Effect of NOAA satellite orbital drift on AVHRR-derived phenological metrics

The U.S. Geological Survey (USGS) Earth Resources Observation and Science (EROS) Center routinely produces and distributes a remote sensing phenology (RSP) dataset derived from the Advanced Very High Resolution Radiometer (AVHRR) 1-km data compiled from a series of National Oceanic and Atmospheric Administration (NOAA) satellites (NOAA-11, −14, −16, −17, −18, and −19). Each NOAA satellite experienced orbital drift during its duty period, which influenced the AVHRR reflectance measurements. To understand the effect of the orbital drift on the AVHRR-derived RSP dataset, we analyzed the impact of solar zenith angle (SZA) on the RSP metrics in the conterminous United States (CONUS). The AVHRR weekly composites were used to calculate the growing-season median SZA at the pixel level for each year from 1989 to 2014. The results showed that the SZA increased towards the end of each NOAA satellite mission with the highest increasing rate occurring during NOAA-11 (1989–1994) and NOAA-14 (1995–2000) missions. The growing-season median SZA values (44°–60°) in 1992, 1993, 1994, 1999, and 2000 were substantially higher than those in other years (28°–40°). The high SZA in those years caused negative trends in the SZA time series, that were statistically significant (at α = 0.05 level) in 76.9% of the CONUS area. A pixel-based temporal correlation analysis showed that the phenological metrics and SZA were significantly correlated (at α = 0.05 level) in 4.1–20.4% of the CONUS area. After excluding the 5 years with high SZA (>40°) from the analysis, the temporal SZA trend was largely reduced, significantly affecting less than 2% of the study area. Additionally, significant correlation between the phenological metrics and SZA was observed in less than 7% of the study area. Our study concluded that the NOAA satellite orbital drift increased SZA, and in turn, influenced the phenological metrics. Elimination of the years with high median SZA reduced the influence of orbital drift on the RSP time series.     

Progressive Transformation of a Flux Rope to an ICME

The solar wind conditions at one astronomical unit (AU) can be strongly disturbed by interplanetary coronal mass ejections (ICMEs). A subset, called magnetic clouds (MCs), is formed by twisted flux ropes that transport an important amount of magnetic flux and helicity, which is released in CMEs. At 1 AU from the Sun, the magnetic structure of MCs is generally modeled by neglecting their expansion during the spacecraft crossing. However, in some cases, MCs present a significant expansion. We present here an analysis of the huge and significantly expanding MC observed by the Wind spacecraft during 9 – 10 November 2004. This MC was embedded in an ICME. After determining an approximate orientation for the flux rope using the minimum variance method, we obtain a precise orientation of the cloud axis by relating its front and rear magnetic discontinuities using a direct method. This method takes into account the conservation of the azimuthal magnetic flux between the inbound and outbound branches and is valid for a finite impact parameter (i.e., not necessarily a small distance between the spacecraft trajectory and the cloud axis). The MC is also studied using dynamic models with isotropic expansion. We have found (6.2±1.5)×10²⁰ Mx for the axial flux and (78±18)×10²⁰ Mx for the azimuthal flux. Moreover, using the direct method, we find that the ICME is formed by a flux rope (MC) followed by an extended coherent magnetic region. These observations are interpreted by considering the existence of a previously larger flux rope, which partially reconnected with its environment in the front. We estimate that the reconnection process started close to the Sun. These findings imply that the ejected flux rope is progressively peeled by reconnection and transformed to the observed ICME (with a remnant flux rope in the front part).     

基于GNSS-RTK的在建超高层风载动态变形监测

首先以海星达H32全能型GNSS-RTK接收机为试验仪器,进行不同星系组合的RTK定位精度试验研究。然后以在建的天津高银117大厦为监测对象,采用GPS+GLONASS+BDS三星系组合对其进行现场强风作用下的RTK动态变形监测。利用巴特沃斯滤波对实测数据进行去噪处理,得到各测点的位移曲线。分析结果表明:GPS单星系定位的平面坐标精度相对较差,双星系组合定位的平面坐标精度与三星系组合定位的平面坐标精度基本相当,但GPS+GLONASS+BDS三星系组合定位的稳定性和可靠性最强;由于施工阶段大厦结构的刚度和整体性与竣工后存在差异,故在强风作用下其按一定施工步距滞后的低矮外框的振动位移幅度大于其高耸内筒结构的振动位移幅度;大厦外框和内筒均存在横风向振动位移,且横风向振动位移与顺风向振动位移的大小相近;监测环境对监测结果有着一定的影响,66层各点的监测值误差要大于95层各点的监测值误差。     

雷达图像中的转换构造信息及其应用

低序次断裂是地壳变形的直接产物，具有丰富的构造变形信息，经过转换的低序次构造。形式多样，图案复杂，是构造研究的重要对象，也是地表稳定性研究的重要基础。利用香港地区航空雷达图像资料，提取其中低序次构造的弱信息，建立转换变形模型，以分析区内不稳定地表的构造背景。区内北东向断裂是主要构造，其右行剪切形成一系列低序次R面，P面，R^1面构造，在雷达图像上表现为线性弱信息并且与微地貌发育有关。利用线性构造增强，提取技术和低序次构造组合分析方法，结合野外地质调查，确定马鞍山地区EW向的张性破裂是NE向张剪断裂的转换，是造成马鞍山滑坡的重要地质因素。     

