东海水母类、浮游贝类及被囊类的垂直分布

有关水母类、浮游贝类及被囊类的垂直分布,迄今国内的报道还不多,只有陈清潮等(1978)在南海西沙、中沙群岛周围海域进行过一些调査工作。但国外早已开展这方面的工作,研究资料很多, Bigelow and Sear(1937), Leloup and Hentschel(1938),Totton(1954), Alvarino(1967),Pugh(1974)等对水母类都有较详细的报道;对浮游贝类和被囊类，Stubbing(1938), Tesch(1946), Thompson(1948), Swell(1953), Wormelle(1962)等也作了一些工作。 浮游动物的垂直分布是一个比较复杂的生态学问题,所涉及的因素很多(Bense,1964; Leloup and Hentschel,1938; Moore,Owre, Jones and Dow,1953)。本文仅就我们现有的材料进行初步分析。 本文系根据1978年5月27日-7月3日“金星”号在东经123°-129°,北纬26°30′一32°30′,水深大于80m的测站,用大型浮游生物网垂直分层采集(层次为0-50m,50-100m,100-250m,250-500m,500-1000m,1000-2000m)所获得的78份浮游生物样品,分析整理而成。     

太平洋西部3个岩芯沉积物的粒度组成及其天然湿容重和含水量的变化

本文讨论了太平洋西部3个岩芯孔的粒度组成、天然湿容重和含水量的变化。沉积物组成以粉砂和粘土细粒为主,砂粒含量很少,而且多为有孔虫介壳。容重与沉积物粒度呈正相关,含水量则呈负相关。当粒度组成不变时,容重随岩芯埋藏深度的增加而增大,而含水量则减少。     

江苏海岸中部近岸冬季潮汐和潮流特征

南黄海西侧的江苏海岸近岸区域,素以地形复杂、潮流强劲、悬沙输运剧烈著称,但是较长期的同步潮位和潮流观测数据仍然缺乏,尤其是在近岸(20 km)浅水(20 m)区域。2014年1月在大丰港附近开展了连续潮位和潮流观测,获得的数据揭示了一系列特征。此地潮汐潮流为正规半日潮,浅水分潮显著。平均潮差为3.05 m,最显著的两个分潮为M2和S2分潮,振幅分别为1.45 m和0.52 m。潮流最显著的半日分潮M2分潮和最显著的浅水分潮M4分潮在沿岸方向上振幅分别为0.84m/s和0.12m/s,在跨岸方向上振幅分别为0.24 m/s和0.01 m/s,沿岸方向占绝对优势。潮波的沿岸传播介于前进波和驻波之间,驻波的特征稍强。M2分潮潮流椭圆最大流(长轴)方向为南偏东7.4°。存在冬季沿岸向北的余流,垂向平均值的大小为2.2 cm/s。以上潮汐潮流特征为该区域海洋物质输运研究提供了基础资料。     

山东沂沭河流域2000BC前后古文化兴衰的环境考古

Neolithic culture series in the Yishu River Basin developed in the order of Beixin culture-Dawenkou culture-Longshan culture-Yueshi culture. During the early and middle stage of Longshan culture （4600-4300 cal. yr BP）, the climate in the Yishu River Basin was warm and wet. Paddy-oriented agriculture planted paddy was very developed. The society was flourishing with great amount of archaeological sites. The cooling starting in 4200 cal. yr BP made the paddies shortfall in output or even no seeds were gathered. This situation intensified the discrepancy between population and resource. The scarcity in natural resource led to substantial decrease in population and subsequent drop in archaeological sites. About 4000 cal. yr BP Longshan culture was displaced by Yueshi culture which was relatively un- derdeveloped, simple and unsophisticated.     

Searching for r-process-enhanced stars in the LAMOST surveyⅠ:the method

The abundance patterns of r-process-enhanced stars contain key information required to constrain the astrophysical site(s)of r-process nucleosynthesis,and to deepen our understanding of the chemical evolution of our Galaxy.To expand the sample of known r-process-enhanced stars,we have developed a method to search for candidates in the LAMOST medium-resolution(R7500)spectroscopic survey by matching the observed spectra to synthetic templates around the EuⅡline at 6645.1 A.We obtain a sample of 13 metal-poor(-2.35<[Fe/H]<-0.91)candidates from 12209 unique stars with 32774 mediumresolution spectra.These candidates will be further studied by high-resolution follow-up observations in the near future.We describe some extensions of this effort to include larger samples of stars,in particular at lower metallicity,using the strength of the BaⅡline at 6496.9 A.     

四川及邻区地震动衰减关系

根据地震构造环境和震害分布特点, 将四川及邻区划分为西南地区和四川盆地地区. 收集了西南地区96次、 四川盆地地区40次近代破坏性地震资料, 并对各次地震的震级参数进行了统一校核. 按照该地区震中烈度与震级、 有感半径与震级的统计关系, 对地震烈度衰减进行了近场与远场特征控制, 建立了地震烈度沿长轴、 短轴和平均轴的衰减关系. 统一了中国与美国面波震级的震级标度, 利用最新得出的美国西部基岩水平向地震加速度反应谱衰减关系, 采用考虑地震加速度的近场距离饱和与震级饱和特征的衰减模型, 转换得到了该地区的基岩水平向地震加速度反应谱衰减关系.      

