X-ray and optical variability of the seyfert galaxy NGC 7469

Based on our UBV RI observations and X-ray data from the RXTE satellite, we have investigated the variability of the galaxy NGC 7469 over the period 1995–2009. In 1995–2000, the optical brightness of the galactic nucleus changed almost by 1 ^m in the U band. In 2000–2009, the amplitude of the optical variations was considerably lower. Regular X-ray observations began only in 2003. The X-ray fractional variability amplitude is higher than the optical one. The optical variability amplitude decreases with increasing wavelength. The full width at half maximum of the X-ray and B-band autocorrelation functions is about 8 and 62 days, respectively. The structure functions (SF) in the X-ray range on time scales up to 7 days and in the optical range on time scales up to 100 days have the form of a power law SF(τ) ∼ τ ^b , where τ is the time shift. On time scales of more than a day, where both structure functions have been determined rather reliably, their slopes differ markedly: b = 1.34 ± 0.06 and b = 0.25 ± 0.05 for the optical and X-ray ranges, respectively. The X-ray and B-band structure functions begin to flatten, respectively, near 6–8 days and on time scales of about 90 days. The observed structure functions can be described by the model of a superposition of independent Gaussian flares whose number changes with duration ω as n(ω) ∼ ω ^α and whose amplitudes depend on duration as A(ω) ∼ ω ^β. The flux distribution and the flux-amplitude relation are consistent with the model of a light curve in the form of a superposition of random flares. Once the fast intensity variations have been filtered out on long time scales, the X-ray light curve correlates well with the optical one. No lag of the X-ray variations relative to those in the B band is detected. The light variations in the R and I bands lag behind those in the B band calculated from the centroid of the cross-correlation function by 2.6 and 3.5 days, respectively, at a 3σ confidence level.     

罗北凹地富钾卤水中锂、硼的空间分布和富集规律研究

文章基于自组织神经网络（SOM）和Kmeans耦合（SOM-KM）方法,利用罗北凹地65组富钾卤水水化学数据,对富钾卤水中锂（Li）和硼（B）资源空间分布和富集规律进行了系统性研究。研究发现富钾卤水中Li,B含量表现出一定的垂向分异性,自上而下B浓度增高,Li浓度降低。聚类结果表明,罗北凹地富钾卤水可聚为4类,各类地下水中Li、B浓度具有明显的空间差异性,高浓度的Li、B集中分布在罗北凹地中东部区域。此外,水化学特征离子分析结果表明,罗北凹地富钾卤水中Li、B元素富集主要受到蒸发浓缩及盐岩溶滤作用控制。     

Estimation of Solar Activity Based on VHF Radar Data

Geomagnetism and Aeronomy - The index of integral solar activity F10.7 is one of the main input parameters of existing ionospheric models, including the model used at early-warning radar stations...     

TOPMODEL在珠江流域布柳河流域的应用及其与新安江模型的比较

TOPMODEL是一种以地形为基础的半分布式流域水文模型.对珠江流域布柳河流域的DEM信息进行处理,提取流域的水系、子流域边界、地形指数及水流路径距离的分布,将TOPMODEL应用于该流域中.另外将新安江模型也应用于该流域进行比较.此外,分析了两种模型结构差异所带来的模拟功能差异.两种模型模拟结果精度差异不大,而TOPMODEL实现了空间产流面积分布的可视化.     

基于大数据架构的地球物理观测数据管理系统

中国地震地球物理观测网络的核心业务软件“十五”地震前兆数据管理系统已运行十多年,随着观测数据量的增长,数据库的读取和统计查询的性能逐渐降低。此外,管理系统存在SQL注入和跨站脚本攻击等漏洞的安全问题,系统架构难以满足业务发展的需求。中国地震台网中心基于分布式组件的大数据架构,使用消息中间件和时序数据库等技术对管理系统进行重构,将原来存储于Oracle数据库中的地球物理观测数据、基础信息、产品数据等按照各自特点在时序数据库中建表,并将历史数据和增量数据都迁移到新的时序数据库,显著提升了系统读写和统计性能、数据的安全性和可用性(多副本技术)。分布式和容器化等技术的引入,增强了系统的高可用性,并可通过横向扩展进一步增加系统的处理能力。     

