基于MODIS数据的湖北省油菜种植分布信息提取   总被引：1，自引：0，他引：1  

王凯  张佳华 《国土资源遥感》2015,(3)

MODIS归一化差值植被指数(MODIS-normalized difference vegetation index,MODIS-NDVI)时间序列产品能够连续反映植被的覆盖情况,是农作物遥感测量的重要数据源。为研究基于MODIS数据的油菜种植分布信息提取技术,选取湖北省为研究区,利用2008—2013年75个时相的MODIS-NDVI时序数据,结合农作物物候和地面调查样本等辅助资料,通过建立油菜种植面积提取模型,采用多次阈值比较方法提取了2009—2013年湖北省油菜种植分布信息,与统计数据比较,总体提取精度为85%左右。最后利用环境小卫星HJ-1A CCD数据进行精度验证,证明了MODIS-NDVI时序数据及本文方法在油菜种植面积提取中的可靠性,对掌握油菜种植面积和产量信息、加强农业生产管理、调整农业结构及辅助政府有关部门制定科学合理的农业政策具有重要意义。  相似文献   

基于扫描统计的甲型H1N1流感聚集性分析     

姚欣  夏天琦  翁敏 《测绘工程》2015,(10):56-58

扫描统计已被广泛应用于地域性疾病的聚集性检测,且可检测这种聚集的差异显著性。文中使用扫描统计的方法,通过对2009~2012年全国各省的甲型H1N1流感数据进行时空扫描以及逐年的空间扫描,生成高发病率地区和低发病率地区聚类,并通过叠置分析反映各个地区归入聚类的频次。利用专题地图和统计表分析甲型流感在2009~2012年中的爆发情况和趋势,并对结果进行客观的分析。  相似文献   

利用暗目标法从高分一号卫星16 m相机数据反演气溶胶光学厚度   总被引：5，自引：3，他引：2  

王中挺  辛金元  贾松林  厉青  陈良富  赵少华 《遥感学报》2015,19(3):530-538

针对高分一号卫星(GF-1)的16 m宽覆盖相机数据,探讨了暗目标法的应用。首先,利用地面观测的植被光谱数据,结合模拟计算,发现利用红蓝波段线性关系能更好地去除地表影响,而利用反演的气溶胶光学厚度AOD进行大气校正能很好地去除伪暗目标;然后,以天津地区和北京地区为试验区进行了反演试验。结果表明,利用本算法能较好地观测气溶胶分布,与地面观测结果均有较好的相关性(R0.8),但反演结果整体偏高,可能是云像元的影响。误差分析表明,整景图像采用统一的观测天顶角会带来较大误差,最大误差为0.3;绝对辐射定标精度在3%以下,反演精度能控制在10%,城市型气溶胶会对反演带来较大误差。  相似文献   

“天绘一号”卫星三线阵CCD影像自检校区域网平差     

张艳  王涛  冯伍法  元朝鹏  王淑香 《遥感学报》2015,19(2):219-227

遥感卫星在空间环境运转过程中,星敏感器的姿态角、成像相机的镜头和CCD等几何参数会发生不可预估的变化,从而对卫星影像的定位精度产生影响。因此,对卫星影像进行自检校区域网平差处理是实现卫星影像精确定位的一项关键技术。本文以"天绘一号"卫星为研究对象,首先分析了"天绘一号"卫星三线阵立体测绘相机的镜头和CCD几何形变,并提出了适用于"天绘一号"卫星三线阵CCD影像的自检校模型;然后建立"天绘一号"卫星三线阵CCD影像的自检校区域网平差模型,对外方位元素和自检校参数进行整体平差,消除存在于外方位元素观测值和自检校标定值中的系统误差,以提高卫星图像定位精度。最后利用嵩山实验场对"天绘一号"卫星三线阵CCD影像进行了自检校区域网平差处理,验证了自检校模型和自检校区域网平差模型的正确性和有效性,并分析研究了不同数目的控制点条件对自检校区域网平差的影响。实验结果证实采用自检校区域网平差技术可以有效地消除系统定位误差,显著提高定位精度。  相似文献   

