厚壳贻贝（Mytilus coruscus）McNF-κB基因的克隆及其在发育中的作用

核因子κB（Nuclear Factor kappa-B,NF-κB）具有免疫、炎症、凋亡、细胞增殖和发育的调节作用,目前NF-κB在脊椎动物和果蝇中的研究较为丰富,在贝类中的报道较少。为进一步探究NF-κB在厚壳贻贝（Mytilus coruscus）免疫和发育中的作用,本研究克隆了厚壳贻贝McNF-κB基因的序列全长,其全长为4 087 bp,开放阅读框为2 613 bp,编码871个氨基酸,具有典型的锚蛋白重复序列（ankyrinrepeat, ANK）结构域和死亡结构域。氨基酸序列分析结果发现,该基因与欧洲贻贝（Mytilus edulis）和地中海贻贝（Mytilus galloprovincialis）分别具有72.76%和66.58%同源性,且在系统进化树中与欧洲贻贝和地中海贻贝聚为一支。经实时荧光定量PCR（qRT-PCR）技术检验表明,McNF-κB基因于厚壳贻贝各组织均有分布,在鳃中表达最高;McNF-κB基因在厚壳贻贝眼点幼虫阶段和稚贝阶段均有表达,且在稚贝阶段表达量显著高于眼点幼虫阶段。利用RNA干扰技术沉默眼点幼虫McNF-κB基因后幼虫变态率显著下降,推测McNF-κB基因调控厚壳贻贝幼虫变态过程。本研究为探究McNF-κB基因如何调控厚壳贻贝发育奠定了基础。     

海水声速剖面基函数的重构性能分析

海水声速剖面通常使用经验正交函数（Empirical Orthogonal Function,EOF）进行稀疏表示,然而基函数会受到数据完备性和数据测量时间的制约,其代表性误差会导致声速剖面重构精度受限。为了提高声速剖面的重构精度,本文利用模糊C均值聚类对BOA_Argo历史数据集进行聚类分析,探讨不同聚类空间的训练集数据对实测声速剖面重构精度的影响。研究表明,声速剖面具有明显的时空聚集特性,聚类后的历史声速剖面集生成的基函数和平均声速剖面具有最优的重构性能。本文研究结果有助于为历史声速剖面训练集的选取提供实际指导意义,进而提高声速剖面重构精度乃至反演精度。     

RFI Test Observations at a Candidate Ska Site in China

Radio frequency interference (RFI) test observations were carried out at one of the candidate Square Kilometre Array (SKA) sites in Guizhou province, following the “RFI Measurement Protocol for Candidate SKA Sites” (hereafter RFI protocol). All data (raw and calibrated) are preserved in some suitable format, such as that set by the international RFI working group of the Site Evaluation and Selection Committee (SESC). An RFI test in December 2003 was performed according to Mode 1 of the RFI Protocol, in order to identify technical difficulties which might arise during a co-ordinated RFI measurement campaign over a period of 1 year. In this paper we describe the current equipment, observational technique and data presentation. The preliminary results demonstrate that the RFI situation at Dawodang depression in Guizhou province makes it quite a promising location for the proposed SKA. Furthermore, the first session of the RFI monitoring program, which was made in May 2004, showed that a complete RFI measurement including both modes 1 and 2 of the RFI Protocol would take about 2 weeks. The possible ways to minimize some limitations of the current equipment are also discussed, which will enable us to meet the RFI protocol.     

Seven-frequency VLBI Observations of the GHz-Peaked-Spectrum Source OQ 208

We present quasi-simultaneous VLBI images of the GHz-Peaked-Spectrum radio source OQ 208 obtained with the Very Long Baseline Array at 1.4,1.7,2.3,5.0,8.4,15.4GHz and the European VLBI Network at 6.7 GHz.The low frequency(1.4,1.7 and 2.3GHz)ob- servations reveal a weak and extended steep-spectrum component at about 30mas away at position angle-110°,which may be a remnant emission.The radio structure of OQ 208 con- sists of two mini-lobes at 5.0,6.7,8.4 and 15.4 GHz.Our spectral analysis further confirms that the southwest lobe undergoes free-free absorption and finds that the free-free absorption is stronger in the inner region.By fitting the 8.4 GHz images from 1994 to 2005,we obtain a separation speed of 0.031±0.006 mas yr~(-1)between the two mini-lobes.This indicates a jet proper motion of 0.105±0.020 c and a kinematic age of 219±42 yr for the radio source.     

