塔中地区志留系碎屑锆石测年及其地质意义

志留系是塔里木盆地第一套砂岩储层广泛分布的沉积盖层,其沉积来源与成因对志留纪构造演化及周边造山带的研究具有重要意义。塔中地区3个志留系样品的碎屑锆石LA?ICP?MS U?Pb定年研究表明,志留系具有比较集中的二期物源年龄：南华纪中期、古元古代中期。碎屑锆石测定的年龄表明塔中志留系物源均来自前寒武纪,塔中东部源区方向的塔南隆起基底在奥陶纪已隆升成为蚀源区。大量的新元古代中期锆石年龄表明塔里木板块在新元古代时期可能与Rodinia超大陆具有相似的聚合与裂解演化史。     

The Late Jurassic ray Kimmerobatis etchesi gen. et sp. nov. and the Jurassic radiation of the Batoidea

The laminated marine mudstones of the Late Jurassic of Kimmeridge, southern England, yield two exceptionally well-preserved partial skeletons of a previously unrecognised species of early batoid. These are described as a new genus and species, Kimmerobatis etchesi gen. et sp. nov. which has a general “guitarfish” bauplan as in all other batoids known from the Jurassic. This species possesses a combination of primitive characters such as centra present within the majority of the synarcual and antorbital cartilages that fail to reach the pectoral skeleton along with more derived characters, such as the lack of fin spines. Until now, little study has been carried out on the affinities of Jurassic batoids, despite their key role in understanding batoid evolution. Results from parsimony and likelihood phylogenetic reconstruction indicates that the whole-bodied Jurassic batoids Spathobatis, Belemnobatis, and Kimmerobatis gen. nov. form their own clade, Spathobatidae, and do not lend support to a monophyletic “Rhinobatidae”. Among Jurassic batoids, Kimmerobatis gen. nov. is most derived, but with derived characters being independently acquired compared to modern batoids (e.g. presence of a postpelvic process). The inclusion of whole bodied Jurassic fossils have generated a more resolved hypothesis of batoid evolution throughout the Cretaceous and into the Cenozoic.     

歧口凹陷歧北斜坡白云岩演化规律研究

在古近系沙河街组沙一段沉积期,为歧口凹陷最大湖扩期,在西南部整体古地理为宽缓的湖湾环境,气候潮湿温暖,物源供给较弱,在这种条件下,该地区发育大面积的碳酸盐岩沉积,以白云岩夹油页岩互层分布为特征。利用歧北斜坡两口重点井的岩心资料,对该区内的白云岩演化特征进行分析。研究表明,湖平面的升降决定了古地理环境,直接影响了白云岩发育的类型。歧北高斜坡区,水体较中斜坡浅,自下而上发育生屑灰岩、微晶云岩、灰质云岩、云质灰岩,表明古地理环境由粒屑滩—局限洼地—湖湾的演化过程;而在歧北中斜坡区,位于港西凸起周缘,早期主要为浅滩环境,发育灰质云岩和云质灰岩,向上过渡为微晶云岩、泥质云岩、泥岩,湖平面的多次升降,决定了该区古地理环境由浅滩—局限洼地—湖湾—半深湖的演化过程。通过地质钻探,该区在部分区域的白云岩已发现油层,证明该区白云岩储集层具有良好油气潜力,白云岩储集层已成为歧口凹陷古近系非常规油气增储的重要领域之一。     

雷暴单体合并进行中雷达回波参数演变及闪电活动的特征分析

雷暴单体合并是促使对流系统成长、增强、持久的重要因素,合并与灾害性天气有着密切的关系。针对23次合并样本（其中有闪电活动的样本10例）,利用多普勒雷达和Safir3000闪电定位系统的探测数据,基于雷达回波参数的构建与计算,分别以一次冰雹暴雨过程和一次强降水过程为例,对合并及雷暴系统的演变进行了物理过程分析,对所有样本特征进行了统计归纳。最后发现并验证了雷达回波参数F_V40up-6（即6 km以上对流单体大于40 dBz体积的变率）常常在合并进行中出现突然减小现象,简称为"突降";同时揭示了合并进行中闪电活动的特征。具体结论如下:（1）就合并最初开始位置而言,高度在5 km之下的样本最多,比例达86%。从合并用时看（即RHI图中30 dBz回波开始衔接至最强回波合为一体为止）,全都在6-36 min,其中用时在12 min以内的占56.5%;达到30 min的仅占16%。合并开始后,在97%的样本中,回波参数V₄₀（即大于40 dBz的总体积）、V_40up-6（即6 km以上大于40 dBz的总体积）出现增大;V₄₀增幅为7%-590%,V_40up-6增幅为3%-638%;V_40up-6最大值出现时刻距合并开始时刻12-18 min的,占总样本的60.1%;24-36 min的,占总样本的34.8%。（2）在雷暴单体合并进行中有"突降"现象的,占总样本的87%;其中又有77%的"突降"出现在距合并开始后的6-18 min内。（3）在10个闪电活动样本中,有9个样本在合并开始后,闪电频数出现了"跃增",甚至出现峰值;全部样本中参与放电的主正电荷区高度随着"突降"均有下降,降幅在1-4 km,而此时的闪电频数几乎没有变化。      

