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21.
ZnO作为一种典型的透明导电氧化物(Transparent conductive oxide,TCO)材料,具有同氧化铟锡(Indium tin oxide,ITO)相比拟的光电性能,其原料丰富、绿色环保、易于制备、生成成本低等优点使ZnO成为最有希望替代ITO的材料。本文以玻璃为衬底,利用量子点种子层作为缓冲层,采用传统水热方法制备了低成本ZnO透明导电薄膜,采用特殊的紫外光辐照工艺对薄膜进行后处理,探索薄膜生长参数和紫外光辐照处理工艺对其透光率和导电性的影响。结果表明,紫外辐照处理不影响薄膜的透光性能,而使材料的方块电阻降低3个数量级,数值从没处理时的1.5×105 Ω/□降低到 150 Ω/□,极大地提高了薄膜的电导率,为ZnO薄膜材料电导率的提高提供了一个简单高效的途径。 相似文献
22.
Profiles of the visible Fe X (6374 Å) coronal emission line as a function of height above the limb were obtained out to 1.16 solar radii in a coronal hole using the NSO/Sacramento Peak Observatory Coronagraph, Universal Spectrograph and a CCD camera. These are the first coronal line profiles obtained as a function of height in a coronal hole from the ground. Analysis of the line widths suggests a large component of nonthermal broadening which increases with height ranging from 40 to 60 km/s, depending upon the assumed temperature or thermal component of the profile. 相似文献
23.
J. L. Kohl S. Fineschi R. Esser A. Ciaravella S. R. Cranmer L. D. Gardner R. Suleiman G. Noci A. Modigliani 《Space Science Reviews》1999,87(1-2):233-236
Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights ? (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for ? = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at ? = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at ? = 1.34, but are significantly larger at ? = 1.5 and much larger for ? > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least ? = 2.0, but never reach the values of O VI. 相似文献
24.
空间环境下的有机热控涂层 总被引:6,自引:3,他引:6
本文综述了国外在空间有机热控涂层领域中的研究工作和试验,着重分析了空间极端环境中紫外光辐照和原子氧侵蚀这两大因素对有机热控涂层的影响。 相似文献
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紫外月球敏感器的几个关键问题 总被引:5,自引:1,他引:5
论述了紫外月球敏感器的由来和功能,从基本原理、消杂光设计、能量 与孔径选择、月像处理和姿态提取算法、超大视场消杂光等关键问题的解决进行 了阐述,并得出结论。 相似文献
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Using empirical velocity distributions derived from UVCS and SUMER ultraviolet spectroscopy, we construct theoretical models
of anisotropic ion temperatures in the polar solar corona. The primary energy deposition mechanism we investigate is the dissipation
of high frequency (10-10000 Hz) ion-cyclotron resonant Alfvén waves which can heat and accelerate ions differently depending
on their charge and mass. We find that it is possible to explain the observed high perpendicular temperatures and strong anisotropies
with relatively small amplitudes for the resonant waves. There is suggestive evidence for steepening of the Alfvén wave spectrum
between the coronal base and the largest heights observed spectroscopically. Because the ion-cyclotron wave dissipation is
rapid, even for minor ions like O5+, the observed extended heating seems to demand a constantly replenished population of waves over several solar radii. This
indicates that the waves are generated gradually throughout the wind rather than propagated up from the base of the corona.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
30.
Beverley J. Wills Zhaohui Shang 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2004,34(12):2584-2587
The evolution of luminous QSOs is linked to the evolution of massive galaxies. We know this because the relic black-holes found locally have masses dependent on the properties of the host galaxy’s bulge. An important way to explore this evolution would be to measure dependences of black-hole masses and Eddington accretion ratios over a range of redshifts, i.e., with cosmological age. For low redshift QSOs (and their lower luminosity Seyfert galaxy counterparts) it has been possible to infer black-hole masses from the luminosities and velocity dispersions of their host-galaxy bulges. These masses agree with those virial black-hole masses calculated from the Doppler widths of the broad Hβ emission lines. The latter method can then be extended to more distant and luminous QSOs, up to redshifts of 0.6 with ground-based optical observations. We discuss ways to extend these explorations to higher redshifts – up to 3 using the widths of QSOs’ broad UV emission lines, and in principle, and to redshifts near 4 from ground-based infrared observations of rest-frame Hβ at 2.5 μm. We discuss the possibility of investigating the accretion history of the higher redshift QSOs using measures of Eddington accretion ratio – the soft X-ray spectral index and the eigenvectors of Principal Components Analyses of QSOs’ UV emission-line spectra. 相似文献