data are not fully in agreement with those previously derived via triangulation technique, thus pointing out possible limitations of this technique. 相似文献
756.
针对与后机身融合的一体化红外抑制器模型,采用数值模拟的方法研究了内部遮挡和出口修型对后机身表面温度场和红外辐射特性的影响。在混合管外部采用遮挡套或曲面遮挡板可有效降低后机身侧壁面对应混合管后段的局部区域最高温度,两种方式均可有效降低水平探测面以及铅垂面上方3~5 μm波段和8~14 μm波段红外辐射强度峰值;然而,加装遮挡套方式会影响旋翼下洗气流的导入,使3~5 μm波段的红外辐射强度在铅垂面下方较基准模型有小幅的增加。对后机身排气口进行出口修型,虽然对降低后机身3~5 μm和8~14 μm波段红外辐射强度的作用效果并不显著,但可以有效消除排气出口下方壁面的高温区,其中采用狭窄流道引气冷却方式可以使得后机身侧壁仅高于环境温度10 K左右。 相似文献
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遮挡板参数对二元喷管气动和红外辐射影响 总被引:1,自引:0,他引:1
采用计算流体力学/红外辐射强度数值计算的方法,以宽高比3.33二元收敛喷管为研究对象,计算分析了二元喷管加双层遮挡板结构对喷管气动和红外辐射影响.结果表明:二元喷管加遮挡板后,总压恢复系数系数和推力系数并未降低,在98.81%和95.15%以上;单层遮挡结构的二元喷管在绝大多数角度都比基准二元喷管高,且增加的幅度较大;与基准二元喷管相比较,双层遮挡板结构的喷管在-90°至-10°探测方向上红外辐射强度降低38%-80%,但是由于上遮挡板的存在,喷管上方(30°-90°)的红外辐射增强;遮挡间距增加,引射气流流量增加,上、下遮挡板红外辐射减小,当遮挡间距增加到35mm时,上遮挡板的红外辐射峰值降低到800W/Sr,下遮挡板红外辐射强度仅为4W/Sr左右.这说明了双层遮挡结构的二元喷管(喷口后延)在某些方向上有较强的红外抑制效果. 相似文献
760.
len Balman 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2006,38(12):2840-2843
I discuss morphology and spectrum of the first resolved and detected classical nova shell in the X-rays – the remnant of GK Persei (1901). The existence of such a nebulosity brings about the possibility of other nova remnants emitting X-rays. I calculate that the X-ray luminosity should be about 1026–1033 ergs s−1 on the onset of cooling for nova remnants. I have done an archival search on 250 classical and recurrent nova candidates using Chandra, XMM-Newton, ROSAT and ASCA databases. There is no significant extended emission detected which places an upper limit of Fx < × 10−12 erg s−1 cm−2 (unabsorbed). Only exceptions are GK Per, RR Pic and DQ Her (all observed by Chandra ACIS-S and GK Per also by ROSAT HRI) where the latter two show marginal extended emission in the X-rays associated with emission knots (DQ Her) or an equatorial ring (RR Pic). 相似文献