Yellowstone＇s acid waters： A plethora of chemical and biological activity

Yellowstone National Park contains numerous thermal and non-thermal acid waters with pH=1.23-5.0. These acid-sulfate waters are produced from the microbial oxidation of elemental sulfur which is formed from abiotic oxidation of hydrogen sulfide. Metal concentrations are usually very low in these waters so that H^＋ is often the major cation and greater in concentration than Al or Fe.Concentrations of Cu, Zn, Cd, Pb, Co, Ni, and Cr are frequently at or below detection limits. Many of these waters closely approximate pure sulfuric acid solutions. Thermal acid waters have been sampled in Norris Geyser Basin, Gibbon Geyser Basin, Lemonade Creek, and Washburn Springs. Non-thermal acid waters frequently contain high arsenic concentrations. Acid-sulfate waters life： numerous Bacteria, Archaea, and Eukarya. Chemoautotrophs, have been sampled in Brimstone Basin. The thermal acid waters contain an abundance of microbial life from all three domains of phototrophs, and heterotrophs are also common in these waters. Several of these microbes are responsible for the rapid oxidation of iron and arsenic in thermal spring overflows and within large pools. Measured oxidation rates are faster by many orders of magnitude than the abioitic oxidation rates. Common archaea in acid waters include Sulfolobus and Thermoplasma. Common bacteria include Acidithiobacillus, Acidimicrobium, Hydrogenobaculum, and Thiomonas. Common eukarya are algae such as Cyanidium, Euglena, Chlorella, Chlamydomonas, Ulothrix, and Zygogonium. Although aquatic life in acid-sulfate waters is dominated by microbes, insect larvae are also found.     

与苏门答腊-安达曼特大地震相联系的板块边界形变

2004年12月26日的苏门答腊-安达曼地震是自现代空间大地测量和宽频带地震学出现以来发生的第一个巨大地震（矩震级Mw〉9．0）。它为研究这种巨大且罕见的事件的特性提供了前所未有的机会。我们根据在苏门答腊西北部的近场全球定位系统（GPS）的探测结果并结合原地和远处的珊瑚礁垂直运动的观测，对这次事件造成的地表位移进行了估计。结果表明，该地震是由范围长〉1500km、宽〈150km范围内的巽他俯冲巨型逆断层破裂造成的。巨型逆断层在苏门答腊北部的近海滑动超过了20m，大部分的滑动深度不超过30km。对比大地测量学和地震学推断的滑动分布，发现在500秒长破裂发生之后的1．5个月内，断层滑动增加了～30％。在我们再次布设GPS测点之前，有震的和无震的滑动都出现在了巨型逆断层的浅部，那里是亚齐大海啸的源头。滑动在断层东南缘的锡默卢岛之下沿走向突然尖灭，在该处地震成核，并且2002年的晚期在此曾发生过一次Mw=7．2级地震。此外，该边缘也与2005年3月28日Mw=8．7的尼亚斯-锡默卢地震破裂的最北端相邻接。     

印度半岛地下水中氟的研究

地下水样品采自印度Andhra Pradesh，Anantapur地区。该地区主要地层为太古代半岛片麻岩。本文分析了该水样的F^-和其他化学参数。结果表明，该区氟源主要来自围岩，这个地区的F^-紧紧地吸附在包含粘土的矿物质土壤中。F^-与成岩的钠之间很强的正相关性反映出了风化侵蚀作用。正是这种相关性导致了F^-拘滤出，而半干旱气候和强灌溉也是F^-产生的原因。研究区循环水的碱性环境使土壤更容易滤出F^-，也导致地下水中的F^-含量高。高蒸发率引起的水在含水层中的滞留时间长和风化带水力传导系数低，将促使含氟矿物的溶解，这是另一个地下水中氟含量进一步增加的因素。提出了提高地下水质量的建议，从而改善居民的健康状况。     

Some Comments on Pressure Calibration over Lower Mantle Conditions

Recently, there is an urgent need in high pressure community for a pressure scale whose accuracy is comparable to the high precision of experimental data.One of the difficulties is the lack of an absolute scale,in particular at high temperature, to evaluate the EOS of standard materials.     

