南海海域红斑后海螯虾(Metanephrops thomsoni)的分子识别与群体遗传分化     

范艳波  王中铎  郭昱嵩  颜云榕  刘楚吾 《海洋与湖沼》2013,44(1):220-225

利用16S rRNA基因序列分子识别红斑后海螯虾,然后对海南附近海域(18°30′-19°00′N,111 °30′-112°30′ E)、北部湾口海域(15°41′ N,110°40′ E)和南沙群岛海域(5°20′-5°29′N,110°09′-111°26′E)三个地理群体进行ITS1的扩增测序.16S rRNA基因序列的结果表明所取样本准确;三个地理群体分别得到616-623bp、619bp和614bp的ITS1全长序列,A、G、T、C含量平均分别为22.3％、29.4％、17.8％和30.6％;其中562个保守位点,39个多态位点.ML和NJ聚类分析显示三个地理群体共聚为三个大支,其中海南群体有群体分化.表明红斑后海螯虾三个地理群体分化极其显著,且海南群体具有相对高的遗传多样性.  相似文献   

重金属Cu、Pb对泥鳅(Misgurnus anguillicaudatus)卵细胞凋亡及DNA损伤的SCGE试验     

唐建勋  程樟顺  郑荣泉  陶晓敏  刘忠良  赵华 《海洋与湖沼》2013,44(1):177-181

采用室内暴露试验方法,以单细胞凝胶电泳技术(SCGE)检测,研究了Cu、Pb不同浓度梯度与不同暴露时间联合染毒对泥鳅卵细胞DNA的损伤.结果表明,各Cu、Pb浓度组DNA平均迁移长度增加,与阴性对照组比较差异有显著性(P＜0.05).此外,随着Cu、Pb染毒剂量的增加,各试验组DNA的平均迁移长度逐渐增加,在试验浓度梯度范围内(Cu 0.01mg/L+Pb 0.05mg/L、Cu 0.10mg/L+Pb 0.50mg/L、Cu 0.25mg/L+Pb 0.75mg/L),存在较为显著的剂量-效应关系(P＜0.05),但未见明显的时间-效应关系(P＞0.05).Cu、Pb可引起泥鳅卵细胞凋亡和DNA损伤,卵细胞的不同损伤水平可望作为较为理想的水环境基因毒性指标.  相似文献   

长江河口盐水入侵对大通枯季径流量变化的响应时间   总被引：4，自引：3，他引：1  

侯成程  朱建荣 《海洋学报》2013,35(4):29-35

应用河口海岸三维数值模式, 计算区域包括大通至长江河口及其邻近海域, 设计高分辨率网格, 数值模拟和分析不同潮型下长江河口盐水入侵对大通径流量变化的响应时间。计算结果表明, 不同潮型期间大通径流量的增加, 河口盐度响应的时间在4.0～6.2 d之间, 但小潮期的响应时间明显长于其他潮型期的响应时间。本文给出了长江河口盐水入侵对大通枯季径流量变化的响应时间, 可为河口水文、泥沙和环境等研究中取何时径流量提供了依据。  相似文献   

虹鳟(Oncorhynchus mykiss)选育群体的血清类固醇激素周年变化     

谷伟  徐革锋  户国  张永泉  王炳谦 《海洋与湖沼》2013,44(3):697-701

采用放射性免疫(RIA)和组织学切片技术,系统地研究了虹鳟(Oncorhynchus mykiss)选育群体的血清性类固醇激素周年变化与性腺发育特点的关系,以及血清中性类固醇激素雌二醇(E2)和睾酮(T)在雌雄亲本中的周年变化规律和生理作用。结果表明,虹鳟性腺发育可划分为6期。雌鱼血清中E2在10月(V期性腺)达到峰值,T浓度在11月达到峰值,而进入繁殖期后(11—12月)E2开始下降。雄鱼血清T浓度在11月达到最大值,E2在6月份达到峰值,在11月之后T开始下降。在各月份,雌鱼E2浓度水平远高于雄鱼,而雄鱼T浓度个别月份低于雌鱼。这些研究揭示出,测定血清性类固醇激素浓度水平可用于准确判断鱼类的生殖状态,且可为虹鳟家系选育出早熟亲本群体提供重要技术依据。  相似文献   

Towards an operational use of space imagery for oil pollution monitoring in the Mediterranean basin: a demonstration in the Adriatic Sea     

