黑河下游绿洲近地层湍流输送特征研究     

张艳武  黄静  吴统文 《气象学报》2009,67(3):433-441

分析2003年9月5-27日在黑河下游额济纳绿洲取得的近地面层湍流观测资料,讨论无量纲湍流方差与稳定度参数Z/L的关系.无量纲风速分量σu/u*、σv/u*和σw/u*在不稳定层结与稳定度Z/L满足1/3次方时,符合Monin-Obkuhov相似理论.在近中性时,σu/u*、σw/u*值比平坦下垫面的略小些,σv/u*值比平坦下垫面的略大.无量纲温度脉动方差和湿度脉动方差在对流状态下与Z/L满足-1/3次方,在稳定和不稳定层结下,随|Z/L|减小而增大.地面热量以感热输送为主,感热通量峰值约为250 W/m2,潜热通量的峰值为170 W/m2;夜间潜热通量较小,感热通量则出现负值.动量通量日间平均在0.2-0.3 N/m2,峰值为0.31 N/m2.黑河下游绿洲柽柳林动力学粗糙度比HEIFE戈壁及其他绿洲下垫面的大,中性时z0m=0.47551 m.中性状态下动量整体输送系数CD=22.2×10-3,不稳定层结时平均值CD=10.3×10-3,稳定层结时平均值CD=7.2 × 10-3.热量整体输送系数CH,中性状态下CH=3.2 × 10-3,不稳定层结时平均值为CH=3.3×10-3,稳定层结时平均值为CH=2.7×10-3.  相似文献   

陇中黄土高原半干旱区总体输送系数的特征   总被引：5，自引：2，他引：3       下载免费PDF全文

杨兴国-  张强  杨启国  王润元  刘宏谊  马鹏里 《高原气象》2010,29(1):44-50

利用在陇中黄土高原半干旱区2003年10月—2005年7月获得的近地层梯度观测资料,采用空气动力学法,计算了动量和感热总体输送系数。结果表明,陇中黄土高原半干旱区动量和感热总体输送系数均存在明显的日变化特征,夏季中午左右分别达到5.6×10-3和6.7×10-3。受下垫面植被的影响,在一年中呈现出双峰型特征,第一峰值出现在春小麦拔节—黄熟期,次高值出现在10月初。动量和感热总体输送系数平均值分别为2.9×10-3和3.1×10-3。当大气处于不稳定状态时,总体输送系数随着风速的增大而减小;相反当大气处于稳定状态时,随着风速的增大而增大。陇中黄土高原半干旱区的总体输送系数高于戈壁、平原草地和海洋下垫面的值,但低于青藏高原草地和城市下垫面的值。  相似文献   

Methane absorption coefficients for the jovian planets from laboratory, Huygens, and HST data     

Erich Karkoschka  Martin G. Tomasko 《Icarus》2010,205(2):674-694

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Ground-based measurements of the methane distribution on Titan     

Paulo F. Penteado  Caitlin A. Griffith 《Icarus》2010,206(1):345-7996

Using spectra taken with NIRSPEC (Near Infrared Spectrometer) and adaptive optics on the Keck II telescope, we resolved the latitudinal variation of the 3ν₂ band of CH₃D at 1.56 μm. As CH₃D is less abundant than CH₄ by a factor of 50±10×10^-5, these CH₃D lines do not saturate in Titan’s atmosphere, and are well characterized by laboratory measurements. Thus they do not suffer from the large uncertainties of the CH₄ lines that are weak enough to be unsaturated in Titan. Our measurements of the methane abundance are confined to the latitude range of 32°S-18°N and longitudes sampled by a 0.04″ slit centered at ∼195°W. The methane abundance below 10 km is constant to within 20% in the tropical atmosphere sampled by our observations, consistent with the low surface insolation and lack of surface methane [Griffith, C.A., McKay, C.P., Ferri, F., 2008. Astrophys. J. 687, L41-L44].  相似文献   