相交圆柱摆式波能装置俘获效率数值分析

摆式波能装置具有结构简单和转化效率高等特点,本文应用AQWA 软件基于势流理论对相交圆柱摆式波能装置进行了数值模拟研究,分析了轴间距比、结构阻尼、净浮力比、水深、波浪特性及吃水深度等主要参数对相交圆柱摆式波能装置俘获效率的影响,并与直板摆式波能装置的俘获效率进行了对比。结果表明：同样条件下,相交圆柱摆式波能装置往往比直板摆式波能装置的俘获效率更高;在研究范围内,轴间距比越大俘获效率越高;潮汐导致的水深变化对底铰摆式波能装置的俘获效率具有明显的影响,在工程应用中应采取适当的措施进行处理。     

新疆阿尔泰库吉尔特伟晶岩海蓝宝石矿物化学研究

海蓝宝石属绿柱石族矿物,产出于花岗伟晶岩中,其结晶过程可贯穿于伟晶质岩浆演化的不同阶段,同时也是岩浆熔体和流体包裹体的重要宿主矿物。库吉尔特伟晶岩是新疆阿尔泰可可托海地区众多伟晶岩脉中产出高质量海蓝宝石的LCT型伟晶岩。本文对库吉尔特伟晶岩中产出的海蓝宝石进行了主、微量元素和流体包裹体研究。流体包裹体岩相学显示,在海蓝宝石中熔体/熔体-流体包裹体(MI/M-FI)和流体包裹体(FI)分布呈现一定的规律, MI/M-FI主要集中在晶体的根部至中部,而FI则富集在边缘区域,说明该海蓝宝石的结晶过程经历了较为完整的伟晶岩岩浆演化阶段。测温结果显示,M-FI的均一温度>550℃,FI的均一温度范围为220~400℃,盐度介于0~14%之间,密度为0.6~0.9 g/cm²,流体属于中-高温、中-低盐度的H₂O-NaCl-CO₂体系。在结晶学和流体包裹体岩相学基础上确定出海蓝宝石晶体代表岩浆-热液过渡阶段和岩浆期后热液阶段的部位,进行电子探针(EPMA)和激光剥蚀电感耦合等离子体质谱分析(LA-ICP-MS),结果显示海蓝宝石为Fe元素主导致色,在海蓝宝石生长过程中Fe²⁺以Na⁺+Fe²⁺→Al³⁺的通道-八面体替代模式进入矿物晶格使其呈现蓝色。在伟晶岩演化早-中期,海蓝宝石中碱金属(Li、Na、K、Cs)与过渡族金属元素(Fe、Mg、Mn)含量变化稳定,进入晚期这些金属元素含量陡增。结合该地区板块运动长期处于挤压俯冲环境,推测库吉尔特伟晶岩岩浆演化过程处于非封闭的状态,晚期仍然有深部岩浆房富集Fe、Mg、Mn的流体呈脉动式注入,导致原始热液流体成分发生波动。     

Comparative Analysis of Mitochondrial Control Region Sequence from Three Flatfish Species （Pleuronectidae）

The 5‘-end of the mitochondrial control region sequences of three flatfishes (Pleuronectiformes: Pleuronectidae) were amplified and sequenced. These sequences were compared with those of other three Pleuronectids species retrieved from GenBank. A phylogenetic tree was constructed based on the partial control region sequences. The results of phylogenetic analysis are consistent with those of conventional systematics. Compared to previous studies, the structure of the 5‘-end of mitochondrial control region was analyzed. The terminal associated sequence motif and its complementary motif were identified at the 5‘-end of the sequences. A conserved sequence block, named as CM5‘ d, was identified in the 5‘-end of control region sequences in all Pleuronectids. Another central conserved sequence block, named as CSB-F, was detected in the central conserved blocks.     

Microwave observations of compact radio sources during solar eclipses on RT-22

Based on the observations of solar eclipses performed on the RT-22 radio telescope at CrAO in the wavelength range 2.0–3.5 cm, we consider the fine spatial structure of the microwave emission from the quiet Sun. We have established that the positions of compact radio sources with a typical size of about 7″.0 and coronal bright points coincide. The mean radio flux exceeds the level of the quiet Sun by 0.28 sfu. The brightness temperatures increase with wavelength and lie within the range 0.3–2.7 MK. Evidence for a nonthermal nature of the emission from compact radio sources has been obtained.