Ferraro G  Bernardini A  David M  Meyer-Roux S  Muellenhoff O  Perkovic M  Tarchi D  Topouzelis K 《Marine pollution bulletin》2007,54(4):403-422

Studies of operational pollution carried out by European commission - Joint Research Centre in the Mediterranean Sea for the years 1999-2004 are briefly introduced. The specific analysis of the Adriatic Sea for the same period demonstrates that this area has been characterized by a relevant number of illegal discharges from ships. After setting the historical background of the project AESOP (aerial and satellite surveillance of operational pollution in the Adriatic Sea), the content, partners and aim of the project are presented. Finally, the results of the first phase of the AESOP project are presented. The results seem very encouraging. For the first time in the Adriatic, real time detection of oil spills in satellite images and an immediate verification by the Coast Guard has been undertaken. An exploratory activity has also been carried out in collaboration with the University of Ljubljana to use automatic information system (AIS) to identify the ships detected in the satellite images.  相似文献   

Chemical contamination of a coral reef by the grounding of a cruise ship in Bermuda   总被引：1，自引：0，他引：1  

Jones RJ 《Marine pollution bulletin》2007,54(7):905-911

Bulk metal analyses of surficial sediments collected around the Norwegian Crown cruise ship grounding site in Bermuda indicated significant but localized contamination of reef sediments by copper and zinc, caused by the stripping of the tri-butyltin (TBT)-free antifouling (AF) paint (Intersmooth 460) from the underside of the hull. Highest copper and zinc values were found in heavily compacted and red-pigmented sediments inside the impact scar and were comparable to levels found close to slip ways of local boat yards where AF paints from hull stripping and cleaning processes are washed into the sea. The re-distribution of AF contaminated sediments by storms and deposition on nearby reefs constitutes a significant ecological risk that could delay recovery processes and reduce the effectiveness of remediation efforts. Whilst the ecotoxicological effects of AF paint particles interspersed with sediment is unknown, and in need of further study, it is argued that the significance of AF paint contamination of grounding sites has been overlooked.  相似文献   

High outflow channels on Mars indicate Hesperian recharge at low latitudes and the presence of Canyon Lakes     

Neil M. Coleman  Cynthia L. Dinwiddie 《Icarus》2007,189(2):344-361

A number of martian outflow channels were carved by discharges from large dilational fault zones. These channels were sourced by groundwater, not surface water, and when observed on high-standing plateaus they provide indicators of elevated paleo-groundwater levels. We identify three outflow channels of Hesperian age that issued from a 750-km-long fault zone extending from Candor Chasma to Ganges Chasma. Two of these channels, Allegheny Vallis and Walla Walla Vallis, have sources >2500 m above the topographic datum, too high to be explained by discharge from a global aquifer that was recharged solely in the south polar region. The indicated groundwater levels likely required regional sources of recharge at low latitudes. The floodwaters that erupted from Ophir Cavus to form Allegheny Vallis encountered two ridges that restricted the flow, forming temporary lakes. The flow probably breached or overtopped these obstructions quickly, catastrophically draining the lakes and carving several scablands. After the last obstacle had been breached, a single main channel formed that captured all subsequent flow. We performed hydrologic analyses of this intermediate phase of the flooding, prior to incision of the channel to its present depth. Using floodwater depths of 30-60 m, we calculated flow velocities of 6-15 m s⁻¹ and discharges in the range of . Locally higher flow velocities and discharges likely occurred when the transient lakes were drained. Variable erosion at the channel and scabland crossing of MOLA pass 10644 suggests that the upper 25-30 m may consist of poorly consolidated surface materials underlain by more cohesive bedrock. We infer that an ice-covered lake with a surface elevation >2500 m probably existed in eastern Candor Chasma because this canyon is intersected by the Ophir Catenae fault system from which Allegheny Vallis and Walla Walla Vallis originated. We introduce a new hydrology concept for Mars in which the groundwater system was augmented by recharge from canyon lakes that were formed when water was released by catastrophic melting of former ice sheets in Tharsis by effusions of flood basalts. This model could help to reconcile the expected presence of a thick cryosphere during the Hesperian with the abundant evidence for groundwater as a source for some of the circum-Chryse outflow channels.  相似文献   

