大地电磁资料精细处理和二维反演解释技术研究(二)——反演数据极化模式选择

针对大地电磁二维反演中TE、TM极化模式的选择问题,设计了多个二维、三维模型进行了正演计算,从数据对比和反演结果对比两方面入手,分析研究了三维模型和二维模型响应数据的差异、反演中极化模式的选择、以及三维模型数据的二维反演近似等问题.研究结果表明:在三维模型条件下,利用二维模型进行反演时,TE模式对模型的二维的近似程度要求远高于TM模式;当三维结构影响较明显时,利用TM模式数据进行二维反演比利用TE模式或利用TE+TM模式联合反演都更合理,反演结果中的虚假结构明显减少;对于TM模式,相位受三维畸变影响较小,视电阻率较大,所以二维反演中可适当加大相位的权;对于实测数据的二维反演,应优先考虑采用TM模式数据进行二维反演,其次是TM+TE模式,一般不要单独采用TE模式.     

玉树地区地壳介质的各向异性特征

本文利用2010年5月7日到10月18日玉树地震震源区及其周边22个地震台站记录的2010年4月14日玉树地震余震数据资料,使用剪切波分裂分析方法初步得到了每一个台站的剪切波快波偏振方向和慢波时间延迟,并分析了玉树及周边地区地壳介质各向异性特征.在该研究区域,甘孜-玉树断裂上部分台站快波偏振方向近于东西向,这一结果与该区域的水平主压应力方向一致.甘孜-玉树断裂带南段玉树周边的台站快剪切波偏振方向为南东向,与断裂带的走向一致,显示了此次地震断裂走滑性质的特征.位于杂多断裂和清水河断裂上的台站及其附近的台站,快波偏振方向与所处的断裂走向基本一致,多为南东东向.各个台站的慢波延迟时间结果分布在4.23~7.01 ms/km范围内,平均慢波延迟时间是5.68 ms/km.在甘孜-玉树断裂带和乌兰乌拉湖-玉树南断裂相交的位置慢波延时总体较高;而低值区位于打贝通-小苏莽断裂的北西端与杂多断裂之间的位置.沿玉树断裂带,慢波延迟时间的梯度值较大,本文这一结果揭示了慢波延迟时间的分布和破裂带的走向、余震的分布有很大关系.     

偏振分析在地震信号检测中的应用

给出了一种3分量地震数据偏振分析的技术,并将其应用到人工地震勘探信号的提取中。该技术基于时域算法,通过对协方差矩阵的本征分析,在滑动时间窗内计算偏振特性,由偏振椭圆导出表征质点运动的各种属性,并利用质点运动的特征构建偏振滤波器。本文对3分量合成地震记录和野外探测实验的实际3分量记录进行偏振分析研究,并在此基础上进行偏振滤波,有效地提高了信噪比。     

平面平行大气中偏振辐射传输的数值计算

利用离散纵坐标(DISORT)法的基本原理,开发了平面平行大气中偏振辐射传输的数值计算模型,并利用解析插值原理实现了对任意天顶方向散射斯托克斯参量的求解.为检验计算模型的可靠性,分别针对分子和气溶胶散射大气进行了数值模拟,并与Coulson等1960年、Garcia等1989年的计算结果进行了比较.结果表明,模型计算结...     

Polarisation measurements with a CdTe pixel array detector for Laue hard X-ray focusing telescopes

Polarimetry is an area of high energy astrophysics which is still relatively unexplored, even though it is recognized that this type of measurement could drastically increase our knowledge of the physics and geometry of high energy sources. For this reason, in the context of the design of a Gamma-Ray Imager based on new hard-X and soft gamma ray focusing optics for the next ESA Cosmic Vision call for proposals (Cosmic Vision 2015-2025), it is important that this capability should be implemented in the principal on-board instrumentation. For the particular case of wide band-pass Laue optics we propose a focal plane based on a thick pixelated CdTe detector operating with high efficiency between 60–600keV. The high segmentation of this type of detector (1–2mm pixel size) and the good energy resolution (a few keV FWHM at 500keV) will allow high sensitivity polarisation measurements (a few % for a 10mCrab source in 10⁶s) to be performed. We have evaluated the modulation Q factors and minimum detectable polarisation through the use of Monte Carlo simulations (based on the GEANT 4 toolkit) for on and off-axis sources with power law emission spectra using the point spread function of a Laue lens in a feasible configuration.     

The Einstein polarization interferometer for cosmology (EPIC) and the millimeter-wave bolometric interferometer (MBI)

We provide an overview of a mission concept study underway for the Einstein Inflation Probe (EIP). Our study investigates the advantages and tradeoffs of using an interferometer (EPIC) for the mission. We also report on the status of the millimeter-wave bolometric interferometer (MBI), a ground-based pathfinder optimized for degree-scale CMB polarization measurements at 90 GHz.     

