大极距激电方法在姚家岭铜铅锌矿床深部找矿中的应用

南陵县姚家岭铜铅锌矿床,是安徽省十五期间新发现的一处中到大型矿床,该区的物探工作,尤以激电中梯扫面和激电测深,在深部找矿中发挥了较为重要的作用,本文阐述大极距激电方法在本区寻找深部隐伏矿体的应用效果。     

An unfolding method for X-ray spectro-polarimetry

X-ray polarimetry has great scientific potential and new experiments, such as X-Calibur, PoGOLite, XIPE, and GEMS, will not only be orders of magnitude more sensitive than previous missions, but also provide the capability to measure polarization over a wide energy range. However, the measured spectra depend on the collection area, detector responses, and, in case of balloon-borne experiments, the absorption of X-rays in the atmosphere, all of which are energy dependent. Combined with the typically steep source spectra, this leads to significant biases that need to be taken into account to correctly reconstruct energy-resolved polarization properties. In this paper, we present a method based on an iterative unfolding algorithm that makes it possible to simultaneously reconstruct the energy spectrum and the polarization properties as a function of true photon energy. We apply the method to a simulated X-Calibur data set and show that it is able to recover both the energy spectrum and the energy-dependent polarization fraction.     

Light scattering by complex particles in the Moon's exosphere: Toward a taxonomy of models for the realistic simulation of the scattering behavior of lunar dust

It is suspected that the lunar exosphere has a dusty component dispersed above the surface by various physical mechanisms. Most of the evidence for this phenomenon comes from observations of “lunar horizon glow” (LHG), which is thought to be produced by the scattering of sunlight by this exospheric dust. The characterization of exospheric dust populations at the Moon is key to furthering our understanding of fundamental surface processes, as well as a necessary requirement for the planning of future robotic and human exploration.We present a model to simulate the scattering of sunlight by complex lunar dust grains (i.e. grains that are non-spherical and can be inhomogeneous in composition) to be used in the interpretation of remote sensing data from current and future lunar missions. We numerically model lunar dust grains with several different morphologies and compositions and compute their individual scattering signatures using the Discrete Dipole Approximation (DDA). These scattering properties are then used in a radiative transfer code to simulate the light scattering due to a dust size distribution, as would likely be observed in the lunar exosphere at high altitudes 10's of km. We demonstrate the usefulness and relevance of our model by examining mode: irregular grains, aggregate of spherical monomers and spherical grains with nano-phase iron inclusions. We subsequently simulate the scattering by two grain size distributions (0.1 and radius), and show the results normalized per-grain. A similar methodology can also be applied to the analysis of the LHG observations, which are believed to be produced by scattering from larger dust grains within about a meter of the surface.As expected, significant differences in scattering properties are shown between the analyses employing the widely used Mie theory and our more realistic grain geometries. These differences include large variations in intensity as well as a positive polarization of scattered sunlight caused by non-spherical grains. Positive polarization occurs even when the grain size is small compared to the wavelength of incident sunlight, thus confirming that the interpretation of LHG based on Mie theory could lead to large errors in estimating the distribution and abundances of exospheric dust.     

Interpretation of the global anisotropy in the radio polarizations of cosmologically distant sources

We present a detailed statistical study of the observed anisotropy in radio polarizations from distant extragalactic objects. This anisotropy was earlier found by Birch (1982) and reconfirmed by Jain and Ralston (1999) in a larger data set. A very strong signal was seen after imposing the cut , whereRM is the rotation measure and its mean value. In this paper, we show that there are several indications that this anisotropy cannot be attributed to bias in the data. We also find that a generalized statistic shows a very strong signal in the entire data without imposing theRM dependent cut. Finally we argue that an anisotropic background pseudoscalar field can explain the observations.     