行星磁场与卫星引力及其相对运动的统计关系

从知道某些天体具有磁场起，人们就对其磁场的起源提出种种解释，例如有电池说，转子说，化石说，发电机说等等。但由于这些学说都分别与某些观测事实相抵触而未被公认，因此星球磁场的起源一直是未能解决的命题。余先河先生提出，星球的磁场起源可能与所受的引力有关，行星的磁场强度正比于其所受卫星的引力；正比于卫星与行星的引力连线转动的相对角速度。本文对这两方面的命题分别进行了相关分析，得到其相关系数分别为：ｒ＝０．８４８１和ｒ＝０．８４２５，它们都在ａ＝０．０１的信度水平上相关。结果表明余新河关于行星磁场起源的设想是有基础的。本文还对其统计结果和可能机制进行了讨论。     

冕洞与太阳活动周及地磁活动的演化关系

本文用1970－1995年的冕洞资料，分析了冕洞的分布规律，磁场极性的演化特征和冕洞的地磁效应，以及它们与太阳黑子周期的演化关系，得到了一些有意义的结论。特别指出赤道冕洞和极区冕洞具有相反的演化规律和不同的特征。     

Investigation of the correlation between morphology and luminosity for two classes of main galaxies

Using an apparent-magnitude limited Main galaxy sample of the Sloan Digital Sky Survey Data Release 7(SDSS DR7), we investigate the correlation between morphologies and luminosity for the Main galaxy sample. Our Main galaxy sample is divided into two classes: Main galaxies only with TARGET_GALAXY flag (bestPrimtarget = 64), and ones also with other flags. It is found that for the second class Main galaxies, the early-type proportion monotonously increases with increasing luminosity nearly in the whole luminosity region. But for the first class Main galaxies, the early-type proportion increases with increasing luminosity only within a certain luminosity region (−22.2 < M _r  < −19.8). In the high luminosity region (M _r  < −22.2), the early-type proportion of the first class Main galaxies even decreases dramatically with increasing luminosity. We also analyze the correlation between morphologies and luminosity of galaxies around the peak of the redshift distribution ( 0.07 ≤ z ≤ 0.08 ). In such a narrow redshift region, we still observe strong correlation between morphologies and luminosity, which shows that this correlation is fundamental.     

应用Hydrolight模式研究含油水体辐射传输特性的关键技术

辐射传输模式Hydrolight在国际水色遥感研究领域已被广泛用于解决水体光学的各种问题,也是进行石油类污染水体辐射传输特性研究的有效模型。结合Hydrolight模式的机理、应用现状及含油水体的特点,提出了将该模式应用于光学特性复杂的石油污染水体辐射传输特性研究时需要解决的关键技术,包括测定石油污染水体吸收系数和散射系数、建立石油污染吸收和散射特性随波长和深度变化的参数化模型、确定油物质的吸附后悬浮颗粒物体散射函数模型等方面。依据2018年8月和2016年8月分别在辽宁大连港和辽宁盘锦辽河油田等区域测定的含油水体数据,讨论了这些关键技术的解决方案。     

海面溢油无人机高光谱遥感检测与厚度估算方法

海上溢油是海洋国家所面临的共同问题,但至今仍没有一种可靠实用的海上溢油准确识别和油量遥感监测方法。为此,本文以无人机高光谱遥感为手段,开展了海面溢油检测与厚度估算方法研究。实验中,通过搭建室外大型水槽溢油实验装置,获取了模拟真实海洋环境条件下不同溢油量的遥感和现场光谱数据,在此基础上,分析并提取了海上溢油特征光谱波段,给出了海上溢油高光谱检测模型;针对现场实验条件下水面油膜厚度难以测定的问题,设计了3种利用总体溢油量的油膜厚度估算模型。得到如下主要结论:（1）675 nm和699 nm是海上溢油检测的有效特征波段,但对极薄的油膜没有检测能力;（2）提出了归一化溢油指数模型、反比例模型和吸收基线模型等3种海上溢油油膜厚度估算模型,其中对于薄油膜（厚度≤ 5 μm）和厚油膜（厚度>50 μm）,反比例模型是溢油厚度反演的首选也是唯一选择。对于中厚度油膜,晴朗天气条件下,归一化溢油指数模型是油膜厚度反演的首选,同时反比例模型和溢油吸收基线模型也都有较好的反演能力,而在多云天气条件下,反比例模型效果最佳。     

印尼苏拉威西地区波尼盆地形成及其石油地质特征

波尼盆地是一个新生代裂谷盆地,勘探程度极低,其含油气系统及主要勘探层系不明。采用类比分析方法,通过对周边构造演化和沉积特征相似盆地的烃源岩、储层特征及含油气系统分析,进一步推测波尼盆地发育始新统潮坪-潟湖相烃源岩,品质较好,为Ⅱ—Ⅲ型干酪根,普遍处于成熟—高成熟阶段,以生油为主。该盆地共发育3套潜在储盖组合,最主要为中、上中新统—上新统Tacipi组生物礁储层及上新统区域性海相泥岩储盖组合,油气勘探前景较好。