Polarimetric study of levitating dust aggregates with the PROGRA experiment

In order to interpret polarimetric remote observations of solar system dust clouds (e.g. cometary coma dust), laboratory measurements are needed. Three samples composed of aggregates are studied: crystallized enstatite, pyrogenic alumina and titanium oxide. The new version of the PROGRA² instrument allows to obtain polarimetric images of the samples under levitation. The dependence of polarization with phase angle and particle size is studied, as well as the effect of the porosity of the particles. Values of polarization at small phase angles are also discussed. The polarization near 90° decreases when the agglomerate size increases and when the porosity increases.     

The polarization-free approximation applied to multi-level non-LTE radiative transfer

The polarization-free (POF) approximation (Trujillo Bueno and Landi Degl'Innocenti, 1996) is capable of accounting for the approximate influence of the magnetic field on the statistical equilibrium, without actually solving the full Stokes vector radiative transfer equation. The method introduces the Zeeman splitting or broadening of the line absorption profile I in the scalar radiative transfer equation, but the coupling between Stokes I and the other Stokes parameters is neglected. The expected influence of the magnetic field is largest for strongly-split strong lines and the effect is greatly enhanced by gradients in the magnetic field strength. Formally the interaction with the other Stokes parameters may not be neglected for strongly-split strong lines, but it turns out that the error in Stokes I obtained through the POF approximation to a large extent cancels the neglect of interaction with the other Stokes parameters, so that the resulting line source functions and line opacities are more accurate than those obtained with the field-free approach. Although its merits have so far only been tested for a two-level atom, we apply the POF approximation to multi-level non-LTE radiative transfer problems on the premise that there is no essential difference between these two cases. Final verification of its validity in multi-level cases still awaits the completion of a non-LTE Stokes vector transfer code.For two realistic multi-level cases (CaII and MgI in the solar atmosphere) it is demonstrated that the POF method leads to small changes, with respect to the field-free method, in the line source functions and emergent Stokes vector profiles (much smaller than for a two-level atom). Real atoms are dominated by strong ultraviolet lines (only weakly split) and continua, and most lines with large magnetic splitting (in the red and the infrared) are at higher excitation energies, i.e. they are relatively weak and unable to produce significant changes in the statistical equilibrium. We find that it is generally unpredictable by how much the POF results will differ from the field-free results, so that it is nearly always necessary to confirm predictions by actual computations.The POF approximation provides more reliable results than the field-free approximation without significantly complicating the radiative transfer problem, i.e. without solving any extra equations and without excessive computational resource requirements, so that it is to be preferred over the field-free approximation.     

用斯托克斯轮廓推导太阳矢量磁场和热力学参量的三维结构

一种根据斯托克斯轮廓分析推导太阳矢量磁场和热力学参量的空间三维结构的新方法在本文中提出．在不考虑散射和原子偏振的假设下，该方法由三个具有不同功能的操作分别作用于太阳大气中一层或二层斯托克斯轮廓组成．这三个操作构成一个运行单元．将此单元运用到从表面到光球底层所划分的大气层格点，然后对扫描区所有的点应用同样的程序便可获得太阳上观察区的矢量磁场和热力学参量的空间三维结构．文中给出了相应的流程图和三个操作的详细描述，并用简化了的程序对理论轮廓进行了拟合．结果表明此方法能较满意地导出矢量磁场尤其是磁场强度的三维空间结构，而热力学参量结构的推导还需进一步改进．     

Dust coma of Comet C/1999 S4 (LINEAR): imaging polarimetry during nucleus disruption

Imaging and polarimetry of Comet C/1999 S4 (LINEAR) during its disruption provide information about the physical properties of the scattering dust particles, and some insight into the structure of the nucleus. A significant decrease in the brightness was noticed, together with a drastic change in the shape of the dust coma. The whole-coma polarization increased, which was typical of a comet with a near 27 percent maximum in polarization, the increase being comparable to previous observations for comets suffering a limited fragmentation. An important gradient in the intensity on the solar side corresponds to the ejected material. The degree of polarization in this region is higher than generally observed in jets and it increases with time as the nucleus (or its fragments) breaks up and ejects relatively large and compact particles. In the surrounding coma, these large particles are fragmented on short time-scales, indicated by the decrease of polarization. These results suggest that the fragile nucleus was not, as far as the physical properties of the dust are concerned, differentiated, and that it was possibly built of primordial cometesimals originating from the same formation region.