柴达木盆地那棱格勒河及其尾闾盐湖锂成矿物源：来自水化学和锶、硫同位素证据

柴达木盆地那棱格勒河尾闾盐湖(一里坪干盐滩、东台吉乃尔盐湖、西台吉乃尔盐湖和察尔汗盐湖别勒滩区段)赋存了我国目前最大的卤水锂矿床。那棱格勒河及其尾闾盐湖锂的物源仍存在一定争议,主要有围岩风化、古湖残留、含盐系地层淋滤、油田水、深部水等,目前缺乏有力的地球化学证据。本文系统采集了那棱格勒河流域及其尾闾盐湖不同水体样品16件,分析了其主、微量元素含量及锶、硫同位素组成。结合前人的研究成果,对区域水体中锂的来源进行了探讨,得出结论如下:那棱格勒河水锂含量(0.45～0.79 mg/L)比楚拉克阿拉干河支流(0.00～0.05 mg/L)高出一个数量级,其高锂含量主要受洪水河支流的补给;洪水河高锂含量与其上游热泉水的补给有关,该热泉水锂、锶含量高、⁸⁷Sr/⁸⁶Sr比值偏高,δ³⁴S值偏低,与青藏高原典型热泉水地球化学特征(锂含量0.4～34.8 mg/L,锶含量0.07～4.24 mg/L,⁸⁷Sr/⁸⁶Sr比值0.71224～0.71259,δ³⁴S值-10....     

地下管线探测电磁场异常特征的理论与实践

分析了频率域中一次电磁场和二次电磁场的分布特征，以及利用Hx,Hx的异常特征点确定地下金属管线的理论依据，指出了在复杂地质情况下进行正常场改正的必要性，最后利用不同类型管线检测实际资料，说明了方法的有效性。     

高频浅地层剖面技术在海底管道探测中的应用

在海底管道的探测中,为获知海管在海底的真实赋存状态,确定其埋藏深度或悬跨高度,多使用高频浅地层剖面仪等传统声学设备。但在海底斜坡、凹坑、凸起等不平整地层处,由于设备自身原理造成的地层探测界面偏移、图像失真及资料多解性问题仍困扰着工程人员。通过正演模拟的方法探究高频浅地层剖面仪在海底特殊地层处海管检测的波场传播特征,探讨资料的解释陷阱,并提出了解决方案。研究结果表明,利用浅地层剖面仪探测管道在海底的赋存状态,应将探测图像与海底地形、地貌、沉积物运移等因素结合起来综合考虑,把探测图像回归到真实海底环境中,以准确评价海底管道的安全状态。     

北黄海盆地东部M隆起构造特征及演化

北黄海盆地是中国东部近海中生代断陷型盆地,详细记载着中国东部复杂的构造活动信息,期间经历了多期岩浆活动和构造反转。M隆起位于北黄海盆地东部,其构造活动记录比周边的坳陷更为详细。为充分认识M隆起的地质结构及沉积响应关系,在充分利用地震、钻测井等资料的基础上,结合区域构造背景,从构造运动学和动力学等方面探讨分析其构造演化历程,进而为北黄海盆地乃至中国东部地区的构造演化提供新的依据。高精度三维地震资料及地质分析揭示,该隆起区发育有5个典型的不整合面,纵向上可划分为5个构造层。结合北黄海盆地所处构造位置、构造变形和沉积充填特征,及板块运动和区域构造演化史,将北黄海盆地东部M隆起自中侏罗世至今的构造演化划分为5个阶段(共9期):裂陷阶段(稳定沉积期、掀斜形成期、早白垩世凹陷沉积期)、构造反转阶段(晚白垩世抬升剥蚀期)、再次裂陷阶段(早渐新世初沉积期、早渐新世末剥蚀期、F2断层活跃期)、再次构造反转阶段(整体抬升期)、区域沉降阶段(区域沉降期)。     

丛粒藻形态多样性与遗传多样性研究

观察了采集自不同地点的3株丛粒藻(Botryococcus braunii)(AGB-Bb01、AGB-Bb02和AGB-Bb03)的显微结构和亚显微结构,以18S rDNA和ITS区序列为目标位点比较分析了16株丛粒藻藻株的遗传距离和序列相似性,重建了系统发生树。结果表明:丛粒藻不同地理株在细胞大小、聚落大小和聚落细胞数目方面存在较明显的差异,亚显微结构显示不同藻株的杯状鞘厚度及细胞包埋程度也存在差异;不同地理株间具有较高的遗传多样性,系统发生树显示所有藻株可分成2个簇群和4个亚群,存在一定程度的地理隔离。研究证明了18S rDNA和ITS区序列是进行丛粒藻基因分型和遗传多样性研究的良好位点。本研究为系统了解丛粒藻的遗传多样性和开展优良藻株选育工作奠定了基础。     

印尼8.7、8.5级远震对云南地区小震的激发和地下流体异常响应初探

2004年12月26日和2005年3月29日,印度尼西亚苏门答腊西北海域相继发生8.7和8.5级地震。通过对这两次地震与云南地震活动关系和地下流体记录异常变化的分析,认为:印尼两次8级地震的发生可能会使云南提前进入新一轮强震活跃期;远震对云南地区小震的激发和导致地下流体记录出现异常变化的因素虽然都与大地震面波的强弱、地质构造环境等有关,但机理不同。     