赣杭构造带中生代红色碎屑沉积盆地的形成和演化

本文是在继讨论赣杭构造带中生代火山盆地的形成和演化之后,再对赣杭构造带中生代红色碎屑沉积盆地（简称赣杭带红盆）的形成和演化作一探讨。涉及的内容主要有：赣杭构造带中生代红盆结构及演化时代;从晚侏罗世末到整个白垩纪各期主要构造运动及与红盆演化的关系;箕状盆地的几个主要特征;红盆演化的动力学背景;红盆所对应的深部构造以及深断裂活动和盆地演化的实际含义等     

巢湖形成演变与现代沉积作用

通过地质调查, 钻孔样品分析及历史资料对比, 得出:1.巢湖位于在中新生代形成的巢湖断陷盆地南部, 形成于更新世发育的河谷平原上, 由于全新世受气候及相应海平面变化和长江河道演变等三者共同影响而积水成湖。成湖历史大约2000年左右, 属河成型浅水湖。2.湖底沉积物平均中值粒径5-6ф, 并形成有三角洲沉积, 开阔湖沉积等五种沉积类型, 东、西、中三湖区的沉积物中分別为0.21, 0.37, 0.14cm/a, 全湖年淤积总量为93×l0⁴t/a。3.湖泊污染加重起始于70年代, 磷除来自外源外, 内负荷引起的释放量达220.56t/a, 这对巢湖富营养化亦有着重要的影响。     

江西相山酸性火山-侵入杂岩精确年代学与演化序列研究

相山火山盆地主体岩石为一套由熔结凝灰岩、流纹英安岩、流纹英安斑岩、碎斑熔岩、粗斑花岗斑岩及似斑状花岗岩组成的酸性火山-侵入杂岩体, 构成了两个完整的喷发-溢流(侵出)-侵入的岩浆活动亚旋回。本文在野外地质调查的基础上, 采用SIMS、LA-ICP-MS技术对主要岩类进行了高精度的锆石U-Pb年代学研究, 并建立了火山-侵入杂岩体的演化序列。结果表明, 打鼓顶组熔结凝灰岩代表了相山火山-侵入活动的最早期产物, 其锆石U-Pb年龄为140.7±2.7 Ma、140.1±1.8 Ma和138.2±1.6 Ma, 第一亚旋回主体流纹英安岩的锆石U-Pb年龄135.0±1.8 Ma。鹅湖岭组熔结凝灰岩代表了火山-侵入活动的第二亚旋回的开始, 其U-Pb年龄为135.6±1.2 Ma, 第二亚旋回主体碎斑熔岩的锆石U-Pb年龄133.6±1.3 Ma, 沙洲单元的粗斑花岗斑岩和似斑状花岗岩属于该亚旋回最晚期的侵入岩, 其锆石U-Pb年龄代表了相山火山-侵入活动的结束时间(分别为133.4±1.2 Ma和133.9±1.1 Ma)。相山早白垩世火山-侵入活动延续时间较短, 整体上呈现一个连续的过程, 初始时间在141 Ma附近, 结束时间在132 Ma左右。概言之, 第一亚旋回(141~135 Ma)以形成熔结凝灰岩、流纹英安岩和流纹英安斑岩为主, 第二亚旋回(135~132 Ma)以熔结凝灰岩、碎斑熔岩、粗斑花岗斑岩和似斑状花岗岩为主。岩石地球化学和野外地质特征也与两个亚旋回火山-侵入岩浆活动相吻合。     

我国海洋经济劳动生产率区域差异与演变分析

劳动生产率差异是导致区域经济发展差异的重要原因,提高劳动生产率是促进经济增长的有效手段。分析我国海洋经济的劳动生产率的区域差异与演变对发展我国海洋经济具有积极意义。在分析我国海洋经济劳动生产率的特点基础上,文章运用基尼系数和泰尔指数计算我国沿海地区1997—2014年海洋经济劳动生产率区域差异,并进行σ-收敛性检验,结果表明区域差异呈现倒V字形走势,1997—2005年呈现σ-发散,2005—2014年呈现σ-收敛。采用泰尔指数分解方法测度表明,环渤海、长三角、泛珠三角三大经济区海洋经济劳动生产率地区内差异占总体差异的比重达80%以上,而地区间差异比重较小,环渤海经济区地区内差异最大。分阶段对我国各沿海地区海洋经济的劳动生产率进行排名并观察演变过程。提出提高我国海洋经济劳动生产率的相关建议:一是努力提高海洋经济全要素生产率;二是促进海洋产业合理布局,努力提高传统海洋产业劳动生产率;三是统筹区域海洋经济发展。     

