表面波对于混合层中湍流强化作用的实验研究

文中介绍了一项二层流体内密度界面处湍流挟卷的实验室研究。实验结果表明,有表面波存在时,混合层下密度界面处的挟卷速度较之无表面波时有明显的增大。这个实验事实的可能的海洋学含义为:不破碎的表面势波对于混合层内湍流有强化的作用,因而成为在考查密跃层变迁问题中应考虑在内的动力因素。     

由偏顶蛤贝壳中稳定同位素剖面追溯海水温度记录

本文用在加拿大诺瓦·斯科舍省芬克湾采集到的两只活体偏顶蛤(Modiolus)贝壳上的氧同位素组成重建了过去十年间的底层海水温度记录,它也可作为一种独立的方法来确定贝壳上外生长线的沉积时间。由于对贝壳进行了密集采样(可多至每个贝壳沉积年份取15个样品),贝壳上的δ~(16)O变化反映了芬克湾底层海水的季节性变化。两只贝壳所得的温度剖面符合得很好,说明它们基本上是与真实的环境温度相对应的。本研究证明在海胆疾病爆发时底层海水的温度并没有异常升高,这说明疾病传播的关键因素是带病的生物体,而不是温度。同位素技术也说明了在贝壳外表面上可见的外生长线是年轮性的,它们是在每年冬季最低水温时沉积出来的。     

下地壳基性麻粒岩流变强度实验研究

镁铁质基性麻粒岩被认为可能是大陆下地壳的主要组成岩石[1,2],涉及当前地球动力学研究中地壳变形和高原隆升,壳幔边界的力学耦合与拆离,底侵和拆沉作用等一系列地球动力学问题阳[3,4],具有重要的地球动力学意义.大陆下地壳的流变学性质是我们深入认识这些地球深部过程的关键点之一.     

Detection of a new interstellar molecular ion, H2COH+ (protonated formaldehyde)

A new interstellar molecular ion, H2COH+ (protonated formaldehyde), has been detected toward Sgr B2, Orion KL, W51, and possibly in NGC 7538 and DR21(OH). Six transitions were detected in Sgr B2(M). The 1(1,0)-1(0,1) transition was detected in all sources listed above. Searches were also made toward the cold, dark clouds TMC-1 and L134N, Orion (3N, 1E), and a red giant, IRC + 10216, without success. The excitation temperatures of H2COH+ are calculated to be 60-110 K, and the column densities are on the order of 10(12)-10(14) cm-2 in Sgr B2, Orion KL, and W51. The fractional abundance of H2COH+ is on the order of 10(-11) to 10-(9), and the ratio of H2COH+ to H2CO is in the range 0.001-0.5 in these objects. The values in Orion KL seem to be consistent with the "early time" values of recent model calculations by Lee, Bettens, & Herbst, but they appear to be higher than the model values in Sgr B2 and W51 even if we take the large uncertainties of column densities of H2CO into account. We suggest production routes starting from CH3OH may play an important role in the formation of H2COH+.     

A photochemical model of the martian atmosphere

The factors governing the amounts of CO, O2, and O3 in the martian atmosphere are investigated using a minimally constrained, one-dimensional photochemical model. We find that the incorporation of temperature-dependent CO2 absorption cross sections leads to an enhancement in the water photolysis rate, increasing the abundance of OH radicals to the point where the model CO abundance is smaller than observed. Good agreement between models and observations of CO, O2, O3, and the escape flux of atomic hydrogen can be achieved, using only gas-phase chemistry, by varying the recommended rate constants for the reactions CO + OH and OH + HO2 within their specified uncertainties. Similar revisions have been suggested to resolve discrepancies between models and observations of the terrestrial mesosphere. The oxygen escape flux plays a key role in the oxygen budget on Mars; as inferred from the observed atomic hydrogen escape, it is much larger than recent calculations of the exospheric escape rate for oxygen. Weathering of the surface may account for the imbalance. Quantification of the escape rates of oxygen and hydrogen from Mars is a worthwhile objective for an upcoming martian upper atmospheric mission. We also consider the possibility that HOx radicals may be catalytically destroyed on dust grains suspended in the atmosphere. Good agreement with the observed CO mixing ratio can be achieved via this mechanism, but the resulting ozone column is much higher than the observed quantity. We feel that there is no need at this time to invoke heterogeneous processes to reconcile models and observations.     