脱壳病和吻肿病东风螺体内致病菌及条件致病菌菌相研究

为探讨东风螺脱壳病和吻肿病与体内外致病菌及条件致病菌的相关性,测定了东风螺养殖水体环境中异养菌菌落总数,并对病螺及健康螺体内致病菌及条件致病菌进行了分离鉴定.经兔血培养基、TCBS培养基和弧菌显色培养基分离培养,用生化试验和细菌16S rDNA序列分析鉴定,结果显示:发生脱壳病的方斑东风螺螺池水体中的异养菌菌落总数为1.34×106 cfu/mL,病螺体内分离的致病菌及条件致病菌有副溶血弧菌、哈氏弧菌、河流弧菌、Vibrio hepatarius、腐败希瓦氏菌、海藻希瓦氏菌和芽孢杆菌,其中优势菌株为副溶血性弧菌溶血菌株和哈氏弧菌;脱壳病与吻肿病共患的泥螺螺池水体中异养菌的菌落总数为1.46×107 cfu/mL,病螺体内分离的致病菌及条件致病菌有副溶血弧菌、哈氏弧菌、鲍鱼希瓦氏菌、海藻希瓦氏菌和芽胞杆菌,优势菌株为海藻希瓦氏菌、鲍鱼希瓦氏菌和哈氏弧菌;健康东风螺螺池水体异养菌菌落总数为7.6×104 cfu/mL,健康东风螺螺体内的优势菌株为副溶血性弧菌非溶血菌株和Vibrio hepatarius.试验结果表明,东风螺脱壳病和吻肿病与养殖水体环境中异养菌的总数及螺体内部致病菌及条件致病菌分布具有一定相关性.     

The extended rotation curve and the dark matter halo of M33

We present the 21-cm rotation curve of the nearby galaxy M33 out to a galactocentric distance of 16 kpc (13 disc scalelengths). The rotation curve keeps rising out to the last measured point and implies a dark halo mass ≳5×10¹⁰ M_⊙. The stellar and gaseous discs provide virtually equal contributions to the galaxy gravitational potential at large galactocentric radii, but no obvious correlation is found between the radial distribution of dark matter and the distribution of stars or gas.
Results of the best fit to the mass distribution in M33 picture a dark halo which controls the gravitational potential from 3 kpc outward, with a matter density which decreases radially as R ^−1.3. The density profile is consistent with the theoretical predictions for structure formation in hierarchical clustering cold dark matter (CDM) models, and favours lower mass concentrations than those expected in the standard cosmogony.     

Modelling the bar in the centre of the starburst galaxy M82

We present VLA A-array 21-cm atomic hydrogen (H  i ) absorption observed against the central region of the starburst galaxy M82 with an angular resolution of ∼1.3 arcsec (≃20 pc). These observations, together with MERLIN H  i absorption measurements, are compared with the molecular (CO) and ionized ([Ne  ii ]) gas distributions and are used to constrain the dynamics and structure of the ionized, neutral and molecular gas in this starburst.
A position–velocity diagram of the H  i distribution reveals an unusual 'hole' feature which, when previously observed in CO, has been interpreted as an expanding superbubble contained within a ring of gas in solid body rotation. However, we interpret this feature as a signature of a nearly edge-on barred galaxy. In addition, we note that the CO, H  i and [Ne  ii ] position–velocity diagrams reveal two main velocity gradients, and we interpret these as gas moving on x₁- and x₂-orbits within a bar potential. We find the best fit to the data to be produced using a bar potential with a flat rotation curve velocity v _b=140 km s⁻¹ and a total length of 1 kpc, a non-axisymmetry parameter q =0.9, an angular velocity of the bar Ω_b=217 km s⁻¹ arcsec⁻¹, a core radius R _c=25 pc, an inclination angle i =80° and a projected angle between the bar and the major axis of the galaxy φ '=4°. We also discuss the orientation of the disc and bar in M82.     

The mass of the Andromeda galaxy

This paper argues that the Milky Way galaxy is probably the largest member of the Local Group. The evidence comes from estimates of the total mass of the Andromeda galaxy (M31) derived from the three-dimensional positions and radial velocities of its satellite galaxies, as well as the projected positions and radial velocities of its distant globular clusters and planetary nebulae. The available data set comprises 10 satellite galaxies, 17 distant globular clusters and nine halo planetary nebulae with radial velocities. We find that the halo of Andromeda has a mass of together with a scalelength of 90 kpc and a predominantly isotropic velocity distribution. For comparison, our earlier estimate for the Milky Way halo is Although the error bars are admittedly large, this suggests that the total mass of M31 is probably less than that of the Milky Way . We verify the robustness of our results to changes in the modelling assumptions and to errors caused by the small size and incompleteness of the data set.
Our surprising claim can be checked in several ways in the near future. The numbers of satellite galaxies, planetary nebulae and globular clusters with radial velocities can be increased by ground-based spectroscopy, while the proper motions of the companion galaxies and the unresolved cores of the globular clusters can be measured using the astrometric satellites Space Interferometry Mission ( SIM ) and Global Astrometric Interferometer for Astrophysics ( GAIA ). Using 100 globular clusters at projected radii 20 R 50 kpc with both radial velocities and proper motions, it will be possible to estimate the mass within 50 kpc to an accuracy of 20 per cent. Measuring the proper motions of the companion galaxies with SIM and GAIA will reduce the uncertainty in the total mass caused by the small size of the data set to 22 per cent.