伽利略系统及其对IGS用户提供的潜在利益

详细介绍了伽利略系统的主要技术特性、当前状态,其对IGS带来的潜在利益以及伽利略系统对IGS的倡议行动和长期计划.     

基于图像结构的无参考模糊图像及其复原图像质量评价方法

针对传统图像的质量评价测度。提出了一种基于边缘检测的无参考模糊图像评价模型。通过测量梯度图像的梯度边缘信息,来评价模糊退化图像和带有模糊效应的复原图像,实验表明：利用本测度所得到的模糊图像质量评价结果与主观评价结果有很好的相关性。本测度较准确地反映了人,对模糊图像质量的主观感受,对于带有模糊效应的复原图像的评价结果也较为符合主观评价结果。     

基于移动监测数据的不同城市场景下PM2.5浓度精细模拟与时空特征解析

城市内部PM_2.5浓度分布具有明显的空间异质性,而传统方法基于遥感数据或监测站点数据进行分析,难以揭示高时空分辨率下城市内部的PM_2.5浓度分布特征,缺少不同时刻城市场景（如：道路、工业区、住宅区等）对PM_2.5浓度复杂非线性影响的解析。本研究将移动监测传感器安装于快递车上,采集福州市主城区南部不同类型场景的PM_2.5浓度,然后融合地理加权回归（Geographical Weighted Regression, GWR）和梯度提升决策树（Gradient Boosting Decision Tree, GBDT）方法,提出一种基于GWR-GBDT的PM_2.5模拟与场景解析模型,能够较好地拟合气象、场景因素与PM_2.5浓度的非线性关系,提升了城市PM_2.5污染精细监测能力;并结合部分依赖图解析不同时段不同场景因素对PM_2.5浓度的非线性作用影响。结果表明：① 基于移动PM_2.5浓度监测数据,利用GWR-GBDT模型能够较好地模拟城市场景、气象和PM_2.5浓度之间的非线性关系,能够有效精细模拟PM_2.5浓度的空间分布,十折验证R²结果为0.52~0.94;② 通过部分依赖图分析同一场景在不同时段对PM_2.5浓度响应的异质性,发现各类场景对PM_2.5浓度提升或抑制作用并不稳定;③ 解析不同时段人类活动与城市场景对PM_2.5浓度的交互作用发现,教育医疗单位和住宅区两类场景对PM_2.5浓度的提升作用都与人类通勤有密切关系,高污染场景中的建筑工地在采取的洒水降尘措施后能在数小时内有效缓解PM_2.5污染,公园文体服务区在多数时段对PM_2.5浓度具有抑制作用,工业区和道路多数时段会致使对PM_2.5浓度提升;④ 从PM_2.5浓度的空间分布来看,福州市主城区南部PM_2.5浓度总体呈现东南高-西北低的分布趋势,建筑工地、道路和工业区场景轻度以上污染面积占比明显高于其他场景,公园场景总体PM_2.5浓度较低,山体公园傍晚会受到周边工业区的影响而导致PM_2.5浓度升高,而城市陆地外围水域对沿岸PM_2.5浓度具有抑制作用;⑤ 研究结果可为不同场景下PM_2.5污染精细化治理、城市规划以及老人、儿童等高危人群的PM_2.5污染暴露风险防范提供支持。     

FN5井区夏子街组异常高阻段成因及油气成藏主控因素

通过岩心、薄片、构造演化史、古地貌等对FN5井区二叠系夏子街组异常高阻段进行综合分析.结果表明:FN5井区二叠系夏子街组异常高阻段发育2种岩性,高阻致密隔层以粗粒级云化凝灰质砂砾岩为主;低阻储层段以细粒级凝灰质细(中细)砂岩为主,储集空间具裂缝—孔隙双重介质特征.垂向上主要分布在夏子街组中部的P2x22砂层组;平面上主要分布在扇三角洲前缘近岸坡折带以下FC1—F20—FN055—FN5—W27井一带,面积为6.2km2,平面形态呈孤立的土豆状.油藏类型为东南方向受乌南断裂控制、其余方向受岩性控制的构造—岩性油藏.其展布受扇三角洲前缘的近岸水下坡折控制,后期成藏受控于异常高阻段的厚度及距主控断裂乌南断裂的距离.具有油层垂向厚度大、单井产量高、储量丰度高特征.为乌尔禾地区二叠系2011年探明储量培植及2012年增储上产的主要层位.     

