渤海GNSS-R机载测风试验及其反演结果     

周兆明  符养 《武汉大学学报(信息科学版)》2008,33(3):241-244

对渤海GNSS-R机载试验进行了海面风场反演.结果表明,风速精度优于1 m/s,风向精度优于20°.  相似文献   

全站仪断面测量方法   总被引：1，自引：0，他引：1  

高斌  鹿罡  赵宝军 《测绘与空间地理信息》2008,31(4)

从野外断面测量的角度出发,主要讨论全站仪在断面测量中的野外观测方法、数据处理思路以及相应的软件研制.  相似文献   

InSAR复数影像配准方法探讨   总被引：1，自引：0，他引：1  

焦明连  蒋廷臣 《测绘与空间地理信息》2008,31(6)

复数影像配准是卫星合成孔径雷达干涉数据处理中的重要步骤之一,本文对目前影像配准最常用的方法进行了研究分析,提出了基于幅度影像的配准方案,并证明该方案配准精度高,适应能力强,运算效率高.  相似文献   

大别山黄石-六安反射地震剖面新的地质解释   总被引：3，自引：0，他引：3  

徐树桐  袁学诚  吴维平  刘贻灿 《地质通报》2008,27(1):19-26

在大别山黄石至六安反射地震剖面上有很多近水平的反射体,表明大别山中心部位的中、下地壳内也有近水平的分层性。反映有流变性和动力学方面的差异,与大型薄皮构造理论对岩石圈性质的认识一致,因而在其运动过程中应服从薄皮构造的运动规律。结合以往对大别山区划分的岩石一构造组合,在前人对此反射地震剖面所作的地质解释的基础上,对反射地震剖面作了较为详细的地质解释,并建立了大别山造山带在此剖面上的两维几何结构。剖面南部为造山过程中形成的背斜构造。地表15km深度内为由碰撞混杂岩组成的扬子与中一朝大陆之间的主滑脱带。剖面中部为造山期后的侵入体。剖面北部为主滑脱带的根带（通常认为的缝合带）,根带被中生代形成的晓天磨子潭断裂带切割。剖面最北端为变质复理石中略晚于主滑脱带的反向冲断带。推溺l下地壳的断开距离在扬子大陆俯冲时（三叠纪前）规模较大,然后逐渐缩小,直至保留到今天的规模。  相似文献   

应用探地雷达探测活动断层   总被引：1，自引：0，他引：1  

薛建  贾建秀  黄航  易兵  张良怀  张羽 《吉林大学学报(地球科学版)》2008,38(2):347-350

在浅覆盖区采用探地雷达探测地震活动断层。通过实验确定出最佳的采集参数和数据处理流程,在雷达剖面上,能够清晰地显示出断层上部的形态特征、上断点埋深和岩土分层。结合钻孔资料,利用雷达剖面上对第四系覆盖的分层结果和上断点所在的层位可以分析和评价断层的活动性。  相似文献   

青藏高原锡铁山—格尔木—亚东剖面地温分布特征     

翟利剑  包汇慧  毕思文 《吉林大学学报(地球科学版)》2008,38(5)

以青藏高原锡铁山—格尔木—亚东剖面作为研究对象,测定不同深度土层的温度。结果表明,除北部柴达木地块地温高出其它地块外,该剖面总体上呈现出青藏高原各地块地温状况南高北低的现象:以拉萨—冈底斯地块的地温为最高,其次为喜马拉雅地块,北部的羌塘地块、可可西里-巴颜喀拉地块、昆仑地块的地温依次降低。测量结果较好地对应于各地块及断裂带的划分,断裂带温度明显高出相邻低温地块温度,并且以狮泉河—雅鲁藏布江断裂带为最高。该试验方法较好地反映了青藏高原热活动状况,为青藏高原热动力学研究提供了依据。  相似文献   

