利用计算机断层成像方法由观测图像重建等离子体层全球密度分布——投影数据不完备问题

在用计算机断层成像方法由EUV观测图像重建等离子体层全球密度分布时,地球的遮挡和有限角度都会导致投影数据不完备,从而无法精确重建出等离子体层的密度分布.本文针对该问题,提出一种基于图像总变差极小化的代数迭代算法.通过重建等离子体层投影数据缺失最为严重的中心子午面,证明该算法能够显著提高重建图像的质量. 并且在IMAGE卫星仅能达到90°的有限投影角度下,此算法重建图像的相关系数可达0.760,而代数迭代算法的相关系数仅为0.696.     

多视角投影重建算法综述

本文主要论述了多视角投影重建的主要方法和思路.多视角问题是不完全投影数据重建的一个特例,也就是投影角度数远小于正常投影角度数的重建问题,比如正常投影数的十分之一或者二十分之一,所以也被称作稀松投影或者少量投影重建问题.由于问题的相似性,一些多视角投影重建的方法和思路来源于有限角度投影重建问题.多视角投影重建断层图像的算法主要有两种思路:一是基于投影数据恢复的方法,如通过插值、空间变换迭代等方法补全投影数据,另一种是通过在迭代过程对重建的图像加以限制,如先验条件、TV约束等.     

利用IMAGE卫星观测数据重建地球等离子体层的磁赤道面分布

美国利用IMAGE卫星的极紫外辐射（EUV）探测器对地球等离子体层进行了连续5年的遥感成像观测。由于IMAGE卫星数据是沿观测路径上的积分投影数据,并且存在地球“遮挡”、“阴影”、“数据缺失”等问题,无法直接利用传统的CT方法对等离子体层进行三维重建。本文利用地球磁场模型,基于地球等离子体层的物理性质,建立一个联系地球磁赤道面密度与投影数据的EUV成像模型,实现了从单个角度的EUV观测图像进行地球等离子层三维重构的方法。      

多层CT重建算法对比研究

目前多层CT的重建算法主要有基于FDK的三维滤波反投影算法以及基于多层投影数据重排的二维FBP重建算法。本文对传统的FDK算法、基于投影角度二维/三维加权的CB-FBP算法以及自适应轴向插值AAI-FBP算法的性能进行了对比实验,并对实验数据进行了细致地分析。实验结果表明:在这几种重建算法中,AAI-FBP算法对于多层CT的重建效果最好,这对于后续多层CT重建算法的改进以及临床应用研究提供了可靠的实验依据。     

基于模型融合的有限角度CT迭代重建方法

针对有限角度扫描的CT重建,提出一种基于模型融合的CT迭代重建方法。模型来源于患者的早期Dicom图像。对扫描角度有限的投影数据,用统计迭代算法进行初步重建,得到预重建图像;将预重建图像与模型进行融合,得到融合图像;然后再次投影,补全原始投影缺失的部分,根据补全的投影数据重建出中间结果,之后重复投影、融合、重建过程直到满足终止条件。仿真实验表明,该算法能完整重建整个目标,在有效保留原目标特征的同时提高了小角度投影数据重建的质量。     

切向CT重建算法的研究

在工业CT的检测过程中,由于各种原因可能造成投影数据的不完备.在这种情况下,直接利用传统的解析重建方法(FBP)或者统计重建方法(EM)都不能给出理想的重建结果,从切向CT扫描方式获得的就是典型的不完备投影数据.本文利用迭代算法来改善重建图像的质量,首先通过已有的投影数据合理估计缺失的投影数据,并通过不断的迭代来改善这种估计,从而使得重建图像不断逼近真实物体.     

基于投影域数据恢复的低剂量CT稀疏角度重建

针对目前CT的X射线电离辐射危害,提出了一种基于低剂量CT投影数据进行稀疏角度重建的方法来降低辐射剂量。本方法首先对低剂量CT的投影数据采用惩罚加权最小二乘(PWLS)方法进行去噪处理,然后对去噪后的投影数据进行稀疏角度的CT图像重建。对Shepp-Logan模体仿真实验及真实实验数据重建结果表明:本文提出的基于低剂量CT的稀疏重建方法可有效地抑制重建图像噪声和条形伪影,实现稀疏角度的低剂量CT图像重建。     

一种基于频域外推的不完全角度CT重建算法

不完全角度重建问题一直是CT图像重建领域研究的重点和难点。目前,通常的不完全角度重建方法是基于空域的迭代方法,但由于正反投影的高计算复杂度,空域迭代方法存在计算耗时,对硬件资源需求大等问题。本文提出了一种基于外推的邻近网格迭代算法（INNG-TV）。首先,平行束采样的数据通过傅里叶变换和样条插值到频域空间,然后在迭代的过程中,傅立叶空间投影已知部分的数据始终不变,缺失部分数据通过对重建图像进行INNG外推得到,同时在图像空间对重建图像做非负、最小化总变分等先验及优化约束。     

图象分块重建算法

本文提出一种图象分块重建算法,通过对投影空间、卷积投影空间、图象空间的分割,实施分块重建运算.适合于多台微机进行并行图象重建,为构造廉价的普及型 CT 提供了一种可能途径.     