HST observations of azimuthal asymmetry in Saturn's rings     

Richard G. French  Heikki Salo  Luke Dones 《Icarus》2007,189(2):493-522

From 378 Hubble Space Telescope WFPC2 images obtained between 1996-2004, we have measured the detailed nature of azimuthal brightness variations in Saturn's rings. The extensive geometric coverage, high spatial resolution (), and photometric precision of the UBVRI images have enabled us to determine the dependence of the asymmetry amplitude and longitude of minimum brightness on orbital radius, ring elevation, wavelength, solar phase angle, and solar longitude. We explore a suite of dynamical models of self-gravity wakes for two particle size distributions: a single size and a power law distribution spanning a decade in particle radius. From these N-body simulations, we calculate the resultant wake-driven brightness asymmetry for any given illumination and viewing geometry. The models reproduce many of the observed properties of the asymmetry, including the shape and location of the brightness minimum and the trends with ring elevation and solar longitude. They also account for the “tilt effect” in the A and B rings: the change in mean ring brightness with effective ring opening angle, |Beff|. The predicted asymmetry depends sensitively on dynamical ring particle properties such as the coefficient of restitution and internal mass density, and relatively weakly on photometric parameters such as albedo and scattering phase function. The asymmetry is strongest in the A ring, reaching a maximum amplitude A∼25% near a=128,000 km. Here, the observations are well-matched by an internal particle density near 450 kg m⁻³ and a narrow particle size distribution. The B ring shows significant asymmetry (∼5%) in regions of relatively low optical depth (τ∼0.7). In the middle and outer B ring, where τ?1, the asymmetry is much weaker (∼1%), and in the C ring, A<0.5%. The asymmetry diminishes near opposition and at shorter wavelengths, where the albedo of the ring particles is lower and multiple-scattering effects are diminished. The asymmetry amplitude varies strongly with ring elevation angle, reaching a peak near |Beff|=10° in the A ring and at |Beff|=15-20° in the B ring. These trends provide an estimate of the thickness of the self-gravity wakes responsible for the asymmetry. Local radial variations in the amplitude of the asymmetry within both the A and B rings are probably caused by regional differences in the particle size distribution.  相似文献   

Saturn eddy momentum fluxes and convection: First estimates from Cassini images     

Anthony D. Del Genio  John M. Barbara  Andrew P. Ingersoll  Ashwin R. Vasavada  Carolyn C. Porco 《Icarus》2007,189(2):479-492

We apply an automated cloud feature tracking algorithm to estimate eddy momentum fluxes in Saturn's southern hemisphere from Cassini Imaging Science Subsystem near-infrared continuum image sequences. Voyager Saturn manually tracked images had suggested no conversion of eddy to mean flow kinetic energy, but this was based on a small sample of <1000 wind vectors. The automated procedure we use for the Cassini data produces an order of magnitude more usable wind vectors with relatively unbiased sampling. Automated tracking is successful in and around the westward jet latitudes on Saturn but not in the vicinity of most eastward jets, where the linearity and non-discrete nature of cloud features produces ambiguous results. For the regions we are able to track, we find peak eddy fluxes and a clear positive correlation between eddy momentum fluxes and meridional shear of the mean zonal wind, implying that eddies supply momentum to eastward jets and remove momentum from westward jets at a rate . The behavior we observe is similar to that seen on Jupiter, though with smaller eddy-mean kinetic energy conversion rates per unit mass of atmosphere (). We also use the appearance and rapid evolution of small bright features at continuum wavelengths, in combination with evidence from weak methane band images where possible, to diagnose the occurrence of moist convective storms on Saturn. Areal expansion rates imply updraft speeds of over the convective anvil cloud area. As on Jupiter, convection preferentially occurs in cyclonic shear regions on Saturn, but unlike Jupiter, convection is also observed in eastward jet regions. With one possible exception, the large eddy fluxes seen in the cyclonic shear latitudes do not seem to be associated with convective events.  相似文献   

Arecibo radar observations of Phobos and Deimos     

Michael W. Busch  Steven J. Ostro  Jon D. Giorgini  Ellen S. Howell  Alice A. Hine  Irwin I. Shapiro 《Icarus》2007,186(2):581-584

In November 2005, we observed the moons of Mars using the Arecibo 2380-MHz (13-cm) radar, obtaining a result for the OC radar albedo of Phobos (0.056±0.014) consistent with its previously reported radar albedo and implying an upper bound on its near-surface bulk density of . We detected Deimos by radar for the first time, finding its OC radar albedo to be 0.021±0.006, implying an upper bound on its near-surface density of , consistent with a high-porosity regolith. We briefly discuss reasons for these low radar albedos, Deimos' being possibly the lowest of any Solar System body yet observed by radar.  相似文献