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151.
用通用大气辐射传输软件CART模拟了POM02太阳辐射计的1020nm、1627nm和2200nm等3个近红外通道的大气透过率特性。结果表明,前两通道处于大气非吸收波段,其透过率很好的遵从Beer-Lambert定律,而2200nm通道则有较强的吸收,吸收光学厚度随大气质量的变化服从指数分布,与Beer-Lambert定律有一定的偏差,其定标需采用改进的Langley法。通过选取好天的5个定标实例证明,采用改进的Langley法定标2200nm通道,可提高其透过率测量精度约3.8%。 相似文献
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Rosalba Perna Charles R. Keeton 《Monthly notices of the Royal Astronomical Society》2009,397(2):1084-1092
In strong gravitational lensing, the multiple images we see correspond to light rays that leave the source in slightly different directions. If the source emission is anisotropic, the images may differ from conventional lensing predictions (which assume isotropy). To identify scales on which source anisotropy may be important, we study the angle δ between the light rays emerging from the source, for different lensing configurations. If the lens has a power-law profile M ∝ R γ , the angle δ initially increases with lens redshift and then either diverges (for a steep profile γ < 1 ), remains constant (for an isothermal profile γ= 1 ), or vanishes (for a shallow profile γ > 1 ) as z l → z s . The scaling with lens mass is roughly δ∝ M 1/(2−γ) . The results for an Navarro–Frenk–White (NFW) profile are qualitatively similar to those for a shallow power law, with δ peaking at about half the redshift of the source (not half the distance). In practice, beaming could modify the statistics of beamed sources lensed by massive clusters: for an opening angle θjet , there is a probability as high as P ∼ 0.02–0.07(θjet /0.5°)−1 that one of the lensed images may be missed (for 2 ≲ z s ≲ 6 ). Differential absorption within active galactic nuclei (AGNs) could modify the flux ratios of AGNs lensed by clusters; a sample of AGNs lensed by clusters could provide further constraints on the sizes of absorbing regions. Source anisotropy is not likely to be a significant effect in galaxy-scale strong lensing. 相似文献
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A number of problems associated with detailed investigation of subsurface geological structure below the bottoms of freshwater reservoirs (rivers, ponds, and lakes) arise during the study of the upper portions of geological sections. The present study is aimed at marginal estimation of the penetrating depth of ground radar investigations in freshwater reservoirs (based on bottom reflections), taking into account the complex nature of conductivity and its dependence upon the frequency under ideal conditions with no noise. The same method can be applied for estimating any given dynamic recording range. 相似文献
156.
微波消解等离子体发射光谱和石墨炉原子吸收光谱法联合测定土壤中多元素 总被引:6,自引:2,他引:4
采用密闭式微波消解系统处理土壤样品,电感耦合等离子体发射光谱法或石墨炉原子吸收光谱法测定土壤样品中铜、砷、铅、锌、钴、铬、锰、镍、钒9个元素。分别从消解液的选择、用酸量及样品消解量等方面进行消解条件的优化,确定了一个最适合土壤消解的前处理体系。各元素的检出限为0.16~2.52μg/g,回收率为95.2%~106.6%,精密度为2.03%~9.79%(n=7)。方法简单快速,效率高,劳动强度低,是进行土壤中多元素测定的高效方法。 相似文献
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159.
J. Liske A. Grazian E. Vanzella M. Dessauges M. Viel L. Pasquini M. Haehnelt S. Cristiani F. Pepe G. Avila P. Bonifacio F. Bouchy H. Dekker B. Delabre S. D'Odorico V. D'Odorico S. Levshakov C. Lovis M. Mayor P. Molaro L. Moscardini M. T. Murphy D. Queloz P. Shaver S. Udry T. Wiklind S. Zucker 《Monthly notices of the Royal Astronomical Society》2008,386(3):1192-1218
The redshifts of all cosmologically distant sources are expected to experience a small, systematic drift as a function of time due to the evolution of the Universe's expansion rate. A measurement of this effect would represent a direct and entirely model-independent determination of the expansion history of the Universe over a redshift range that is inaccessible to other methods. Here we investigate the impact of the next generation of Extremely Large Telescopes on the feasibility of detecting and characterizing the cosmological redshift drift. We consider the Lyα forest in the redshift range 2 < z < 5 and other absorption lines in the spectra of high-redshift QSOs as the most suitable targets for a redshift drift experiment. Assuming photon-noise-limited observations and using extensive Monte Carlo simulations we determine the accuracy to which the redshift drift can be measured from the Lyα forest as a function of signal-to-noise ratio and redshift. Based on this relation and using the brightness and redshift distributions of known QSOs we find that a 42-m telescope is capable of unambiguously detecting the redshift drift over a period of ∼20 yr using 4000 h of observing time. Such an experiment would provide independent evidence for the existence of dark energy without assuming spatial flatness, using any other cosmological constraints or making any other astrophysical assumption. 相似文献
160.
T. V. Zinov’eva 《Astronomy Letters》2008,34(2):118-132
We consider the effects of the grain size, shape, structure, and chemical composition as well as the angle between the grain rotation axis and the incident ray on the full widths at half maximum (FWHM) of the polarization bands in the two deepest infrared absorption bands observed in the spectra of protostars, the water-ice band centered at 3.1 μm and the silicate band centered at 9.7 μm, using a core—mantle confocal spheroid model with various axial ratios a/b and relative volumes of the core material. We have found that the observed polarization bands with FWHMp < 0.3 μm in the water-ice absorption band can be explained only by oblate and prolate particles with r v ≤ 0.35 μm and the polarization bands with FWHMp ≈ 0.3 μm can be explained only by particles with r v ≈ 0.35 μm. Broad silicate absorption bands (FWHM ≈ 3 μm) with broad polarization bands (FWHMp ≈ 2.7 μm) can be explained by particles with r v ≈ 0.35 μm. Narrow silicate absorption bands (FWHM ≤ 3 μm) with any FWHM of the polarization bands can be explained by a mixture of particles of two types of olivine. Narrow polarization bands (FWHMp ≈ 2 μm) with broad absorption bands can be explained only by very small particles, r v ≤ 0.1 μm. We have found the relationships between the effective polarization and extinction cross sections and estimated the ranges of observed polarizabilities that can be explained by particles of given shape and orientation in each of the bands independently. Independent studies of the observational data for each of the bands are shown to give a wider choice of particle model parameters. 相似文献