Ultraviolet dust aerosol properties as observed by MARCI     

Michael J. Wolff  R. Todd Clancy  Michael C. Malin 《Icarus》2010,208(1):143-2499

Observations by the Mars Color Imager (MARCI) on board the Mars Reconnaissance Orbiter (MRO) in two ultraviolet (UV, Bands 6 and 7; 258 nm, and 320 nm, respectively) and one visible (Band 1, 436 nm) channels of the 2007 planet encircling dust storm are combined with those made by the two Mars Exploration Rovers (MERs) to better characterize the single scattering albedo (ω₀) of martian dust aerosols. Exploiting the low contrast of the surface in the UV (and blue) as well as the reduced importance of surface reflectance under very dusty conditions, we utilize the sampling of photometric angles by the MARCI cross-track geometry to synthesize an analog of the classical Emergence Phase Function (EPF). This so-called “pseudo-EPF”, used in conjunction with the “ground-truth” measurements provided by the MERs, is able to effectively isolate the effects of the dust ω₀. The motivation for this approach is the elimination of a significant portion of the type of uncertainty involved in many previous radiative transfer analyses. Furthermore, we produce a self-consistent set of complex refractive indices (m=n+ik) through our use of an explicit microphysical representation of the aerosol scattering properties. Because of uncertainty in the exact size of the dust particles during the epoch of the observations, we consider two effective particle radii (r_eff) to cover the range anticipated from the literature: 1.6 and 1.8 μm. The resulting set of model-data comparisons, ω₀, and m are presented along with an assessment of potential sources of error and uncertainty. Analysis of the Band 1 results is limited to ω₀ as a “proof-of-concept” for our approach through a comparison to contemporaneous CRISM EPF results at 440 nm. The derived ω₀ are: assuming , and 0.765, for Bands 6, 7, and 1, respectively; for , for the same band order. For either r_eff case, the total estimated error is 0.022, 0.019, and 0.010, again for Bands 6, 7, and 1. We briefly discuss our retrievals, including the asymmetry parameter (g) associated with our model phase functions, within the context of previous efforts, with an emphasis on the improved precision of our results compared to those in the literature. We also suggest several applications of our results, including an extension of the dust climatological record using MARCI Band 7 pseudo-EPFs outside of 2007 global dust event. Initial work on this particular application using a sample of 135 pseudo-EPFs near the MERs suggests that optical depth retrievals with a precision in the range 0.2-0.4 may be possible under moderate loading conditions (i.e., τ < 1.5).  相似文献   

UVIS observations of the FUV OI and CO 4P Venus dayglow during the Cassini flyby     

B. Hubert  J.C. Gérard  V.I. Shematovich  A.I. Stewart 《Icarus》2010,207(2):549-557

We analyze FUV spatially-resolved dayglow spectra obtained at 0.37 nm resolution by the UVIS instrument during the Cassini flyby of Venus. We use a least-squares fit method to determine the brightness of the OI emissions at 130.4 and OI 135.6 nm, and of the bands of the CO fourth positive system which are dominated by fluorescence scattering. We compare the brightness observed along the UVIS foot track of the two OI multiplets with that deduced from a model of the excitation of these emissions by photoelectron impact on O atoms and resonance scattering of the solar 130.4 nm emission. The large optical thickness 130.4 nm emission is accounted for using a radiative transfer model. The airglow intensities are calculated along the foot track and found to agree with the observed 130.4 nm brightness within ∼10%. The modeled OI 135.6 nm brightness is also well reproduced by the model. The oxygen density profile of the VTS3 model is found to be consistent with the observations. We find that self-absorption of the (0, v″) bands of the fourth positive emission of CO is important and we derive a CO vertical column of about 6.4 × 10¹⁵ cm⁻² in close agreement with the value provided by the VTS3 empirical atmospheric model.  相似文献   

Constraints on Mercury’s surface composition from MESSENGER and ground-based spectroscopy     