巴音布鲁克高寒区气象观测分析

本文通过2011-2013年中天山高寒无人区自建的自动气象站获取的稀缺气象资料,客观地揭示了观测区域的气象条件,给出部分气象特征参数变化特征,为中天山高山达坂区气象观测研究工作奠定一定基础,并得出如下结果：（1）迎风坡盛行风向SE、N,SE占35%,N占25%,N向风力集中4级以下,SE明显偏大,3级风比重15%,4级风比重7%,5级风比重4%;6级风比重1%,6级以上的风力几乎为零。背风坡主导风向角度范围在247.5°-337.5°,风力基本在6级以下,6级及以上风力出现概率不足1%。3-5级风占的比重较大。（2）日平均气温≤-10℃日数所占观测总日数的百分比,其值分别为：0.0%（恰西）、44.5%（江不肯达坂）、9.8%（江巴口子）、15.1%（铁力买提达坂）。恰西、江不肯达坂、江巴口子、铁力买提达坂4站日平均相对湿度≥80%的频率分别为5.9%、18.4%、16.1%和22.6%。（3）换算得出恰西、江不肯达坂、江巴口子、铁力买提达坂观测期间10m高度最大瞬时风速与小时平均风速分别为33.8/27.9m/s、41.0/27.3 m/s、25.7/17.7m/s、34.0/17.2 m/s。     

2010年西北太平洋与南海热带气旋活动异常的成因分析

利用中国气象局热带气旋（TC）资料、NCEP/NCAR 再分析资料和美国 NOAA 向外长波辐射（OLR）等资料,分析了2010年西北太平洋（WNP）及南海（SCS）热带气旋活动异常的可能成因,讨论了同期大气环流配置和海温外强迫对TC生成和登陆的动力和热力条件的影响。结果表明,2010年生成TC频数明显偏少,生成源地显著偏西,而登陆TC频数与常年持平。导致7～10月TC频数明显偏少的大尺度环境场特征为：副热带高压较常年异常偏强、西伸脊点偏西,季风槽位置异常偏西,弱垂直风切变带位置也较常年偏西且范围偏小,南亚高压异常偏强,贝加尔湖附近对流层低高层均为反气旋距平环流,这些关键环流因子的特征和配置都不利于 TC 在WNP的东部生成。影响TC活动的外强迫场特征为：2010年热带太平洋经历了El Ni?o事件于春末夏初消亡、La Ni?a事件于7月形成的转换;7～10月,WNP海表温度维持正距平,140°E以东为负距平且对流活动受到抑制;暖池次表层海温异常偏暖,对应上空850 hPa为东风距平,有利于季风槽偏西和TC在WNP的西北侧海域生成。WNP海表温度和暖池次表层海温的特征是2010年TC生成频数偏少、生成源地异常偏西的重要外强迫信号。有利于7～10月热带气旋西行和登陆的500 hPa风场特征为：北太平洋为反气旋环流距平,其南侧为东风异常,该东风异常南缘可到25°N,并向西扩展至中国大陆地区;南海和西北太平洋地区15°N以南的低纬也为东风异常;在这样的风场分布型下,TC容易受偏东气流引导西行并登陆我国沿海地区。这是2010年生成TC偏少但登陆TC并不少的重要环流条件。     

Energy distributions of the large-scale horizontal currents caused by wind in the baroclinic ocean

Wind is the main energy source for the generation of the internal waves and the ocean mixing. Wunsch[1] estimated that about 1 TW (1 TW = 1012 W) energy was transported into the ocean from the winds by us-ing the altimeter data. Watanabe et al.[2] numerically calculated that the mixing processes obtained 0.7 TW energy from the global wind, which afforded most of the energy needed by the maintenance of the Merid-ional Overturning Circulation (MOC). During the past 50 years, in the Norther…     

青海互助一次局地强降水天气多普勒雷达回波分析

利用西宁CINRAD/CD多普勒天气雷达资料及自动站观测数据等从影响降水的主要因子方面探讨了2011年7月2日晚青海互助县一次局地强降水的成因,结果表明:多单体强回波带的活动是造成互助短时强降水的主要原因;速度图上强的辐合和逆风区是预报强降水的关键因子;垂直风廓线图上强烈的垂直风切变是不稳定能量积聚的表现,与强降水联系紧密;垂直累计液态含水量(VIL)和回波顶高也能为强降水预报提供有效信息。     

Tides in the Tongan Region of the Pacific Ocean

Tidal levels and currents in the Tongan region of the Pacific were simulated using a two-dimensional frequency-domain finite element model. The eight major diurnal and semidiurnal tidal constituents were modeled successfully, using open boundary conditions taken from a global tidal model based on the Topex/Poseidon satellite altimeter. Comparison of model results with observations from the single tide gauge site in the area were later used to adjust the boundary conditions. The validity of omitting horizontal eddy viscosity from the finite element model was checked by running an equivalent finite difference model. The results show that although the submarine Tongan ridge does not appear to trap tidal energy, there are residual tidal currents and possible recirculations which are capable of influencing biological productivity around Tonga. The model results are reduced to a simple method for predicting tidal heights in outlying areas, based only on the tidal calendar for the capital, Nuku'alofa.     

凤城市赛马镇风洞洞穴特征及发育基本条件

赛马镇风洞是我国东北规模较大的岩溶洞穴,洞长在2000m以上,已探测长度1265m.风洞具有纵坡降较小、支洞繁多、形态奇异及国内罕见的溶蚀景观“天锅”等特征.岩性、构造、水文地质特征等是控制洞穴发育的基本条件.风洞的发育约始于中更新世40万年前.