准噶尔盆地小拐地区佳木河组储层特征及主控因素

小拐地区佳木河组属低孔、低渗储层,为明确该区储层的主控因素,根据岩心观测、薄片鉴定、分析化验等结果,研究其沉积特征、储集空间、物性特征、成岩作用等.结果表明:小拐地区佳木河组为一套巨厚陆上冲积扇—扇三角洲复合沉积,岩石颗粒组分复杂、成熟度低,储层主要储集空间包括界面孔、微裂缝、溶蚀孔、构造裂缝等;储层受裂缝—孔隙双重介质影响,非均质性强.该区构造裂缝较为发育,以构造成因的直立剪切裂缝为主,对储层改造具有重要作用,裂缝发育情况与油气显示及产能密切相关;该区储层发育的主控因素包括岩性岩相、构造运动、成岩作用等.该区岩性岩相是控制储层发育的根本条件,构造运动产生的主控断裂有利于油气运移与聚集、强化储层裂缝发育,成岩作用中的溶蚀作用有效改善区内储层储渗性能.     

副溶血弧菌噬菌体衣壳蛋白的组成分析及其主组分的分离纯化

<正>目前,针对传统抗生素治疗细菌感染中出现的耐药性及药物残留等问题,亟需寻找一种新型的替代药物。噬菌体对治疗病原菌感染的多种优越性,成为抗菌新药研究开发的新热点和理想材料。对噬菌体的溶菌机制[1-3]以及实践应用[4-6]等已有较多报道。笔者主要对副溶血弧菌噬菌体衣壳蛋白的组成进行了初步研究,并用SDS-PAGE电泳法分离纯化了其主要组分,为制备该蛋白质的抗体,建立副溶血弧菌噬菌体的免疫学检测方法奠定基础。     

Investigations of Stephenson's Hα stars

Hitherto unstudied objects from Stephenson's list of Hα emission line objects at high galactic latitude were observed spectroscopically to prove their nature. 9 out of 11 objects show Hα in emission. Spectroscopy combined with photometric information indicates most of them being classical Be stars, while one object is a Post‐AGB star and one a T‐Tauri star. The classification of two objects, which are showing Hα in emission, is unclear. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

A direct imaging search for close stellar and sub‐stellar companions to young nearby stars

A total of 28 young nearby stars (ages ≤60 Myr) have been observed in the K_s‐band with the adaptive optics imager Naos‐Conica of the Very Large Telescope at the Paranal Observatory in Chile. Among the targets are ten visual binaries and one triple system at distances between 10 and 130 pc, all previously known. During a first observing epoch a total of 20 faint stellar or sub‐stellar companion‐candidates were detected around seven of the targets. These fields, as well as most of the stellar binaries, were re‐observed with the same instrument during a second epoch, about one year later. We present the astrometric observations of all binaries. Their analysis revealed that all stellar binaries are co‐moving. In two cases (HD 119022 AB and FG Aqr B/C) indications for significant orbital motions were found. However, all sub‐stellar companion candidates turned out to be non‐moving background objects except PZ Tel which is part of this project but whose results were published elsewhere. Detection limits were determined for all targets, and limiting masses were derived adopting three different age values; they turn out to be less than 10 Jupiter masses in most cases, well below the brown dwarf mass range. The fraction of stellar multiplicity and of the sub‐stellar companion occurrence in the star forming regions in Chamaeleon are compared to the statistics of our search, and possible reasons for the observed differences are discussed. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Results and perspectives of young stellar object long look programs

Both Chandra and XMM‐Newton have performed long look programs for studying the YSO physics. I will discuss recent results on the controversial issue of Class 0 YSO X‐ray emission, the observational evidence of magnetic funnels interconnecting the YSO with its circumstellar disk and the Fe 6.4 keV fluorescent line emission and its origin. While recent results of the XMM‐Newton DROXO program challenge the “standard” interpretation of the Fe 6.4 kev line origin as due to photoionized fluorescing disk material, the discovery of X‐ray excited Ne 12.81 μ m line is a clear evidence of the interaction between X‐rays and disk material. Future long look observations with XMM‐Newton are required to clarify the X‐ray effects on YSO disk. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)