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211.
A. Kepa B. SylwesterM. Siarkowski J. Sylwester 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008
X-ray spectrometer RESIK has observed spectra in the four wavelength bands from 3.3 Å to 6.1 Å. This spectral range contains many emission lines of H- and He-like ions for Si, S, Ar and K. These lines are formed in plasma of coronal temperatures (T > 3 MK). Analysis of their intensities allows studying differential emission measure distributions (DEM) in temperature range roughly between 3 MK and 30 MK. The aim of present study was to check whether any relationship exists between the character of DEM distribution, the event phase and the X-ray flare class. To do this we have calculated and analyzed the DEM distributions for a set of flares belonging to different GOES classes from the range B5.6–X1. The DEM distributions have been calculated using “Withbroe–Sylwester” multiplicative, maximum likelihood iterative algorithm. As the input data we have used absolute fluxes observed by RESIK in several spectral bands (lines + continuum). Respective emission functions have been calculated using the CHIANTI v. 5.2 atomic data package. 相似文献
212.
稀土钇提高离子镀TiN膜层与基体结合力的研究 总被引:2,自引:0,他引:2
研究了稀土钇不同含量时对离子镀TiN膜层与基体结合力的影响.用扫描电镜,俄歇谱仪,X射线衍射等手段,对加入稀土钇的TiN膜层作了分析。结果表明,加适量稀土钇后,TiN膜层与基体的结合力大大提高。其微观机制是,加稀土钇后,膜层相组成发生变化,在膜-基之间形成一过渡层,塑性相(Ti相)增加,脆性相(Ti2N)减少,从而减小了膜-基界面间的应力。此外,结果还表明,稀土钇能明显提高镀膜过程中钛料蒸发率,使成膜速率增加,在相同镀膜时间内TiN膜层加厚。 相似文献
213.
研究在脉冲氩弧焊条件下铝基复合材料SiCp/2124Al的可焊性。通过正确选择填充材料和在焊接过程中加入微量脉冲,大大减弱了增强体SiC颗粒与基体Al之间的界面反应。拉伸实验和显微硬度测试表明,接头质量良好,与母材强度相比,接头的抗拉强度未见有大幅度下降;金相组织观察显示,焊缝组织致密、无夹杂和裂纹等缺陷。对接头进行X射线衍射相结构分析和拉伸断口扫描电镜观察等微观分析,并从热力学角度探讨焊接过程中抑制SiC/Al界面反应发生的机理,提出了在氩弧焊条件下获得高质量SiCp/Al焊接接头应采取的措施。 相似文献
214.
215.
216.
一种新的脉冲星累积脉冲轮廓时间延迟测量算法 总被引:1,自引:0,他引:1
为提高X射线脉冲星导航系统中累积脉冲轮廓的时间延迟测量精度,分析了X射线脉冲星累积脉冲轮廓的特点和现有时延测量算法的缺陷,提出了一种粗略估计和精确测最相结合的时间延迟测量算法.该算法首先利用三阶互小波累积量进行粗略估计,可抑制尺度伸缩和噪声的影响;然后通过抛物面内插法精确测量时间延迟,避免了小步长的迭代运算,可大幅度降低算法的运算量.利用美国罗希(Rossi)X射线时变探测卫星的实测脉冲星数据进行实验,结果表明:该算法可屏蔽由多普勒效应和相位间隔长度的不同引起的尺度伸缩,能够抑制噪声,测量误差小于现有算法;当相位间隔为0.9°时,该算法的测量精度达到最高;该算法运算量小,不足现有算法的10%,适用于X射线脉冲星导航系统. 相似文献
217.
采用XPS方法研究了卡托辛对复合固体推进剂氧化剂AP热分解过程的作用机理。结果表明,热氧化后Fe原子的结合能向高位移动,再根据Fe2p3/2谱强度的变化,说明卡托辛在AP热分解过程中是逐渐氧化过程,Fe—C共轭键逐渐断裂;Cl原子的结合能向低位移动,且在200 eV左右出现低结合能的峰,同时其强度逐渐增大,Cl原子在200 eV处形成的低结合能态的可能途径是卡托辛的分解产物环戊二烯离子与HClO4的分解产物HCl发生反应,加速了HClO4的分解速度;卡托辛的二茂铁基夹心结构破坏后生成的Fe2O3具有较高的反应活性,亦加速AP离解产物HClO4的分解速度。 相似文献
218.