联邦德国运输体系的现代化与区域规划——以巴登富腾堡卅为例

联邦德国在第二次世界大战后,经济恢复最显著的特点是运输体系发展方向的确定。战前运输联系是柏林和萨克森、鲁尔产煤区间东西向的联系为主,现在则着重加强南北地区间的运输联系。这种经济发展战略影响着铁路和公路建设。从六十年代中期以来,遂成为全国空间远景规划的战略方针。     

景观是一个地理系统

地球及其周围的宇宙空间,是由呈同心圆排列的圈或壳组成的,这种独特的特征称为地圈(geosphere) (图1)。地理学研究的主要对象,就是包括该星球表面在内的     

地质学与矿床

前言这次会议的主要目的,是要评述一下运用地球物理和地球化学寻找新矿床的技术情况。通过本评论中提供的历史情况和对比研究,我们也希望改进地质、地球物理和地球化学之间的配合及每门学科的专业研究范围内的合作。我的责任是提供一种概念正在发生变化的地质结构,这些概念与将要讨论的地球物理和地球化学的改良和新技术是一致的。我想简单地评述一下过去十五年中发展     

Correcting Radial Velocities for Long-Term Magnetic Activity Variations

We study stars in the Lick planetary survey for correlations between simultaneous measurements of high-precision radial velocities vr and magnetic activity (as measured in an SIR emission index from Ca ii lambda8662). We find significant correlations in approximately 30% of the stars. After removing linear trends between SIR and vr, we find that the dispersion in vr in these stars is decreased by an average of 17%, or approximately 45% of the dispersion above the measurement noise. F stars and less active stars with variable Ca ii H and K lines are the most successfully corrected. The magnitude of the slope of the SIR versus vr relations increases proportional to vsini and (excepting M dwarfs) tends to decrease with decreasing Teff. We argue that the main cause of these effects is modification of the mean line bisector shape brought on by long-term, magnetic activity-induced changes in the surface brightness and convective patterns. The correlations can be used to partially correct vr data for the effects of long-term activity variations, potentially permitting study of planets around some (higher mass) younger stars and planets producing smaller stellar reflex velocities.     

The Detection of Multimodal Oscillations on alpha Ursae Majoris

We have used the star camera on the Wide-Field Infrared Explorer satellite to observe the K0 III star alpha UMa, and we report the apparent detection of 10 oscillation modes. The lowest frequency mode is at 1.82 μHz, and it appears to be the fundamental mode. The mean spacing between the mode frequencies is 2.94 μHz, which implies that all detected modes are radial. The mode frequencies are consistent with the physical parameters of a K0 III star, if we assume that only radial modes are excited. Mode amplitudes are 100-400 μmag, which is consistent with the scaling relation of Kjeldsen & Bedding.     

Hard X-Ray Emission from the Galaxy Cluster A2256

After the positive detection by BeppoSAX of hard X-ray radiation up to approximately 80 keV in the Coma Cluster spectrum, we present evidence for nonthermal emission from A2256 in excess of thermal emission at a 4.6 sigma confidence level. In addition to this power-law component, a second nonthermal component already detected by ASCA could be present in the X-ray spectrum of the cluster, which is not surprising given the complex radio morphology of the cluster central region. The spectral index of the hard tail detected by the Phoswich Detection System on board BeppoSAX is marginally consistent with that expected for the inverse Compton model. A value of approximately 0.05 μG is derived for the intracluster magnetic field of the extended radio emission in the northern regions of the cluster, while a higher value of approximately 0.5 μG could be present in the central radio halo, which is likely related to the hard tail detected by ASCA.