磷处理粉煤灰可作农业土壤磷源   总被引：2，自引：0，他引：2  

申俊峰  M.A.Powell  D.B.Hayden 《地学前缘》2008,15(6):112

粉煤灰(简称CCP或ash)具有改良土壤,增加植物产量的功能。此外,由于它特殊的多孔结构,也可用作吸纳并承载植物养分的载体。用NaH2PO4配制成含磷0.10mol/L浓度的溶液,对采自加拿大西安大略省Sarnia地区Lambton电厂的底灰(bottomash)进行振荡浸渍处理。结果表明,振荡浸渍66h后的粉煤灰中磷含量可达784×10-6。以磷处理粉煤灰、未进行磷处理的粉煤灰和石英砂按比例混合,作为基本生长介质进行玉米种植实验,其中实验配方设计为生长介质中含磷量分别为标准含磷浓度(50×10-6)的10%、25%、50%、75%和100%。生长26、34和46d后分别与不含磷的空白配方、施加含氮-磷-钾为0-20-0标准磷肥并控制磷含量为标准浓度(50×10-6)配方进行生物产量对比。生长实验结果表明,以磷处理粉煤灰供磷的生长介质,当含磷量为标准浓度的25%至100%时,其植物生长量就比添加标准浓度磷肥的配方好。种植46d后的生物生长量统计结果显示,含磷分别为标准浓度50%、75%和100%的实验介质中,玉米杆的鲜重较施标准磷肥介质中玉米分别增长39.46%、42.73%和46.13%;玉米杆干重依次增加29.71%、13.39%和28.87%;根鲜重平均增加16.62%;根干重平均增加14.03%。上述实验结果启示,粉煤灰可以很好地吸纳承载磷养分,并持续供给植物吸收生长,如果采用吸纳磷(或其他养分)的粉煤灰改良砂质土壤将有重要意义。  相似文献   

Carbonyl products of the gas phase reaction of ozone with 1,1-disubstituted alkenes     

Eric Grosjean  Daniel Grosjean 《Journal of Atmospheric Chemistry》1996,24(2):141-156

Carbonyl products have been identified and their formation yields measured in experiments involving the gas phase reaction of ozone with 1,1-disubstituted alkenes at ambient T and p=1 atm. of air. Sufficient cyclohexane was added to scavenge the hydroxyl radical in order to minimize OH-alkene and OH-carbonyl reactions. Formation yields (carbonyl formed/ozone reacted) of primary carbonyls were close to the value of 1.0 that is consistent with the mechanism: O₃+R₁R₂C=CH₂ (HCHO+R₁R₂COO)+(1–)(R₁COR₂+H₂COO) where formaldehyde and the ketone R₁ COR₂ are the primary carbonyls and R₁R₂COO and H₂COO are the corresponding biradicals. Measured values of were 0.58–0.82 and indicate modest preferential formation of formaldehyde and the disubstituted biradical as compared to the ketone and the biradical H₂COO. Carbonyls other than the primary carbonyls were identified. Their formation is discussed in terms of subsequent reactions of the disubstituted biradicals R₁R₂COO. Similarities and differences between disubstituted and monosubstituted biradicals are outlined.  相似文献   

The origin of accretionary lapilli   总被引：1，自引：0，他引：1  

J. S. Gilbert  S. J. Lane 《Bulletin of Volcanology》1994,56(5):398-411

Experimental investigations in a recirculating wind tunnel of the mechanisms of formation of accretionary lapilli have demonstrated that growth is controlled by collision of liquid-coated particles, due to differences in fall velocities, and binding as a result of surface tension forces and secondary mineral growth. The liquids present on particle surfaces in eruption plumes are acid solutions stable at 100% relative humidity, from which secondary minerals, e.g. calcium sulphate and sodium chloride, precipitate prior to impact of accretionary lapilli with the ground. Concentric grain-size zones within accretionary lapilli build up due to differences in the supply of particular particle sizes during aggregate growth. Accretionary lapilli do not evolve by scavenging of particles by liquid drops followed by evaporation — a process which, in wind tunnel experiments, generates horizontally layered hemispherical aggregates. Size analysis of particles in the wind tunnel air stream and particles adhering to growing aggregates demonstrate that the aggregation coefficient is highly grain-size dependent. Theoretical simulation of accretionary lapilli growth in eruption plumes predicts maximum sizes in the range 0.7–20 mm for ash cloud thicknesses of 0.5–10 km respectively.  相似文献   

Structure and energy transfer of unstable hot star winds     

A. Feldmeier 《Astrophysics and Space Science》1994,221(1-2):393-408

Due to the instability of the radiation line force, the winds of hot, luminous stars should show a pronounced time-dependence resulting from the nonlinear growth of initially small perturbations. Following the method of Owocki, Castor & Rybicki (1988), we describe the time-dependent wind structure obtained with an independently developed code. Under the central assumption ofisothermality, our results are in very good agreement with the ones by Owocki et al. We find that the response of the wind to periodic base perturbations remains largely periodic, at least up tor 2...3R _* , with no clear evidence of stochastic behaviour.In order to test the foregoing assumption of isothermality and to compute the X-ray emission from models of structured winds, we have also incorporated theenergy equation into our simulations. We encountered the numerical problem that all radiative cooling zones collapse because of the oscillatory thermal instability (cf. Langer et al. 1981). We present a method to hinder this collapse by changing the cooling function at low temperatures. The resulting wind showsresolved cooling zones; but, for a supergiant wind relatively close to the star (r 10R _* ), the macroscopic wind structure is very similar to isothermal calculations. Most of the hot material is caused by shell-shell collisions.  相似文献