We compare CLOUDY predictions for the equilibrium ionization in the interstellar cloud surrounding the solar system with pick-up ion data. The incident radiation field includes contributions from hot stars, the emission from the conductive cloud boundary and the diffuse FUV back-ground. To within the observational uncertainties, CLOUDY predictions for the ratios n(He)/n(O), n(N)/n(O), n(Ne)/n(O), and n(He)/n(Ne) are consistent with pick-up ion data, provided that O and N are filtered by 50% in the heliopause region and the outer heliosphere as predicted by others. Thus, the steady-state ionization model and assumed radiation field appear approximately valid. However, the youth and low intervening column density towards the Vela pulsar leave open the possibility that the parent supernova explosion 10,500 years ago, and 200 pc distant, may also have affected LISM ionization, although the mechanism is uncertain. Support for this last possibility is provided by the apparent signature of the Vela explosion in the terrestrial geological record.Abbreviations ISM
Interstellar Medium
- FUV
Far Ultraviolet
- EUV
Extreme Ultraviolet
- SNR
SN remnant
- SXRB
SXR Background
- LISM
Local Interstellar Matter 相似文献
219.
John O. Goldsten Edgar A. Rhodes William V. Boynton William C. Feldman David J. Lawrence Jacob I. Trombka David M. Smith Larry G. Evans Jack White Norman W. Madden Peter C. Berg Graham A. Murphy Reid S. Gurnee Kim Strohbehn Bruce D. Williams Edward D. Schaefer Christopher A. Monaco Christopher P. Cork J. Del Eckels Wayne O. Miller Morgan T. Burks Lisle B. Hagler Steve J. DeTeresa Monika C. Witte 《Space Science Reviews》2007,131(1-4):339-391
A Gamma-Ray and Neutron Spectrometer (GRNS) instrument has been developed as part of the science payload for NASA’s Discovery
Program mission to the planet Mercury. Mercury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) launched
successfully in 2004 and will journey more than six years before entering Mercury orbit to begin a one-year investigation.
The GRNS instrument forms part of the geochemistry investigation and will yield maps of the elemental composition of the planet
surface. Major elements include H, O, Na, Mg, Si, Ca, Ti, Fe, K, and Th. The Gamma-Ray Spectrometer (GRS) portion detects
gamma-ray emissions in the 0.1- to 10-MeV energy range and achieves an energy resolution of 3.5 keV full-width at half-maximum
for 60Co (1332 keV). It is the first interplanetary use of a mechanically cooled Ge detector. Special construction techniques provide
the necessary thermal isolation to maintain the sensor’s encapsulated detector at cryogenic temperatures (90 K) despite the
intense thermal environment. Given the mission constraints, the GRS sensor is necessarily body-mounted to the spacecraft,
but the outer housing is equipped with an anticoincidence shield to reduce the background from charged particles. The Neutron
Spectrometer (NS) sensor consists of a sandwich of three scintillation detectors working in concert to measure the flux of
ejected neutrons in three energy ranges from thermal to ∼7 MeV. The NS is particularly sensitive to H content and will help
resolve the composition of Mercury’s polar deposits. This paper provides an overview of the Gamma-Ray and Neutron Spectrometer
and describes its science and measurement objectives, the design and operation of the instrument, the ground calibration effort,
and a look at some early in-flight data. 相似文献
220.
Scott D. Barthelmy Louis M. Barbier Jay R. Cummings Ed E. Fenimore Neil Gehrels Derek Hullinger Hans A. Krimm Craig B. Markwardt David M. Palmer Ann Parsons Goro Sato Masaya Suzuki Tadayuki Takahashi Makota Tashiro Jack Tueller 《Space Science Reviews》2005,120(3-4):143-164
he burst alert telescope (BAT) is one of three instruments on the
Swift MIDEX spacecraft to study gamma-ray bursts (GRBs). The BAT first detects the GRB and localizes the burst direction to an
accuracy of 1–4 arcmin within 20 s after the start of the event. The GRB trigger initiates an autonomous spacecraft slew to
point the two narrow field-of-view (FOV) instruments at the burst location within 20–70 s so to make follow-up X-ray and optical
observations. The BAT is a wide-FOV, coded-aperture instrument with a CdZnTe detector plane. The detector plane is composed
of 32,768 pieces of CdZnTe (4×4×2 mm), and the coded-aperture mask is composed of ∼52,000 pieces of lead (5×5×1 mm) with a
1-m separation between mask and detector plane. The BAT operates over the 15–150 keV energy range with ∼7 keV resolution,
a sensitivity of ∼10−8 erg s−1 cm−2, and a 1.4 sr (half-coded) FOV. We expect to detect > 100 GRBs/year for a 2-year mission. The BAT also performs an all-sky
hard X-ray survey with a sensitivity of ∼2 m Crab (systematic limit) and it serves as a hard X-ray transient monitor. 相似文献