J. Warell  A. Sprague  D.A. Rothery  J. Helbert 《Icarus》2010,209(1):138-163

The composition and chemistry of Mercury’s regolith has been calculated from MESSENGER MASCS 0.3-1.3 μm spectra from the first flyby, using an implementation of Hapke’s radiative transfer-based photometric model for light scattering in semi-transparent porous media, and a linear spectral mixing algorithm. We combine this investigation with linear spectral fitting results from mid-infrared spectra and compare derived oxide abundances with mercurian formation models and lunar samples. Hapke modeling results indicate a regolith that is optically dominated by finely comminuted particles with average area weighted grain size near 20 μm. Mercury shows lunar-style space weathering, with maturation-produced microphase iron present at ∼0.065 wt.% abundance, with only small variations between mature and immature sites, the amount of which is unable to explain Mercury’s low brightness relative to the Moon. The average modal mineralogies for the flyby 1 spectra derived from Hapke modeling are 35-70% Na-rich plagioclase or orthoclase, up to 30% Mg-rich clinopyroxene, <5% Mg-rich orthopyroxene, minute olivine, ∼20-45% low-Fe, low-Ti agglutinitic glass, and <10% of one or more lunar-like opaque minerals. Mercurian average oxide abundances derived from Hapke models and mid-infrared linear fitting include 40-50 wt.% SiO₂, 10-35 wt.% Al₂O₃, 1-8 wt.% FeO, and <25 wt.% TiO₂; the inferred rock type is basalt. Lunar-like opaques or glasses with high Fe and/or Ti abundances cannot on their own, or in combination, explain Mercury’s low brightness. The linear mixing results indicate the presence of clinopyroxenes that contain up to 21 wt.% MnO and the presence of a Mn-rich hedenbergite. Mn in M1 crystalline lattice sites of hedenbergite suppresses the strong 1 and 2 μm crystal field absorption bands and may thus act as a strong darkening agent on Mercury. Also, one or more of thermally darkened silicates, Fe-poor opaques and matured glasses, or Mercury-unique Ostwald-ripened microphase iron nickel may lower the albedo. A major part of the total microphase iron present in Mercury’s regolith is likely derived from FeO that is not intrinsic to the crust but has been subsequently delivered by exogenic sources.  相似文献   

农田排水沟渠的环境效应与生态功能综述   总被引：9，自引：0，他引：9       下载免费PDF全文

陆海明  孙金华  邹鹰  朱乾德  丰华丽 《水科学进展》2010,21(5):719-725

农田排水沟渠作为农业景观中重要的景观单元,能够调节农田生态系统水分平衡,改变流域水文情势。农田养分可以随排水过程迅速流失,也可以通过沉淀与吸附机制被农田沟渠所截留或者通过植物吸收后收割与反硝化去除等机制脱离农田生态系统。作为农田生态系统边缘的交错带,农田排水沟渠较高的植物多样性可以提供动物栖息地和避难场所,增加农田生态系统生物多样性。清淤、收割和控制排水等管理措施对于农田排水沟渠的环境效应和生态服务功能有着不同的影响。今后应加强从多个学科研究农田排水沟渠的环境效应和生态功能,探索生态排水沟渠的构建和管理技术,实现农田排水沟渠水利功能和生态功能的"双赢"。  相似文献   

临沂市城乡建设用地增减挂钩试点工作调查与思考     

李德强  李涛  王步远 《山东地质》2010,(7):49-51,55

2006年以来,临沂市先后被列为全国第一、二批城乡建设用地增减挂钩试点城市。试点工作中周密部署、科学规划、注重创新,走出了一条符合临沂实际的增减挂钩新路子,较好地实现了农民得实惠、企业得市场、发展得空间、政府得人心。但也存在一些值得重视的问题,需要作进一步的思考与探索,以便积极稳妥地推动城乡建设用地增减挂钩试点工作。  相似文献   

蒙阴县城乡建设用地增减挂钩工作现状与思考     

张淑森 《山东地质》2010,(11):74-76

蒙阴县充分利用城乡建设用地增减挂钩政策,加大农村居民点的整合搬迁复垦力度,积极推进新农村建设,改变了村容村貌,缓解了发展与用地的矛盾,加快了城乡统筹的步伐。  相似文献