利用空间实测数据进行板块构造分析     

田亮  刘武凤  姜鹏远  孙建军 《测绘科学》2015,(12):149-152

针对全球台站数量剧增、空间定位测量精度越发提高的情况,该文利用ITRF2008框架GPS、卫星激光测距、甚长基线干涉测量实测站速度信息,北美、中国以及欧洲连续运行卫星定位网络站速度信息进行基准统一,联合解算国际地球自转服务协议中14个主要大陆板块的欧拉矢量,对原有的板块运动参数进行精化;提出最小二乘海量台站选取方法。实验结果表明,该台站选取方法能够有效提高海量台站的筛选效率和可靠性;稳定台站的数量越多,分布越均匀,越能够体现板块运动的现势性。  相似文献   

地震波面波空间相干性规律研究     

朱园园  丁海平 《震灾防御技术》2021,16(3):467-475

In this paper, seismic records of Taiwan LSST array and SMART-1 array were selected to calculate the S-wave and surface wave coherence coefficients at different station distances. And then the coherence function model proposed by Loh was used to fit the calculation results. After comparison and analysis, we found that when the distance d < 50 m, the coherency coefficients of surface wave and S-waves are basically the same; when the distance d = 50 m , the coherency coefficients of surface wave is smaller than that of S-wave, and as the distance increases, the differences gradually increase. When the distance d > 500 m, the spatial coherency of the surface wave hardly exists, so no further consideration is needed. Finally, the surface wave coherency model parameters were given in this paper, which can be used as a reference for the synthetic ground motion field in the seismic analysis for long and large structures in large basins.  相似文献   

Observations of Comet 9P/Tempel 1 around the Deep Impact event by the OSIRIS cameras onboard Rosetta     

Horst Uwe Keller  Sonia Fornasier  Stubbe F. Hviid  Jörg Knollenberg  Miriam Rengel  Gabriele Cremonese  Detlef Koschny  Ekkehard Kührt  Holger Sierks  Cesare Barbieri  Hans Rickman  Michael F. A'Hearn  Maria-Antonella Barucci  Vania da Deppo  Björn J.R. Davidsson  Stefano Debei  Fritz Gliem  José J. Lopez Moreno  Giampiero Naletto  Angel Sanz Andrés 《Icarus》2007,187(1):87-103

The OSIRIS cameras on the Rosetta spacecraft observed Comet 9P/Tempel 1 from 5 days before to 10 days after it was hit by the Deep Impact projectile. The Narrow Angle Camera (NAC) monitored the cometary dust in 5 different filters. The Wide Angle Camera (WAC) observed through filters sensitive to emissions from OH, CN, Na, and OI together with the associated continuum. Before and after the impact the comet showed regular variations in intensity. The period of the brightness changes is consistent with the rotation period of Tempel 1. The overall brightness of Tempel 1 decreased by about 10% during the OSIRIS observations. The analysis of the impact ejecta shows that no new permanent coma structures were created by the impact. Most of the material moved with . Much of it left the comet in the form of icy grains which sublimated and fragmented within the first hour after the impact. The light curve of the comet after the impact and the amount of material leaving the comet ( of water ice and a presumably larger amount of dust) suggest that the impact ejecta were quickly accelerated by collisions with gas molecules. Therefore, the motion of the bulk of the ejecta cannot be described by ballistic trajectories, and the validity of determinations of the density and tensile strength of the nucleus of Tempel 1 with models using ballistic ejection of particles is uncertain.  相似文献   

Radio OH observations of 9P/Tempel 1 before and after Deep Impact   总被引：1，自引：0，他引：1  

Ellen S. Howell  Amy J. Lovell  F. Peter Schloerb 《Icarus》2007,187(1):228-239

We observed 18-cm OH emission in Comet 9P/Tempel 1 before and after Deep Impact. Observations using the Arecibo Observatory 305 m telescope took place between 8 April and 9 June, 2005, followed by post-impact observations using the National Radio Astronomy Observatory 100 m Green Bank Telescope 4-12 July, 2005. The resulting spectra were analyzed with a kinematic Monte Carlo model which allows estimation of the OH production rate, neutral gas outflow velocity, and distribution of the out-gassing from the nucleus. We detected typically 24% variability from the overall OH production rate trend in the two months leading up to the impact, and no dramatic increase in OH production in the days post-impact. Generally, the coma is well-described, within uncertainties, by a symmetric model with OH production rates from 1.6 to , and mean water outflow velocity of . At these low production rates, collisional quenching is expected to occur only within 20,000 km of the nucleus. However, our best-fit average quenching radius is 64,200 ± 22,000 km in April and May.  相似文献   

