南海北部表层沉积物中锆元素的地球化学初步研究

本文通过对南海北部表层沉积物中锆的分布特点和迁移方式的研究,探讨南海北部锆石砂矿的形成过程和富集规律,及锆的地球化学分布与古海岸线的相互关系。 研究区的范围,东起台湾浅滩,西至雷州半岛东岸及海南岛东南沿岸的陆架、陆坡区(110°—120°E)及东沙群岛以南部分海域(17°50′N以北)。样品多数采自大陆架和陆坡区,少数采自海盆,最大的采样深度达3800m。全区共选出115个表层沉积物样品,进行了X光、萤光光谱分析、化学分析、矿物显微镜下鉴定等。     

西沙礁序列的磁性地层学研究

利用西沙群岛西琛一井３３０ｍ以上井段的１４９块岩心标本，用美国２－Ｇ型超导磁力仪进行了古地磁测定，获得了一个从更新世至中新世晚期包括布容，松山，高斯和吉尔伯特四个极性时及若干亚极性的磁性地层柱，为礁序列的划分对比，提供了新的依据。     

福建红树林上钻孔动物的生态

福建红树林上的钻孔动物共发现了５种，其中软体动物的龙骨节铠船蛆Ｂａｎｋｉａ ｃａｒｉｎａｔａ、裂铠船蛆Ｔｅｒｅｄｏ ｍａｎｎｉ和甲壳动物的光背团水虱Ｓｐｈａｅｒｏｍａ ｒｅｔｒｏｌａｅｖｉｓ是破坏红树林的主要的钻孔动物。钻孔动物钻凿红树茎的基部和裸露的根部，垂直分布受潮汐水位制约，在红树林区的纵深分布与水流畅通程度有关。     

等离子体技术及其在地质上的应用

激光烧蚀微探针等离子体质谱的地质应用。自1989年以来，我们实验室就积极开展了激光烧蚀微探针(LAM)试样引入系统的研究工作，这种技术适合于ICP—MS分析地质样品中小体积矿物(激光烧蚀孔穴直径低于10—100μm)．对某些样品．采用Nd：YAG激光的基本IR波长(1064nm)，作为多数用途，4倍频率(uv)的波长(266nm)能产生较小的直径，并较好地形成孔穴．     

秋茄和榕树叶片中正构烷烃分布和单体化合物δ13C值及其光合作用

对深圳福田、阳江、海南新竹红树林秋茄Kandelia candel及海口榕树Ficusm icrocarpa叶中类脂物进行萃取,分离出正构烷烃,通过气相色谱(GC)及色谱-质谱(GC MS)分析,测出了正构烷烃的碳数分布和相对含量.气相色谱-稳定同位素比质谱仪(GC-IRMS)测定了正构烷烃单体化合物的稳定同位素组成δ13C.秋茄叶和榕树叶正构烷烃的碳数分布均为C17C33,主要集中在C23-C31(＞90%).化合物含量最高为C27的有深圳福田秋茄、海南新竹秋茄、海口榕树,而阳江秋茄为C25.单体化合物的稳定同位素δ13C深圳福田秋茄为-31.42‰-34.48‰,阳江秋茄为-31.69‰-33.62‰,海南新竹秋茄为-30.30‰-33.04‰,海口榕树为-29.92‰33.56‰;平均值分别为-32.95‰、32.67‰、31.67‰、-31.74‰.结果表明,秋茄和陆地植物榕树的光合作用都是通过C3途径,是典型C3植物.     

风应力涡度和边界力对东中国海环流的效应

多年来，很多国内外学者对东中国海环流的机理进行了研究。近几年，奚盘根等(1980)和冯士筰等(1981)基于f-坐标系的风涡度一热盐梯度全流方程分别数值地模拟了冬、夏季东中国海环流。他们指出，控制东中国海环流主要因子是边界力(黑潮)、热盐力和底形分布。袁耀初等(1982)也数值地模拟了东中国海环流结构，     

温度,光周期和换水率对黑鲷卵,鱼苗的影响

黑鲷商业化生产在某些国家已是一项重要的水产养殖行业。众所周知,温度是影响海水鱼苗卵黄囊时期的决定性因素之一,并且在营养生命开始时,它决定着鱼苗的生物特性。Tandler和Mason(1983年)发现:黑鲷鱼苗在孵化后最初12天的存活率,在连续光照下培养比12小时光周期有了明显地改善。还发现:光照强度在205～1370勒克斯之间对这种鱼的存活和体长生长有积极的作用。而且黑鲷鱼苗     

Shock chemistry in the molecular clouds associated with SNR IC 443

Several interstellar molecules have been detected toward the highly perturbed B and G clouds associated with the supernova remnant IC 443 via their 3 mm transitions, including N2H+, SiO, SO, CN, HNC, and H13CO+. The (J, K) = (1, 1) and (2, 2) inversion lines of metastable ammonia have also been observed, as well as the J = 3-2 transition of HCO+ at 1.2 mm. Analysis of the (1, 1) and (2, 2) inversion lines of NH3 indicates minimum gas kinetic temperatures of TK = 70 K toward cloud B, and TK = 33 K in cloud G. Modeling of the J = 1-0 and J = 3-2 transitions of HCO+ implies densities greater than 10(5) cm-3 toward both positions. These data clearly show that hot and dense material is present in IC 443, and they suggest the presence of shocks in both regions. A careful analysis of the HCO+ lines indicates that the HCO+ abundance is at most enhanced by factors of a few over that found in cold, quiescent gas. This conclusion contradicts past claims of HCO+ abundance enhancements of several orders of magnitude in the perturbed regions. The N2H+ abundance was also found to be similar to that in cold gas, suggesting that there is no increase in ionization in the clouds. The abundances of SO and CS, as well as CN and NH3, do not appear to differ significantly from those found in cold dark clouds, although chemistry models predict sulfur-containing species to undergo high-temperature enhancements. SiO, however, is found to have an abundance in the perturbed gas 100 times larger than the upper limits observed in the dark cloud TMC 1, a result in agreement with high temperature chemistry models. In addition, the HNC/HCN ratio in both IC 443 B and G was found to be approximately 0.1--far from the ratio of 1 predicted by low-temperature ion-molecule chemistry, but similar to the values observed in clouds where elevated temperatures are present.