Total Synthesis of Marine Cyclic Enol-Phosphotriester Salinipostin Compounds

Due to their structural diversity and variety of biological activities, marine natural products have been the subject of extensive study. These compounds, especially phospholipid polycyclic aromatic hydrocarbons, have a wide range of pharmacological applications, including embedded DNA and central nervous system, anti-tumor, anti-virus, anti-parasite, anti-bacterial, and antithrombotic effects. Unfortunately, the insufficient drug sources have limited the development of these compounds. In this study, we isolated salinpostin compounds from a fermentation solution of marine-derived Salinospora sp., which has a common bicyclic enol-phosphotriester core framework, as well as potent and selective antimalarial activities against P. falciparum with EC_(50)=50 nmolL~(-1). The chemical synthesis of these compounds in greater quantities is necessary for their use in bioactivity studies. Thus we explored a short route with high yields and mild reaction conditions, which can generate combinatorial libraries for drug discovery and lead optimization. We developed a new total synthesis method for six cyclic enol-phosphotriester salinipotin compounds and their diastereomers. For the total synthesis of cyclipostin P, we prepared cyclic enol-phosphotriester salinipostin compounds in 10 steps from a readily accessible starting material, 1,3-dihydroxyacetone, and obtained an overall yield of 1.29%. We fully characterized these compounds by proton nuclear magnetic resonance(~1H-NMR), carbon-13 NMR(~(13)C-NMR), and high-resolution mass spectrometry(HRMS) analyses, and found they coincide absolutely with the same compounds reported previously.     

DMSP/OLS夜间灯光数据研究成果知识图谱分析

利用CitesSpace软件对1997-2017年DMSP/OLS夜间灯光数据进行知识图谱分析,梳理国内外研究热点与演化历史,发掘研究难点,为后来研究者提供方向。本文选取Web of Science 核心数据集数据库收录的文献,进行合著特征分析、关键词共现分析和文献共被引分析。结果表明：① 夜间灯光数据相关研究最活跃的国家、机构和作者分别是美国、中国科学院和Elvidge;② 社会经济条件估计（人口、人口密度和电力）和城市扩展变化监测一直是国内外研究的热点和前沿;③ 目前的研究难点是如何减少灯光溢出效应以及灯光过饱和现象对研究精度的影响;④ 研究学科交叉性强,涉及地理学、测绘科学与技术、应用经济学、社会学等领域。因此,未来的研究趋势主要表现在数据处理方法的优化、研究领域的拓展以及深化已有研究成果3个方面。     

“海上丝绸之路”沿线重要港口竞争力评价

“海上丝绸之路”是促进亚欧和亚非互联互通的重要通道,对其沿线重要港口的竞争力研究,可以为海上丝绸之路的建设提供参考。本文综合考虑港口的自然条件、腹地环境、基础设施、服务水平、政府廉洁度,及其在航运网络中的地位差别等因素,运用熵权-层次分析法对沿线51个国家的99个重要港口的竞争力进行评价。结果表明,① 港口综合竞争力空间分布呈明显的区域化特征,且与国家经济发展水平显著相关,地中海地区港口竞争力普遍较强,亚洲次之,非洲最弱。② 港口的网络地位对竞争力的影响最大,竞争力强的港口多位于重要水域的战略通道,网络地位高,辐射范围广。③ 我国投资的部分沿线港口综合竞争力与成熟港口之间还存在一定差距,但是具备较大的竞争力提升空间。     

融合实时路况信息的北京市就医可达性分析

就医可达性是衡量区域医疗公平性的标准之一,为均衡医疗设施配置提供了理论依据。两步移动搜索法(2SFCA)是一种较为成熟的可达性计算方法,但仍存在研究最小基本单元尺度较大、供需点间时间估算忽略路网的通达性和实时路况等问题。本文利用高德地图获取依据实时路况规划最优驾车路线的时间,通过2SFCA评估北京市1 575个居民点在工作日的5个时段和4种出行时间阈值内到达208所医院的可达性。结果表明:北京市就医可达性空间分布不均衡,随搜索阈值的增大,分布形态由多峰值分布向以西城区和东城区为中心的环状扩散分布转换。时段分异特征显著,各时段可达性为一般及以上居民点比例由高至低依次为夜晚、中午、下午、早高峰、晚高峰。     