An on Orbit Determination of Point Spread Functions for the <Emphasis Type="Italic">Interface Region Imaging Spectrograph</Emphasis>

Using the 2016 Mercury transit of the Sun, we characterize on orbit spatial point spread functions (PSFs) for the Near- (NUV) and Far- (FUV) Ultra-Violet spectrograph channels of NASA’s Interface Region Imaging Spectrograph (IRIS). A semi-blind Richardson–Lucy deconvolution method is used to estimate PSFs for each channel. Corresponding estimates of Modulation Transfer Functions (MTFs) indicate resolution of 2.47 cycles/arcsec in the NUV channel near 2796 Å and 2.55 cycles/arcsec near 2814 Å. In the short (\({\approx}\,1336~\mathring{\mathrm{A}}\)) and long (\({\approx}\,1394~\mathring{\mathrm{A}}\)) wavelength FUV channels, our MTFs show pixel-limited resolution (3.0 cycles/arcsec). The PSF estimates perform well under deconvolution, removing or significantly reducing instrument artifacts in the Mercury transit spectra. The usefulness of the PSFs is demonstrated in a case study of an isolated explosive event. PSF estimates and deconvolution routines are provided through a SolarSoft module.     

A space-based decametric wavelength radio telescope concept

This paper reports a design study for a space-based decametric wavelength telescope. While not a new concept, this design study focused on many of the operational aspects that would be required for an actual mission. This design optimized the number of spacecraft to insure good visibility of approx. 80% of the radio galaxies– the primary science target for the mission. A 5,000 km lunar orbit was selected to guarantee minimal gravitational perturbations from Earth and lower radio interference. Optimal schemes for data downlink, spacecraft ranging, and power consumption were identified. An optimal mission duration of 1 year was chosen based on science goals, payload complexity, and other factors. Finally, preliminary simulations showing image reconstruction were conducted to confirm viability of the mission. This work is intended to show the viability and science benefits of conducting multi-spacecraft networked radio astronomy missions in the next few years.     

The astrometric signal of microlensing events caused by free floating planets

Astrometric observations of microlensing events can be used to obtain important information about lenses. During these events, the shift of the position of the multiple image centroid with respect to the source star location can be measured. This effect, which is expected to occur on scales from micro-arcseconds to milli-arcseconds, depends on the lens-source-observer system physical parameters. Here, we consider the astrometric and photometric observations by space and ground-based telescopes of microlensing events towards the Galactic bulge caused by free floating planets (FFPs). We show that the efficiency of astrometric signal on photometrically detected microlensing events tends to increase for higher FFP masses in our Galaxy. In addition, we estimate that during five years of the Gaia observations, about a dozen of microlensing events caused by FFPs are expected to be detectable.     

基于稳定同位素技术的光背团水虱食性分析

为了探究光背团水虱的食性特征,本研究利用碳、氮稳定同位素技术于2015年冬季和2016年夏季对广西北海廉州湾红树林中光背团水虱及其食物来源的碳、氮稳定同位素比值（δ13C值和δ15N值）进行分析。结果显示,冬季和夏季光背团水虱的δ13C值大小范围为-22.85‰~-21.87‰,平均值为（-22.46±0.35）‰;δ15N值大小范围为11.02‰~12.85‰,平均值为（11.88±0.56）‰;光背团水虱的δ13C值、δ15N值变化范围较小,表明其食物来源较为简单。单因素方差分析结果显示,冬季与夏季光背团水虱的平均δ13C值差异不显著（P>0.05）,而夏季的δ15N值普遍高于冬季δ15N值,差异显著（P<0.05）;不同生长阶段的光背团水虱δ13C值、δ15N值会随着体长的增长而增大,差异显著（P<0.05）,表明光背团水虱在生长的过程中可能发生了食性转变。光背团水虱的δ13C值与浮游生物的δ13C值相近,而与红树植物δ13C值差距较远,说明光背团水虱主要以浮游生物为食物来源。基于R语言稳定同位素混合模型（SIAR）计算结果显示,冬季和夏季各粒径级别浮游生物对不同生长阶段的光背团水虱的贡献率趋势基本一致,表现为1.2~25 μm粒级的浮游生物对光背团水虱平均贡献率最高,其次为25~50 μm粒级,粒径大于100 μm的浮游生物对体长小于5.5 mm的光背团水虱贡献率较低,对体长大于5.5 mm的光背团水虱的贡献率随着体长增大而相应增大,说明不同生长阶段的光背团水虱食性有差异。对光背团水虱食性分析的结果可为深入研究团水虱爆发的原因及危害红树林的作用机理提供基础资料。