一种基于数据外插改进的ART迭代算法

本文针对有限角度的投影数据的CT图像重建问题,提出了一种基于数据外插改进的ART算法.该算法的基本思想足运用已知角度的投影数据来补全未知角度的投影数据,再用ART算法进行图像重建.最后用模拟的投影数据进行了重建图像的数值实验.实验结果表明该算法不但提高了重建图像质量,同时也提高了图像达代的收敛速度.     

Modeling of properties of the plasmasphere under quiet and disturbed conditions

Based on theoretical models of the ionosphere and the plasmasphere, the ion composition variations in the plasmasphere and the plasmapause structure were studied depending on the choice of the distribution model of the magnetospheric convection electric field at low and high geomagnetic activity at the equinox and the December solstice. Based on the model calculations performed, the plasmapause shape and size during an increase and decrease in geomagnetic activity were studied. It was revealed that the size of the plasmasphere mainly depends on the magnetic local time (MLT) sector and the level of geomagnetic activity, and it greatly depends on the maximum universal time during the equinox. The Earth’s plasmasphere asymmetry is manifested in the noon-midnight and morning-evening directions. The analysis results of daily and seasonal variations in the ionic composition of the Earth’s plasmasphere at a moderate solar activity level show that there is a certain increase in the ion concentrations of H⁺ and He⁺ in the winter period probably due to an increase in the exospheric density at the summer to winter transition. The data obtained are in good agreement with satellite observations which makes it possible to use the model proposed to study the plasmasphere under different geophysical conditions.     

Restoration of the proton density distribution in the Earth’s plasmasphere from measurements along the INTERBALL-1 satellite orbit

Based on experimental data obtained in 1995?C2000 on board the INTERBALL-1 spacecraft using the ALPHA-3 instrument, a semi-empirical two-dimensional model of the Earth plasmasphere is developed, which allows for the plasma distribution in the entire meridional plane to be restored from the temperature and proton density measurements along the satellite orbit. The model has also been tested using the data of the IMAGE spacecraft. The model uses theoretical expressions (Lemaire and Schere, 1974) that describe the plasma distribution in the plasmasphere for the cases of thermal equilibrium and collisionless initial partial filling of plasmaspheric shells; therefore, the parameters of the constructed model have a clear physical meaning and make it possible, in particular, to estimate the degree of plasmasphere filling.     

磁宁静期核心等离子体层电子密度分布的统计研究

等离子体层已有数十年研究历史,但对其核心等离子体区域却一直没有一个相对准确的界限和模型定义.基于范阿伦辐射带卫星RBSP-A在2012年9月18日至2014年10月13日约两年的观测,我们统计研究了磁宁静期间核心等离子体层电子密度随磁地方时(MLT)及磁壳指数(L-value)的分布特征.发现了核心等离子体层电子密度在不同MLT条件下随L值的变化趋势几乎一致,但与以前的等离子体层经验模式计算的电子密度存在较大的偏差.在不同L值下电子密度随MLT的变化趋势也相差不大,而且随MLT存在明显的逐日和半日变化.最后我们获得了等离子体层电子密度随L值和MLT变化的经验公式.研究结果对空间等离子体层建模及研究具有重要的意义.     

顶部电离层和等离子体层电子密度分布——基于GRACE星载GPS信标测量的CT反演

本文利用两颗跟飞的GRACE卫星载GPS信标测量数据和基于差分相对TEC的层析算法,实现了全球范围的顶部电离层和等离子体层(450~5000 km) 层析成像.反演结果表明,利用低轨道卫星载GPS信标测量数据可以有效地重建顶部电离层和等离子体层的全球二维分布图像.对不同地磁活动条件下的天基层析反演结果表明,等离子体层电子密度随纬度的分布是不均匀的;在低纬赤道带,从顶部电离层向上延伸直到等离子体层,以及等离子体层中局地的电离增强云团,经常出现近似垂直于磁力线的电子密度柱状增强结构.     