北斗在南/北极地区的基本定位性能评估

基于BDS、GPS系统的星座结构,对当前的BDS二代导航系统（BD2）、全部建成后的BDS系统在极地科考站（黄河站、昆仑站、中山站、长城站）和北极圈的可见卫星数、DOP值、定位精度等进行评估,并将建成后的BDS、GPS及其组合系统在南/北极的基本定位性能进行对比分析。仿真结果表明,当前的BD2只实现了极地的部分覆盖,对极地提供导航定位的能力有限,大范围内的定位精度大于30.0 m; BDS在极地的定位精度将与GPS相当,可见卫星数可达13颗左右,PDOP值优于1.6,定位精度优于8.0 m;GPS/BDS组合后在极地的PDOP值优于1.4,定位精度优于6.0 m。
     

BDS卫星失效对区域定位精度的影响评估

基于STK软件实现了2016-09 BDS系统星座结构的仿真,并选取可见卫星数、DOP值、系统可用性作为评估BDS卫星星座设计结构的指标,分析单颗与全部倾斜轨道卫星（IGSO）、地球静止轨道卫星（GEO）失效后对我国大陆地区BDS系统可用性的影响。结果表明,IGSO4卫星与GEO5卫星失效后对BDS在区域的定位性能影响较大,失效后的GDOP值分别为1.98、2.16。取BDS卫星正常运行时区域平均GDOP最大值(S=2.60)作为系统可用性阈值时,系统可用性分别降低了1.79%、32.63%;阈值取2S(5.20)、3S(7.80)、4S(10.40)、5S(13.00)时,系统可用性均可达100.00%。GEO整体失效后BDS系统在高精度定位中仍部分可用,而IGSO整体失效后BDS系统可用性受到大幅度限制。因此,增加在轨备份卫星时需重点考虑GEO5、IGSO4,并适当增加IGSO卫星的数目。     

沉积盆地异常低压(负压)与油气分布

在沉积盆地油气勘探过程中,异常压力与油气聚集的关系愈显密切,而异常压力不仅仅是指异常高压,国内外在发现许多异常高压油气藏的同时,也发现了相当数量的异常低压油气藏,而且异常低压在世界许多盆地中均有分布。因此,深入研究异常低压的形成机理及与油气分布的关系,同样重要和不容忽视。本文介绍了异常低压的概念、特征和分类,详细分析了异常低压的形成机制：地层剥蚀卸载后的弹性回返(反弹)作用、流体的供排不平衡、轻烃的扩散作用、断裂和不整合面的压力释放作用、渗透作用和温度变化等;最后论述了异常低压与油气分布的关系。     

Origin of EL3 chondrites: Evidence for variable C/O ratios during their course of formation—A state of the art scrutiny

Mineral inventories of enstatite chondrites; (EH and EL) are strictly dictated by combined parameters mainly very low dual oxygen (fO₂) and sulfur (fS₂) fugacities. They are best preserved in the Almahata Sitta MS‐17, MS‐177 fragments, and the ALHA 77295 and MAC 88136 Antarctic meteorites. These conditions induce a stark change of the geochemical behavior of nominally lithophile elements to chalcophile or even siderophile and changes in the elemental partitioning thus leading to formation of unusual mineral assemblages with high abundance of exotic sulfide species and enrichment in the metallic alloys, for example, silicides and phosphides. Origin and mode of formation of these exotic chondrites, and their parental source regions could be best scrutinized by multitask research experiments of the most primitive members covering mineralogical, petrological, cosmochemical, and indispensably short‐lived isotopic chronology. The magnitude of temperature and pressure prevailed during their formation in their source regions could eventually be reasonably estimated: pre‐ and postaccretionary could eventually be deduced. The dual low fugacities are regulated by the carbon to oxygen ratios estimated to be >0.83 and <1.03. These parameters not only induce unusual geochemical behavior of the elements inverting many nominally lithophile elements to chalcophile or even siderophile or anthracophile. Structure and mineral inventories in EL3 and EH3 chondrites are fundamentally different. Yet EH3 and EL3 members store crucial information relevant to eventual source regions and importantly possible variation in C/O ratio in the course of their evolution. EL3 and EH3 chondrites contain trichotomous lithologies (1) chondrules and their fragments, (2) polygonal enstatite‐dominated objects, and (3) multiphase metal‐rich nodules. Mineralogical and cosmochemical inventories of lithologies in the same EL3 indicate not only similarities (REE inventory and anomalies in oldhamite) but also distinct differences (sinoite‐enstatite‐graphite relationship). Oldhamite in chondrules and polygonal fragments in EL3 depict negative Eu anomaly attesting a common cosmochemical source. Metal‐dominated nodules in both EL3 and EH3 are conglomerates of metal clasts and sulfide fragments in EH3 and concentrically zoned C‐bearing metal micropebbles (≥25 μm ≤50 μm) in EL3 thus manifesting a frozen in unique primordial accretionary metal texture and composition. Sinoite‐enstatite‐diopside‐graphite textures reveal a nucleation and growth strongly suggestive of fluctuating C/O ratio during their nucleation and growth in the source regions. Mineral inventories, sulfide phase relations, sinoite‐enstatite‐graphite intergrowth, carbon and nitrogen isotopic compositions of graphite, spatial nitrogen abundance in graphite in metal nodules, and last but not least ¹²⁹I/¹²⁹Xe and ⁵³Mn/⁵³Cr systematics negate any previously suggested melting episode, pre‐accretionary or dynamic, in parental asteroids.     

