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。     

川中磨溪—高石梯地区下寒武统龙王庙组层序格架内滩体的发育演化特征及对储层的控制

川中磨溪—高石梯地区龙王庙组可划分为两个三级层序。通过大量岩心、薄片以及测井资料综合分析,磨溪—高石梯地区龙王庙期整体属于局限台地沉积,可划分为台内滩、滩间洼地以及潟湖亚相。以台内滩颗粒含量、沉积构造以及单层滩体沉积厚度为基础,结合测井响应特征分析,将台内滩划分为滩核、滩翼以及白云岩坪等微相,并建立了台内滩的3种典型沉积序列:滩翼—滩核—白云岩坪、潟湖—滩间洼地—台内滩,以及滩间洼地—台内滩。层序格架内台内滩的纵横向发育特征表明:SQ_2时期较SQ_1时期更为发育,滩体单层厚度和总厚度均较大,层序界面附近的滩核—白云岩坪沉积序列上部为最有利的储层发育相带。     

塔里木盆地西南地区早中寒武世岩相古地理

塔里木盆地西南地区早中寒武世岩相古地理存在一定争议,这制约了该区的勘探评价。综合利用露头、钻井和地震资料,开展沉积相、地震相分析,并结合区域构造背景,恢复了岩相古地理格局,提出了相应的沉积模式。中下寒武统发育陆棚相、开阔台地相、局限台地相、蒸发台地相和缓坡相。震旦纪末期麦盖提斜坡南部形成水下低隆起,向南在西南坳陷区残留部分被动陆缘,主要发育缓坡相、陆棚相;麦盖提斜坡区地势较高,地层较薄,主要发育局限台地和蒸发台地潮坪;巴楚隆起区水体局限,在干燥炎热气候下形成了厚度较大的蒸发台地膏盐湖沉积。巴楚隆起区和麦盖提斜坡区中下寒武统膏盐岩分布广泛,与下伏碳酸盐岩可构成良好的储盖组合,西南坳陷区残留部分被动陆缘,烃源岩发育条件较好,这表明塔西南具有较好的油气前景。     

尼日尔Termit盆地上白垩统Madama组地震相识别与沉积相演化分析

以层序地层学及沉积学理论为指导,综合运用测井、录井以及地震资料,将尼日尔Termit盆地上白垩统Madama组划分为一个三级层序(MS),并进一步识别出低位体系域、海侵体系域以及高位体系域。在等时层序地层格架内,识别出前积反射地震相、河道充填反射地震相、平行-亚平行反射地震相以及杂乱反射地震相等四种类型,并识别出辫状河三角洲的沉积相类型。认为层序MS的低位体系域主要发育辫状河三角洲前缘亚相,高位体系域则主要发育辫状河三角洲平原亚相。Madama组整体表现为一个海退的沉积演化过程。     

柴达木盆地东部新生代盆地结构与演化

本文对柴达木盆地东部新生代盆地结构和构造演化进行了研究.地震剖面揭示柴达木盆地东部新生界分别向南、北盆地边缘变薄和尖灭,盆地北部被欧龙布鲁克山和埃姆尼克山隆起强烈改造.通过对新生代地层厚度横向变化以及地层剖面分析,确定欧北断裂自中新世晚期开始向北逆冲,导致欧龙布鲁克山发生隆升和德令哈凹陷的形成.埃北断裂从上新世开始活动,与欧北断裂同时向北逆冲,导致德令哈凹陷进一步沉降,形成厚度达2600m的狮子沟组.埃南断裂在第四纪开始大规模向南逆冲,不仅造成其北侧的欧龙布鲁克山和埃姆尼克山隆起强烈抬升和向南推覆,而且导致南侧霍布逊凹陷的形成,成为柴达木盆地第四纪沉积中心.早期提出的前陆盆地和背驮式盆地模型显然不能解释柴达木盆地东部新生代构造格架和演化历史.本次研究认为柴达木盆地东部的形成是强烈的水平挤压作用导致地壳发生大规模褶皱的结果,即柴达木盆地东部新生代是一个大规模向斜.该向斜盆地模型很好地解释了新生代地层向盆地边缘减薄以及沉积中心主要位于盆地中部等现象.了解柴达木盆地东部构造发展对了解青藏高原侧向扩展具有重要意义.     