Changes in Jupiter’s zonal velocity between 1979 and 2008

We show that the peak velocity of Jupiter’s visible-cloud-level zonal winds near 24°N (planetographic) increased from 2000 to 2008. This increase was the only change in the zonal velocity from 2000 to 2008 for latitudes between ±70° that was statistically significant and not obviously associated with visible weather. We present the first automated retrieval of fast (∼130 m s⁻¹) zonal velocities at 8°N planetographic latitude, and show that some previous retrievals incorrectly found slower zonal winds because the eastward drift of the dark projections (associated with 5-μm hot spots) “fooled” the retrieval algorithms.We determined the zonal velocity in 2000 from Cassini images from NASA’s Planetary Data System using a global method similar to previous longitude-shifting correlation methods used by others, and a new local method based on the longitudinal average of the two-dimensional velocity field. We obtained global velocities from images acquired in May 2008 with the Wide Field Planetary Camera 2 (WFPC2) on the Hubble Space Telescope (HST). Longer-term variability of the zonal winds is based on comparisons with published velocities based on 1979 Voyager 2 and 1995-1998 HST images. Fluctuations in the zonal wind speeds on the order of 10 m s⁻¹ on timescales ranging from weeks to months were found in the 1979 Voyager 2 and the 1995-1998 HST velocities. In data separated by 10 h, we find that the east-west velocity uncertainty due to longitudinal fluctuations are nearly 10 m s⁻¹, so velocity fluctuations of 10 m s⁻¹ may occur on timescales that are even smaller than 10 h. Fluctuations across such a wide range of timescales limit the accuracy of zonal wind measurements. The concept of an average zonal velocity may be ill-posed, and defining a “temporal mean” zonal velocity as the average of several zonal velocity fields spanning months or years may not be physically meaningful.At 8°N, we use our global method to find peak zonal velocities of ∼110 m s⁻¹ in 2000 and ∼130 m s⁻¹ in 2008. Zonal velocities from 2000 Cassini data produced by our local and global methods agree everywhere, except in the vicinity of 8°N. There, the local algorithm shows that the east-west velocity has large variations in longitude; vast regions exceed ∼140 m s⁻¹. Our global algorithm, and all of the velocity-extraction algorithms used in previously-published studies, found the east-west drift velocities of the visible dark projections, rather than the true zonal velocity at the visible-cloud level. Therefore, the apparent increase in zonal winds between 2000 and 2008 at 8°N is not a true change in zonal velocity.At 7.3°N, the Galileo probe found zonal velocities of 170 m s⁻¹ at the 3-bar level. If the true zonal velocity at the visible-cloud level at this latitude is ∼140 m s⁻¹ rather than ∼105 m s⁻¹, then the vertical zonal wind shear is much less than the currently accepted value.     

Could CoRoT-7b and Kepler-10b be remnants of evaporated gas or ice giants?

We present thermal mass loss calculations over evolutionary time scales for the investigation if the smallest transiting rocky exoplanets CoRoT-7b (∼1.68R_Earth) and Kepler-10b (∼1.416R_Earth) could be remnants of an initially more massive hydrogen-rich gas giant or a hot Neptune-class exoplanet. We apply a thermal mass loss formula which yields results that are comparable to hydrodynamic loss models. Our approach considers the effect of the Roche lobe, realistic heating efficiencies and a radius scaling law derived from observations of hot Jupiters. We study the influence of the mean planetary density on the thermal mass loss by placing hypothetical exoplanets with the characteristics of Jupiter, Saturn, Neptune, and Uranus to the orbital location of CoRoT-7b at 0.017 AU and Kepler-10b at 0.01684 AU and assuming that these planets orbit a K- or G-type host star. Our findings indicate that hydrogen-rich gas giants within the mass domain of Saturn or Jupiter cannot thermally lose such an amount of mass that CoRoT-7b and Kepler-10b would result in a rocky residue. Moreover, our calculations show that the present time mass of both rocky exoplanets can be neither a result of evaporation of a hydrogen envelope of a “Hot Neptune” nor a “Hot Uranus”-class object. Depending on the initial density and mass, these planets most likely were always rocky planets which could lose a thin hydrogen envelope, but not cores of thermally evaporated initially much more massive and larger objects.