CCD imaging polarimetry of Comet 2P/Encke

We present results and analysis of imaging polarimetric observations of Comet 2P/Encke. The observations were carried out at the 2-m RCC telescope of the Bulgarian National Astronomical Observatory on December 13, 1993 and on January 14, 1994, at phase angles 51.1° and 80.5°, respectively. A wide-band red filter 6940/790 Å was used. This filter is transparent for the continuum and the weak emission bands of NH₂ and H₂O⁺. There is a sunward dust fan with well-defined polarization, which peaks at≈13% in the image obtained on January 14, 1994. Along the sunward fan the degree of polarization decreases progressively. Outside of the fan the coma displays a low polarization of ≈3%. We suggest that this low polarization is caused by the NH₂ emission in the pass-band of the red wide-band filter. Assuming a spherically symmetric NH₂ coma we are able to correct the observed polarization for this effect. The correction leads to an increase of the observed polarization by 1 to 4% at distances 10,000 and 1500 km from the nucleus. A rough estimate shows that the polarization in the near nucleus region of Comet Encke is similar to that for the dusty comets. Even after correction the polarization of Comet Encke's dust fan is significantly less that the polarization observed in dusty comets. The reasons influencing the distribution of dust polarization in the coma are discussed. More polarimetric and colorimetric observations of the dust in Comet Encke on its return in 2003 are needed.     

Brightness and Polarization Variations of S Per and T Per

Results of photoelectric BV observations of the brightness and polarization in the V band for S Per and T Per over a period of eight years are presented. An attempt is made to isolate the interstellar polarization. A comparison of the variations in the brightness and intrinsic polarization reveals some relationships among these quantities.     

The solution of the vector radiative transfer equation using the discrete ordinates technique: Selected applications

The paper is devoted to the presentation of a newly developed radiative transfer code SCIAPOL_1.0 for a plane-parallel turbid slab illuminated by the monodirectional wide beam. The SCIAPOL_1.0 is based on the discrete-ordinates solution of the vector radiative transfer equation.The code is applied to a number of problems, including studies of the applicability of the scalar approximation for the calculation of light reflectance from aerosols, clouds, and molecular atmospheres. We also study the accuracy of the single scattering approximation as applied to the calculation of light reflection from molecular and cloudy atmospheres and propose new approximations for the calculation of the reflection function and the degree of light polarization under unpolarized light illumination conditions.     

Polarization Observation Experiments for Radio Flares of Stars at the 6 cm Band

We have performed radio polarization observation experiments of the stars V772 Her and β Per with the Urumqi 25 m radio telescope at the 6 cm waveband, and obtained light curves of the stars after data processing and calibration. A radio ?are from the star V772 Her was detected on 2011 April 13. The degree of linear polarization of this ?are is about 30%, and the polarization angle is about 4°. We have detected also the slowly-varying component of the radio radiation from β Per, as well as a short ?are superposed on it, which has a very weak linear polarization.     

四川芦山MS7.0和汶川MS8.0地震前地电场变化研究

应用四川芦山M_S7.0和汶川M_S8.0震中周围部分地电场观测台站的资料,主要利用地电场波形比较和极化方位变化两种方法,并结合观测台站的工作日志,对两次地震前地电场观测资料进行了分析研究,并得出:芦山M_S7.0和汶川M_S8.0地震前部分台站地电场波形出现变异现象,主要表现为两种形式:日变波形的畸变(如盐源台和泸沽湖台)和相应时段地电场频谱特性出现变化,这些变异基本上出现在震前1~2个月内;利用两次地震前地电场观测的日均值计算了部分观测台站的地电场极化方位,发现在震前地电场的极化方位出现了大幅变化,最大变化幅度达160°,最小变化幅度也有10°;初步研究还发现,两次地震前夕,震中周围部分台站极化方位的正向或反向延长线,相汇集的区域与地震的震中有一定联系;对于研究所得结果,从地震电信号的产生机制和震源特性方面进行了尝试性理论解释.     

A_3钢在MgCl_2溶液中腐蚀行为研究

以MgCl2溶液模拟氯氧镁水泥孔隙液,研究了A3钢在MgCl2溶液中的腐蚀行为和腐蚀速率,并利用电化学测试仪对A3钢腐蚀过程的电化学特征进行了研究。实验结果表明,随着MgCl2浓度的减小以及在MgCl2溶液中浸泡时间的延长,A3钢的腐蚀失重速率逐渐变小;极化曲线测试与腐蚀失重试验结果相吻合;阻抗曲线(EIS)研究发现,随着A3钢在MgCl2溶液中浸泡时间的延长钝化膜的电阻变大;扫描电镜观察表明,经MgCl2溶液腐蚀后,在A3钢样品表面产生了许多腐蚀产物,XRD分析证实主要产物为Fe3O4和MgFe2O4。