Characterization of Banded Iron Formations by Two-Dimensional XRF Imaging and XANES Analyses

Abstract: Synchrotron radiation-induced X–ray fluorescence (SR–XRF) and conventional X-ray fluorescence (XRF) analyses were applied to determine the distributions of iron, manganese, calcium, titanium, and silicon, and chemical forms of iron and trace manganese in three banded iron formation (BIF) samples. The XRF imagings on the weathered and altered BIF from the Cleaverville Formation (3. 3–3. 1 Gyr), Western Australia, showed redistributions of iron, calcium, and manganese with the disappearance of the primary bandings, while, in contrast, titanium preserved its primary depositional distribution. The XRF imagings on the BIF from the Hamersley Group (2. 5 Gyr), Western Australia, showed that manganese and titanium distribute originally at boundary region between the iron-rich mesoband and the silica-rich mesoband. The X-ray Absorption Near Edge Structure (XANES) analysis revealed that the chemical forms of manganese and iron well represent the rhythmic change of the bandings.     

大地电磁场偏移成像方法的改进与应用

本文在对电磁场成像技术进行系统研究和总结的基础上,分析综述了大地电磁场成像技术的研究现状与存在问题,进而提出了改进的有限差分法大地电磁场偏移成像技术,使差分方程精度和成像分辨率得到了提高,并对客观选取背景电导率、两种极化模式联合成像以及多参数和再次成像进行了创新研究,最后利用模型试验和实际大地电磁场资料的实例展示了该方法偏移成像的成果及其实用性.     

What can we learn from accretion disc eclipse mapping experiments?

The accretion disc eclipse mapping method is an astrotomographic inversion technique that makes use of the information contained in eclipse light curves to probe the structure, the spectrum and the time evolution of accretion discs in cataclysmic variables. This paper presents examples of eclipse mapping results that have been key to improve our understanding of accretion physics. (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Stellar surface imaging: mapping brightness and magnetic fields

Rapidly rotating late‐type stars typically display signs of magnetic activity that exceed those seen on the Sun by over two orders of magnitude. The techniques of Doppler imaging and Zeeman Doppler imaging have been instrumental in unveiling magnetic activity patterns at the photospheres of these active stars. Essentially, these techniques work by inverting time‐series of high resolution spectra to produce temperature, brightness and/or magnetic field maps at the surfaces of stars. I will describe how these techniques work and review what they have taught us about the nature of magnetic activity in rapid rotators over the last 20 years. Finally, I will conclude by outlining the capabilities of these techniques in light of new instrumentation that is now becoming available. (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Differential rotation of cool active stars

The surface differential rotation of active solar‐type stars can be investigated by means of Doppler and Zeeman‐Doppler Imaging, both techniques enabling one to estimate the short‐term temporal evolution of photospheric structures (cools spots or magnetic regions). After describing the main modeling tools recently developed to guarantee a precise analysis of differential rotation in this framework, we detail the main results obtained for a small number of active G and K fast rotating stars. We evoke in particular some preliminary trends that can be derived from this sample, bearing the promise that major advances in this field will be achieved with the new generation of spectropolarimeters (ESPaDOnS/CFHT, NARVAL/TBL). (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Spots on FK Com: active longitudes and “flip‐flops”

We have earlier investigated the surface structures of a late‐type, single, giant FK Com for the years 1994–1998 using Doppler imaging. These surface temperature maps revealed long‐lived active regions at high latitudes. Long‐term photometric observations also show that these active regions tend to occur at two permanent active longitudes which are 180 degrees apart from each other, and that the activity switches the longitude with an average period of about 3 years (the “flip‐flop” phenomenon). In this work we present new Doppler maps of FK Com obtained 1998‐2003 and light‐curve maps obtained 2002–2003. These new maps are investigated together with the earlier temperature maps and light‐curve maps, with an aim of further studying the active longitudes, “flip‐flop” phenomenon and surface differential rotation on FK Com. (© 2004 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

影像测量仪的光学成像误差分析及计算

对光学影像测量仪的光学成像误差,特别对摄像镜头的畸变误差进行了研究。运用标准模版标定法,计算出镜头成像的各项畸变参数,分析了畸变误差大小及其分布状况。应用畸变参数对测量结果进行校正,结果表明,径向畸变较大,切向畸变和薄棱镜畸变较小,且图像中心区域畸变很小,边缘畸变增大。在精密测量中需要考虑到畸变的影响,并对所测得的图像坐标进行修正。     

成像测井在地质油藏研究中的应用

成像测井包含了大量的地质信息,可以更加直观和准确地显示出地下油藏的地质特征,能够对构造（构造倾角、断层）和沉积（层理面、岩性面、古水流方向）等方面进行分析和应用。而且,成像测井是研究裂缝性储层的最有效和直观的手段,能够满足评价裂缝油气藏所需要的包括孔洞、裂缝发育程度及其有效性和面孔率等参数。此外,成像测井还有助于确定现今地应力方向及判断井眼的稳定性,为钻采工程方面提供科学决策的重要依据。总之,成像测井与其他专业密切配合,能够解决更多的地质油藏问题,从而为勘探开发提供更多科学有效的手段。     

田野土墩墓地学影像特征与成像机理及解译分析——以浙北湖州地区为例

浙北湖州地区土墩墓分布广,数量多。建立符合浙北实际的土墩墓影像解译标志是调查、发现和研究土墩墓的技术关键。本文总结了多种土墩墓的分布规律和影像特征,并对易与土墩墓混淆的其他墓葬和地物的影像进行了研究。在此基础上对土墩墓影像的成像机理作了分析和归纳,得出土墩墓影像地表特征的基本规律。     

地磁与地电混合观测台地磁的地电测数干扰处理方法

我国地震前兆观测台网中地磁与地电观测仪器经常相距很近。 而地电台每小时加电观测一次, 由于电磁感应, 使得地磁观测资料有间隔为1小时的高频干扰, 使得地震前兆信息或其他地球物理过程产生的异常信息在地磁数据分析中难以分辨。 经过分析这些干扰信息特点, 提出了采用Fourier变换在频率域中将高频干扰进行滤除和采用与典型干扰波形相关的方法去除地电测数干扰, 该文对安徽蒙城地震台的观测资料的处理结果表明了方法的有效性。 很多中国大陆地震前兆观测台具有类似的干扰, 因此该方法具有一定推广价值。