Use of the physically based modeling to choose an adequate method for determining the plasmapause position

From the data on the cold plasma measurements onboard the INTERBALL-1 spacecraft (1995–2000), the plasmapause positions determined from the most frequently used formal criterion—a fivefold or higher decrease in plasma density with an increase in the L-shell by 0.5—and visually from the measured energy spectra of thermal protons have been analyzed and compared. The difference in the results of the both empiric techniques makes it possible to estimate the thickness of the boundary layer of the plasmasphere. The model of the Earth’s plasmasphere developed earlier by the authors (Verigin et al., 2012; Kotova et al., 2015) based on the theoretical expressions makes it possible to reconstruct the plasma distribution throughout the plasmasphere from the measurements along a single pass of the orbiter and to find the plasmapause position defined as the last closed stream line. Comparison of the plasmapause position obtained with empirical techniques to the position of this boundary calculated with physically based models of the plasma distribution in the plasmasphere has shown that the modeled position of the plasmapause approximately coincides with that determined from the formal criterion described above.     

Comparison of the measured and modelled electron densities and temperatures in the ionosphere and plasmasphere during 20/30 January, 1993

We present a comparison of the electron density and temperature behaviour in the ionosphere and plasmasphere measured by the Millstone Hill incoherent-scatter radar and the instruments on board of the EXOS-D satellite with numerical model calculations from a time-dependent mathematical model of the Earths ionosphere and plasmasphere during the geomagnetically quiet and storm period on 20/30 January, 1993. We have evaluated the value of the additional heating rate that should be added to the normal photoelectron heating in the electron energy equation in the daytime plasmasphere region above 5000 km along the magnetic field line to explain the high electron temperature measured by the instruments on board of the EXOS-D satellite within the Millstone Hill magnetic field flux tube in the Northern Hemisphere. The additional heating brings the measured and modelled electron temperatures into agreement in the plasmasphere and into very large disagreement in the ionosphere if the classical electron heat flux along magnetic field line is used in the model. A new approach, based on a new effective electron thermal conductivity coefficient along the magnetic field line, is presented to model the electron temperature in the ionosphere and plasmasphere. This new approach leads to a heat flux which is less than that given by the classical Spitzer-Harm theory. The evaluated additional heating of electrons in the plasmasphere and the decrease of the thermal conductivity in the topside ionosphere and the greater part of the plasmasphere found for the first time here allow the model to accurately reproduce the electron temperatures observed by the instruments on board the EXOS-D satellite in the plasmasphere and the Millstone Hill incoherent-scatter radar in the ionosphere. The effects of the daytime additional plasmaspheric heating of electrons on the electron temperature and density are small at the F-region altitudes if the modified electron heat flux is used. The deviations from the Boltzmann distribution for the first five vibrational levels of N₂(v) and O₂(v) were calculated. The present study suggests that these deviations are not significant at the first vibrational levels of N₂ and O₂ and the second level of O₂, and the calculated distributions of N₂(v) and O₂(v) are highly non-Boltzmann at vibrational levels v > 2. The resulting effect of N₂(v > 0) and O₂(v > 0) on NmF2 is the decrease of the calculated daytime NmF2 up to a factor of 1.5. The modelled electron temperature is very sensitive to the electron density, and this decrease in electron density results in the increase of the calculated daytime electron temperature up to about 580 K at the F2 peak altitude giving closer agreement between the measured and modelled electron temperatures. Both the daytime and night-time densities are not reproduced by the model without N₂(v > 0) and O₂(v > 0), and inclusion of vibrationally excited N₂ and O₂ brings the model and data into better agreement.     

利用计算机断层成像方法由观测图像重建等离子体层全球密度分布——地球遮挡问题

本文是利用计算机断层成像(CT)方法中的滤波反投影法(FBP)和代数迭代法(ART),根据等离子体层的仿真模型,重建其全球密度分布.在重建过程中,地球遮挡是一个很重要的问题.计算结果表明两种方法都可以使用,但ART比FBP重建的效果好.ART重建图像的相关系数可达0.98,而FBP重建图像的相关系数仅为0.86.FBP重建的偏差是由地球遮挡引起,向阳面靠近地球区域的密度会减小.从定量分析中可以进一步看出地球遮挡所引起的偏差变化.     

Mathematical modeling of nighttime enhanced electron density regions in the Earth’s ionospheric <Emphasis Type="Italic">F</Emphasis>2 layer and plasmasphere

A mathematical modeling method and the global numerical model of the Earth’s upper atmosphere were used to study nighttime enhanced electron density regions (EEDRs) in the ionospheric F2 layer and their possible manifestations at altitudes of the Earth’s plasmasphere. It has been established that EEDRs are formed owing to latitudinally nonuniform longitudinal (along the magnetic field) plasma flows from the plasmasphere into the nighttime ionosphere and the wind transport of ions along geomagnetic field lines. The specific features of the effect of ionospheric-plasmaspheric plasma transport processes, related to their three-dimensional character, on EEDRs have been revealed.