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。     

青藏高原及邻区未来地震活动性趋势数值分析

区域中长期地震危险性数值分析研究,需要对其初始构造应力场有所了解,但目前以及未来一段时期内仍无法直接观测到深部孕震层区域的应力场状况.本文首先基于岩石库仑-摩尔破裂准则,利用青藏高原及邻区百年历史范围内的强震信息,来反演估算该区域的初始应力场.然后,考虑区域构造应力加载及强震造成的应力扰动共同作用,重现了历史强震的发展过程.然而对于初始应力场的反演估算,本文仅能给出区域其上下限的极限值,并不能唯一确定.因此,采用Monte Carlo随机法,进行大量独立的随机试验计算,生成数千种有差异的区域初始应力场模型,且保证每种模型都能令历史强震有序发生,但未来应力场演化过程不尽相同.最后,将数千种模型在未来时间段内的危险性预测结果集成为数理统计结果,据此给出了区域未来的地震危险性概率分布图.初步结果显示未来强震危险性概率较高地区集中在巴颜喀拉块体边界及鲜水河断裂带地区.     

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。     

准噶尔盆地古隆起的分布与基本特征

准噶尔盆地外侧三大边界动力体系的作用及基底结构的差异性导致准噶尔盆地在不同地质时期发育不同性质的隆起构造。石炭纪晚期东北侧的造山作用形成了盆地北部隆起,晚二叠世北部隆起分异为陆梁隆起与乌伦古坳陷;早二叠世西北侧的造山作用形成了车排子隆起,随后的冲断作用形成了克拉玛依--夏子街断裂带。燕山期的压扭作用形成了沉积盖层中的车排子--莫索湾隆起。新生代北天山向北的冲断作用导致准噶尔盆地南部地区急剧挠曲沉降,盆地向南掀斜,隆起向北迁移。据基底的性质、形成时间、活动方式、地质结构与保存状态等特点将准噶尔盆地的隆起划分为继承型、间断型、掀斜型与冲断带型等4种基本类型。     

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.     

In situ Pb and bulk Sr isotope analysis of the Yinchanggou Pb-Zn deposit in Sichuan Province (SW China): Constraints on the origin and evolution of hydrothermal fluids

The Yinchanggou Pb-Zn deposit, located in southwestern Sichuan Province, western Yangtze Block, is stratigraphically controlled by late Ediacaran Dengying Formation and contains >0.3 Mt of metal reserves with 11 wt% Pb + Zn. A principal feature is that this deposit is structurally controlled by normal faults, whereas other typical deposits nearby (e.g. Maozu) are controlled by reverse faults. The origin of the Yinchanggou deposit is still controversial. Ore genetic models, based on conventional whole-rock isotope tracers, favor either sedimentary basin brine, magmatic water or metamorphic fluid sources. Here we use in situ Pb and bulk Sr isotope features of sulfide minerals to constrain the origin and evolution of hydrothermal fluids. The Pb isotope compositions of galena determined by femtosecond LA-MC-ICPMS are as follows: ²⁰⁶Pb/²⁰⁴Pb = 18.17–18.24, ²⁰⁷Pb/²⁰⁴Pb = 15.69–15.71, ²⁰⁸Pb/²⁰⁴Pb = 38.51–38.63. These in situ Pb isotope data overlap with bulk-chemistry Pb isotope compositions of sulfide minerals (²⁰⁶Pb/²⁰⁴Pb = 18.11–18.40, ²⁰⁷Pb/²⁰⁴Pb = 15.66–15.76, ²⁰⁸Pb/²⁰⁴Pb = 38.25–38.88), and both sets of data plotting above the Pb evolution curve of average upper continental crust. Such Pb isotope signatures suggest an upper crustal source of Pb. In addition, the coarse-grained galena in massive ore collected from the deep part has higher ²⁰⁶Pb/²⁰⁴Pb ratios (18.18–18.24) than the fine-grained galena in stockwork ore sampled from the shallow part (²⁰⁶Pb/²⁰⁴Pb = 18.17–18.19), whereas the latter has higher ²⁰⁸Pb/²⁰⁴Pb ratios (38.59–38.63) than the former (²⁰⁸Pb/²⁰⁴Pb = 38.51–38.59). However, both types of galena have the same ²⁰⁷Pb/²⁰⁴Pb ratios (15.69–15.71). This implies two independent Pb sources, and the metal Pb derived from the basement metamorphic rocks was dominant during the early phase of ore formation in the deep part, whereas the ore-hosting sedimentary rocks supplied the majority of metal Pb at the late phase in the shallow part. In addition, sphalerite separated from different levels has initial ⁸⁷Sr/⁸⁶Sr ratios ranging from 0.7101 to 0.7130, which are higher than the ore formation age-corrected ⁸⁷Sr/⁸⁶Sr ratios of country sedimentary rocks (⁸⁷Sr/⁸⁶Sr_200 Ma = 0.7083–0.7096), but are significantly lower than those of the ore formation age-corrected basement rocks (⁸⁷Sr/⁸⁶Sr_200 Ma = 0.7243–0.7288). Again, such Sr isotope signatures suggest that the above two Pb sources were involved in ore formation. Hence, the gradually mixing process of mineralizing elements and associated fluids plays a key role in the precipitation of sulfide minerals at the Yinchanggou ore district. Integrating all the evidence, we interpret the Yinchanggou deposit as a strata-bound, normal fault-controlled epigenetic deposit that formed during the late Indosinian. We also propose that the massive ore is formed earlier than the stockwork ore, and the temporal-spatial variations of Pb and Sr isotopes suggest a certain potential of ore prospecting in the deep mining area.     