Naturally acidic and metalliferous waters at unmined volcanogenic massive sulfide deposits in the Bonnifield mining district, Alaska Range, east-central Alaska

The Bonnifield district hosts 26 tmmined volcanogenic massive sulfide （VMS） occurrences. Environmental geochemical samples of water and stream sediment were collected at several occurrences, concentrating on the two best-exposed and largest deposits, Red Mountain （RM） and Sheep Creek （SC）. Limited samples were also collected at the poorly exposed WTF deposit. The deposits are Late Devonian to Early Mississippian, and are hosted by felsic metavolcanic and carbonaceous schist members of the Totatlanika Schist or Keevy Peak Fm. Spring and stream waters at RM and SC have pH values commonly 〈3.5 （as low as 2.4 at RM and 2.5 at SC）, high conductivity （up to 11000 μS/cm）, and very high （Is to 100s mg/L） dissolved contents of Al, Cd, Co, Cu, Fe, Ni, and Pb. Waters at RM are characterized by extremely high REE contents （summed REE median 3200 μg/L, n=33）. At both RM and SC, pyrite oxidation and dissolution produce low pH waters that interact with and dissolve bedrock minerals, resulting in acidic, metal-laden, naturally degraded streams that are mostly devoid of aquatic life. Ferricrete is common. In contrast, WTF barely produces a surficial environmental footprint, mostly due to topography and relief. RM and SC are well exposed in the areas of relatively high relief, and both exhibit extensive areas of quartz-sericite-pyrite-alteration. While WTF shares many of the same deposit-and alteration characteristics, it is concealed by tundra in a large, nearly flat area. Surface water at WTF is absent and outcrops are sparse. Even though WTF is roughly the same size as Red Mountain （both around 3 million tonnes） and has similar base- and precious-metal grades, the surficial geochemical manifestation of WTF is minimal. However, exposure through mining of the altered, mineralized rock at WTF potentially could initiate the same processes of pyrite oxidation, acid generation, and mineral dissolution that are observed naturally at RM and SC.     

俄罗斯西西伯利亚和外贝加尔区古河道型铀矿床

本文系统地介绍了俄罗斯3个具有工业意义的古河道型铀矿化发育区（外乌拉尔，西西伯利亚和外贝加尔）的地质背景，铀矿化特征和铀成矿条件，指出切割到基底的古河道型铀矿床，既可产于跨地区的造山周围，也可产于活化的年青地台和古老地盾，既可形成于干燥的气候条件，也可形成于潮湿的气候条件。古河道型铀矿化可以从含矿层的沉积开始一直延续到被泥岩层或玄武岩层完全封盖。古河道的后成氧化分带有两种形式：氧化带－铀矿化带－原生灰色岩石；氧化带－氧化铁再沉积带－漂白带－原生灰色岩石。古河道型铀矿床具宽广的元素谱，这主要是与含矿围岩富含有机质和在氧化带尖灭处存在各种地球化学障有关。     

湖南印支期过铝质花岗岩的形成: 岩浆底侵与地壳加厚热效应的数值模拟

在合理构建华南印支期地质-物理模型的基础上, 利用FLAC软件, 模拟了该区印支期过铝质富钾花岗岩形成与基性岩浆底侵, 及陆壳变形叠置加厚两种动力学背景的可能联系. 模拟结果表明, 220 Ma±的基性岩浆底侵能导致地壳含水矿物相岩石的深熔, 但除非印支期存在大规模基性岩浆的底侵作用, 否则其热效应持续时间和热效应波及范围难以形成具大岩基规模的湖南印支期花岗岩. 在陆壳叠置加厚模型中, 地壳的叠置加厚可导致中下地壳界面温度升高到700℃以上, 引起片麻质岩石熔融, 当加厚因子达1.3, 白云母矿物脱水熔融产生的熔体达到熔体流动临界比例(≥20%), 从而形成花岗岩基; 结合印支期挤压逆冲推覆构造和同期基性火山岩极少出露的地质事实, 认为陆壳变形加厚可能是湖南印支期构造岩浆作用形成的主导因素.