On the Collision Nature of Two Coronal Mass Ejections: A Review

Observational and numerical studies have shown that the kinematic characteristics of two or more coronal mass ejections (CMEs) may change significantly after a CME collision. The collision of CMEs can have a different nature, i.e. inelastic, elastic, and superelastic processes, depending on their initial kinematic characteristics. In this article, we first review the existing definitions of collision types including Newton’s classical definition, the energy definition, Poisson’s definition, and Stronge’s definition, of which the first two were used in the studies of CME–CME collisions. Then, we review the recent research progresses on the nature of CME–CME collisions with the focus on which CME kinematic properties affect the collision nature. It is shown that observational analysis and numerical simulations can both yield an inelastic, perfectly inelastic, merging-like collision, or a high possibility of a superelastic collision. Meanwhile, previous studies based on a 3D collision picture suggested that a low approaching speed of two CMEs is favorable for a superelastic nature. Since CMEs are an expanding magnetized plasma structure, the CME collision process is quite complex, and we discuss this complexity. Moreover, the models used in both observational and numerical studies contain many limitations. All of the previous studies on collisions have not shown the separation of two colliding CMEs after a collision. Therefore the collision between CMEs cannot be considered as an ideal process in the context of a classical Newtonian definition. In addition, many factors are not considered in either observational analysis or numerical studies, e.g. CME-driven shocks and magnetic reconnections. Owing to the complexity of the CME collision process, a more detailed and in-depth observational analysis and simulation work are needed to fully understand the CME collision process.     

EUV and Magnetic Activities Associated with Type-I Solar Radio Bursts

Type-I bursts (i.e. noise storms) are the earliest-known type of solar radio emission at the meter wavelength. They are believed to be excited by non-thermal energetic electrons accelerated in the corona. The underlying dynamic process and exact emission mechanism still remain unresolved. Here, with a combined analysis of extreme ultraviolet (EUV), radio and photospheric magnetic field data of unprecedented quality recorded during a type-I storm on 30 July 2011, we identify a good correlation between the radio bursts and the co-spatial EUV and magnetic activities. The EUV activities manifest themselves as three major brightening stripes above a region adjacent to a compact sunspot, while the magnetic field there presents multiple moving magnetic features (MMFs) with persistent coalescence or cancelation and a morphologically similar three-part distribution. We find that the type-I intensities are correlated with those of the EUV emissions at various wavelengths with a correlation coefficient of 0.7?–?0.8. In addition, in the region between the brightening EUV stripes and the radio sources there appear consistent dynamic motions with a series of bi-directional flows, suggesting ongoing small-scale reconnection there. Mainly based on the induced connection between the magnetic motion at the photosphere and the EUV and radio activities in the corona, we suggest that the observed type-I noise storms and the EUV brightening activities are the consequence of small-scale magnetic reconnection driven by MMFs. This is in support of the original proposal made by Bentley et al. (Solar Phys. 193, 227, 2000).