Radio observations of Comet 9P/Tempel 1 before and after Deep Impact     

Nicolas Biver  Dominique Bockelée-Morvan  Jacques Crovisier  Alain Lecacheux  Gabriel Paubert  Matthew Sumner  Åke Hjalmarson  Anders Winnberg  Aage Sandqvist 《Icarus》2007,187(1):253-271

Comet 9P/Tempel 1 was the target of a multi-wavelength worldwide investigation in 2005. The NASA Deep Impact mission reached the comet on 4.24 July 2005, delivering a 370-kg impactor which hit the comet at 10.3 km s⁻¹. Following this impact, a cloud of gas and dust was excavated from the comet nucleus. The comet was observed in 2005 prior to and after the impact, at 18-cm wavelength with the Nançay radio telescope, in the millimeter range with the IRAM and CSO radio telescopes, and at 557 GHz with the Odin satellite. OH observations at Nançay provided a 4-month monitoring of the outgassing of the comet from March to June, followed by the observation of H₂O with Odin from June to August 2005. The peak of outgassing was found to be around between May and July. Observations conducted with the IRAM 30-m radio telescope in May and July 2005 resulted in detections of HCN, CH₃OH and H₂S with classical abundances relative to water (0.12, 2.7 and 0.5%, respectively). In addition, a variation of the HCN production rate with a period of 1.73±0.10 days was observed in May 2005, consistent with the 1.7-day rotation period of the nucleus. The phase of these variations, as well as those of CN seen in July by Jehin et al. [Jehin, E., Manfroid, J., Hutsemékers, D., Cochran, A.L., Arpigny, C., Jackson, W.M., Rauer, H., Schulz, R., Zucconi, J.-M., 2006. Astrophys. J. 641, L145-L148], is consistent with a rotation period of the nucleus of 1.715 days and a strong variation of the outgassing activity by a factor 3 from minimum to maximum. This also implies that the impact took place on the rising phase of the “natural” outgassing which reached its maximum ≈4 h after the impact. Post-impact observations at IRAM and CSO did not reveal a significant change of the outgassing rates and relative abundances, with the exception of CH₃OH which may have been more abundant by up to one order of magnitude in the ejecta. Most other variations are linked to the intrinsic variability of the comet. The Odin satellite monitored nearly continuously the H₂O line at 557 GHz during the 38 h following the impact on the 4th of July, in addition to weekly monitoring. Once the periodic variations related to the nucleus rotation are removed, a small increase of outgassing related to the impact is present, which corresponds to the release of ≈5000±2000 tons of water. Two other bursts of activity, also observed at other wavelengths, were seen on 23 June and 7 July; they correspond to even larger releases of gas.  相似文献   

Palomar and Table Mountain observations of 9P/Tempel 1 during the Deep Impact encounter: First results     

James M. Bauer  Paul R. Weissman  Mitchell Troy  Carey M. Lisse  Martha S. Hanner 《Icarus》2007,187(1):296-305

We present the first results of the Palomar Adaptive Optics observations taken during the Deep Impact encounter with 9P/Tempel 1 in July 2005. We have combined the Palomar near-IR imaging data with our visual wavelength images obtained simultaneously at JPL's Table Mountain Observatory to cover the total wavelength range from 0.4 to 2.3 μm in the B, V, R, I, J, H, and K filter bands, spanning the dates from 2005 July 03-07. We also include in our overall analysis images taken on the pre-encounter dates of June 1 and June 15, 2005. The broad wavelength range of our observations, along with high temporal resolution, near-IR sensitivity, and spatial resolution of our imaging, have enabled us to place constraints on the temperature of the impact flash and incandescent plume of >700 K, and to provide mean dust velocities of order approximately 1.25 h after impact derived from our 1.64 μm observations. Our ejected dust mass estimates, as derived from our near-IR observations, are an order of magnitude less than those previously reported for visual wavelength observations.  相似文献