Analysis of petroleum hydrocarbons in mangrove sediments of Red Sea of Yemen

A field work has been carried out to identify the occurrence of oil and oil products pollution in mangrove sediment from Red Sea of Yemen. The concentration of total petroleum hydrocarbons is from 700ng/g at Kamaran Island station to 400 ng/g at Al-Hodiedah station, and the total organic carbon （TOC） in samples ranges from 0. 07% at Dhubab station to 0. 03% at Kamaran Island station. This pollution is as a result of localized oil pollution and/or heavy ship traffic in the Red Sea and Gulf of Aden.     

“高密度浊流”是砂质碎屑流吗？

习惯上认为，浊流是一种液性流，其沉积物靠液态湍动支撑；而碎屑流是一种塑性流，其沉积物靠基质强度、分散压力和上浮力支撑。“高密度浊流”的概念是指高浓度的、通常是非湍动的液态流，其沉积物主要靠基质强度、分散压力和上浮力支撑。以往认为顶部带有湍流云的牵引毯代表高密度浊流其实是一个错误，因为牵引毯既不是液性流也不是湍流。碎屑流也可能在其顶部带有湍流云。牵引毯／碎屑流与其上面的湍流云在流变学、沉积物支撑机制     

蒙塔那州博耳德地区岩基中的铀矿化

本文介绍了花岗岩类(石英二长岩及花岗闪长岩)岩基型侵入体中矽化带型热液铀矿床的岩体、区域构造、伴生有色金属矿床、铀矿床本身及成矿年代。铀矿化和灰色及黑色微粒石英脉或玉髓脉的关系密切。铀矿化晚于锌铅矿化。铀矿化年代为6000万年。其后有英安岩的侵入。     

什么是断层陡坎？

近十年来，不断加强对构造活动性的仪器观测和历史记录。人们把注意力集中于根据地质，地貌的记录鉴别和研究古地震上，重要的是识别断层地貌特片，例如，断层陡坎，它可能是某一区域构造活动类型及其活动时间的明显标志。     

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.