北疆沙尔布尔提山地区早泥盆-早石炭世沉积相、物源演变及其意义

准噶尔西北部沙尔布尔提山地区下泥盆统到下石炭统的沉积可划分为滨海相和海岸平原相。其中下泥盆统和布克赛尔组底部的乌图布拉克亚组为滨海碎屑岩相,曼格尔亚组为滨海碎屑岩和碳酸盐岩相,芒克鲁亚组为滨海碳酸盐岩相。中泥盆统呼吉尔斯特组为海岸平原相。上泥盆统洪古勒楞组底部为海岸平原相,向中部过渡为滨海碳酸盐岩相,顶部为滨海碎屑岩相。下石炭统黑山头组为滨海碎屑岩相。下泥盆统和下石炭统的古流向总体从北向南,显示研究区以北地区为物源区,即成吉斯-塔尔巴哈台褶皱带。结合沉积相的研究成果,本区可能属成吉斯-塔尔巴哈台褶皱带以南的晚古生代陆缘区。物源演变趋势分析揭示早泥盆世成吉斯-塔尔巴哈台带中的早古生代岛弧发生隆起,为乌图布拉克亚组提供成熟度很低的碎屑物质。随着岛弧被剥蚀殆尽,中、晚泥盆世呼吉尔斯特组和洪古勒楞组沉积时转而接受岩屑型再旋回造山带的物源供应,而早石炭世的物源则为过渡型再旋回造山带区。这种物源变化反映了成吉斯-塔尔巴哈台褶皱带的建造特征和隆起过程。     

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.     

云南兰坪盆地北部东缘铅锌矿床喷流沉积成因的厘定———来自矿物学和硫同位素证据

通过详细的野外地质工作和显微镜下观察,对云南兰坪盆地东北部维西—乔后断裂带上三叠统石钟山组(T₃s)中产出的铅锌矿床成因进行厘定。研究结果表明,测区内存在大量典型的同生沉积矿床标志,如:纹层构造、条纹条带构造、网脉构造、黄铁矿条带软沉积构造、黄铁矿草莓状结构、黄铁矿胶状构造、闪锌矿同心环状构造等。青甸湾矿床金属硫化物硫同位素测试结果显示,黄铁矿的δ34 S介于3.7‰ ~ 8.1‰,均值5.34‰; 闪锌矿的δ34 S介于5.2‰ ~ 10.0‰之间,均值为7.18‰; 方铅矿的δ34 S介于5.2‰ ~ 9.9‰之间,均值为7.275‰,铅锌矿床硫来源于海水硫酸根无机还原。结合矿床形成时代及大地构造背景,认为该区铅锌矿为喷流沉积作用形成。      

Numerical modelling of rise and fall of a dense layer in salt diapirs

Numerical models are used to study the entrainment of a dense anhydrite layer by a diapir. The anhydrite layer is initially horizontally embedded within a viscous salt layer. The diapir is down-built by aggradation of non-Newtonian sediments ( n = 4, constant temperature) placed on the top of the salt layer. Several parameters (sedimentation rate, salt viscosity, perturbation width and stratigraphic position of the anhydrite layer) are studied systematically to understand their role in governing the entrainment of the anhydrite layer. High sedimentation rates during the early stages of the diapir evolution bury the initial perturbation and, thus, no diapir forms. The anhydrite layer sinks within the buried salt layer. For the same sedimentation rate, increasing viscosity of the salt layer decreases the rise rate of the diapir and reduces the amount (volume) of the anhydrite layer transported into the diapir. Model results show that viscous salt is capable of carrying separate blocks of the anhydrite layer to relatively higher stratigraphic levels. Varying the width of the initial perturbation (in our calculations 400–800 m), from which a diapir triggers, shows that wider diapirs can more easily entrain an embedded anhydrite layer than the narrower diapirs. The anhydrite layer is entrained as long as rise rate of the diapir exceeds the descent rate of the denser anhydrite layer. We conclude that the four parameters mentioned above govern the ability of a salt diapir to entrain an embedded dense layer. However, the model results show that the entrained blocks inevitably sink back if the rise rate of the diapir is less than the rate of descent of the anhydrite layer or the diapir is permanently covered by a stiff overburden in case of high sedimentation rates.