岱崮地貌的基本特征、成因和演化

岱崮地貌是一种寒武系碎屑岩之上的平顶灰岩地貌,为中国五大地貌之一,对其研究具有地质学、古地理环境等科学意义。本文通过野外地质调查及室内研究,分析研究了岱崮地貌的特征、成因和演化,得出以下结论：1） 岱崮镇的崮主体呈NW向展布,由崮体和崮基组成。崮体包括崮顶、崮腰和崮底,崮顶为灰岩,崮腰和崮底以碎屑岩为主,崮基为前寒武系岩浆岩或太古宇泰山群;2） 近水平岩层是岱崮地貌发育的基础;3） NNW向、NW向和近EW向断层是岱崮地貌形成的根本因素,NW向和NE 向节理是主控因素,控制了岱崮地貌的走向、密度;4） 岱崮地貌古生代以来经历了多个时期的演化,经过加里东运动、海西运动和印支运动留存的寒武系-中奥陶统、上石炭统-二叠系是岱崮地貌形成的基础,燕山期中侏罗世末-晚侏罗世（162～149.8 Ma）、白垩纪（140～90 Ma）及喜马拉雅早期（65～43 Ma）产生的断层及节理是岱崮地。     

思茅坳陷油气地质特征与勘探前景

思茅坳陷存在古生界和中一新生界两套沉积盖层,具有多套生储盖组合。以二叠系、三叠系为主力烃源岩,储层低孔低渗,侏罗系一白垩系“红层”组成区域盖层。思茅坳陷气水同喷、原油显示表明,该区海相地层仍有油气勘探前景,以存在K3-N区域盖层、断裂改造较弱、源岩成熟度较低、构造发育的英德一景谷、勐腊一勐满含油气保存单元为首选靶区,具有一定勘探前景。     

兴文侵蚀型天坑的形成演化过程研究

According to the first-hand investigation and study on Xingwen Global Geopark,the results and the data show that apart from Dayanwan and Xiaoyanwan collapsed karst Tiankeng,there are other karst landforms in Bowang Mount scenic spot such as Feiwu Cave,Dao Cave,Cangshuiyan Gorge,Nanxing TanKeng and so on.These typical karst landforms could be regarded as different vestiges of erosive karst Tiankeng of Xingwen Global Geopark,which stand for the evolutional processes of erosive karst Tiankeng separately.Moreover,the evolutional processes of erosive karst Tiankeng could be divided into the following continuous processes:an erosive karst Tiankeng develops from the processes of eroding and dissolving & extending of silo Sinkhole,and subsequently degrades to a large gorge or doline.It is worth pointing out that except for erosion of flowing water,at the same time,collapse effect has been playing extremely important role in the forming processes of these special erosive landforms.