各向异性介质地震波场的优化褶积微分算子法数值模拟

在前人工作基础上,通过对窗函数参数进行优化实现了对基于Shannon奇异核理论的交错网格褶积微分算子的优化过程.应用这种优化褶积微分算子方法对各向异性介质进行了数值模拟,讨论了优化褶积微分算子法模拟的PML吸收边界条件以及稳定性条件,分析了弹性波在此类介质中的传播特征,并与高阶交错网格有限差分方法进行了对比.数值实验结果表明,该方法适用于各向异性介质中弹性波场模拟,精度高,稳定性好,是一种研究复杂介质中地震波传播的有效数值方法.     

双相介质地震波场数值模拟的迭积微分算子及其PML边界条件

将基于计算数学中Forsyte 广义正交多项式的迭积微分算子引入到地震波动方程的一阶速度--应力方程的空间微分运算中去,并采用时间错格有限差分算子替代传统的差分算子以匹配高精度的空间迭积微分算子,从而发展一种全新的地震波场正演模拟方法,来解决复杂非均匀介质模型中的波场传播问题.为了大幅衰减人工边界引起的反射,本文将完全匹配层(Perfectly Matched Layer,PML)吸收边界条件引入到所构建的方法中,以解决迭积微分算子法的边界问题.以二维波动方程为例,用迭积微分算子法实现了双相介质的地震波场正演模拟,模拟结果表明,双相介质模型较好地解释了含流体孔隙特性.同时也表明迭积微分算子法是一种非常实用、有效的数值模拟方法.     

声波与弹性波场数值模拟中的褶积微分算子法

基于富氏变换正反技术，分别讨论了各向同性声波与弹性波场模拟中的常规微分算子的设计方案，并将这些褶积微分算子分别应用于非均匀各向同性介质中声波与弹性波场模拟当中．为了更好地压制截断引起的吉谱斯效应，我们引入了汉宁窗．理论模型计算表明:这种褶积微分算子法具有快速，高精度且对计算机内存需求低的优点，是一项颇具潜力的高速、高保真的数字仿真技术．      

热层大气密度反演与建模研究进展

热层是位于地球表面大约90 km到近1 000 km的大气圈层,它与电离层和低层大气都存在着复杂的耦合关系;同时热层作为人类航天器空间活动的主要区域,其大气直接影响着各类低轨航天器的运行轨迹.近年来,热层大气观测资料的逐步增加推动了热层大气变化特性的研究和大气模式的发展.本文首先综述了基于多源卫星观测数据的热层大气密度反演算法.着重介绍了基于精密轨道数据以及加速度计数据反演密度的主要算法,以及各种反演策略的优缺点.总结了当前工程常用的MSIS、Jacchia以及DTM热层大气模式在数据源、算法实现过程及其适用范围等方面的异同.接着介绍了基于当前最新大气密度观测数据结合已有大气模式,应用多项式、稀疏矩阵拟合以及数据同化等技术的大气模式优化研究进展.最后概述了基于观测数据研究热层大气响应磁暴、耀斑以及日食等空间事件方面的科学进展.     

错格傅里叶伪谱微分算子在波场模拟中的应用

本文在传统傅里叶微分矩阵的基础上,对原始微分算子进行改进,引入了错格微分算子的傅里叶伪谱方法．尽管该方法增加了一些计算量,但却极大地提高了计算精度和稳定性．而且,该方法将微分计算过程由传统的傅里叶变换转换为一般的矩阵矢量乘积,大大降低了微分求解过程的复杂程度．在均匀介质中,将错格伪谱微分算子计算的结果和解析解进行比较,结果表明本文算子几乎达到了解析解的精度．而在分层均匀介质中的实验结果同时显示,该方法精度高、稳定性好,是一种研究层状介质中地震波传播的有效数值方法．     

地震波传播的微分几何描述

本文以复杂介质中的走向函数为基础,引入走时场的微分流形,从微分几何观点看,复杂介质中的射线方程即为流形上的测地线方程,复杂介质中的标量波动方程即为流形上的协变标量场方程,从而建立起复杂介质中地震波传播的微分几何描述,文中还讨论该方法在射线追踪,波场变换等方面的应用。     

粘弹性介质地震波传播的褶积微分算子法数值模拟研究

早期的褶积微分算子法都是基于正反傅立叶变换而实现的,其精度比四阶有限差分稍高。本文将计算数学中的Forsyte广义正交多项式微分算子与褶积算子相结合,构建了一个新的快速、高精度褶积微分算子,其计算结果非常接近实验函数微分的精确值,精度与l6阶有限差分相当。粘弹性波动方程更真实地描述了实际地下介质中弹性波的传播规律及其波场特征。本文以二维粘弹性波动方程为例,推导了粘弹性介质波动方程的离散格式,用迭积微分算子法实现了粘弹性介质的地震波场正演模拟,并对其波传播特征进行了分析。计算结果表明该算法能正确模拟粘弹性介质中的地震波,正确地反映粘弹性介质中波场的传播规律。     

基于辛格式离散奇异褶积微分算子的弹性波场模拟

本文发展了基于辛格式离散奇异褶积微分算子(SDSCD)的保结构方法模拟弹性波场,求解弹性波动方程时,引入辛差分格式进行时间离散,采用离散奇异褶积微分算子进行空间离散.相比于传统的伪谱方法,该方法提高了计算精度和稳定性.数值结果表明SDSCD方法可以有效地抑制数值频散,为解决大尺度、长时程地震波场模拟问题提供了合适的数值方法.     

2.5维地震波场褶积微分算子法数值模拟

早期的褶积微分算子都是基于正反傅立叶变换而实现的,其精度比四阶有限差分的精度稍高,本文将计算数学中的Forsyte广义正交多项式微分算子与褶积算子相结合,构建了一个新的快速、高精度褶积微分算子,其计算结果非常接近实验函数微分的精确值,精度与16阶有限差分的精度相当,远优于错格伪谱法的精确度.另外,2.5维数值模拟比二维模拟可以更真实地模拟三维介质的臬个剖面的波场,并且2.5维地震波模拟的计算量比三维模拟的计算量及计算耗时要大大减少.本文利用基于Forsyte广义正交多项式褶积微分算子法计算2.5维非均匀介质地震波场,模拟结果表明,该算法的计算速度快,计算精度高,能够直观、高效地反映复杂介质中波场的传播规律,并且2.5维波场数值模拟具有更高的计算效率,是一种非常值得深入研究并广泛应用的方法.     

应用分数阶微分对地震波稳恒Q值的时间域模拟

根据分数阶微分,在时间域应用新的模拟算法求解了Kjartansson的稳恒Q 值模型。在应力扩容公式中,代替2阶时间微分,Kjartansson的模型要求2γ阶的微分,这里γ为0<γ<1/2。应用Grunwald-Letnikov和中心差分近似计算了分数阶微分。对整阶微分,上述方法是标准算子的有限差分的拓广。模拟中应用了傅里叶方法计算空间微分,因此,可以处理复杂的几何问题。合成井间地震实验展示了这种新颖模拟算法的能力。     

Long-term thermospheric neutral wind observations over the northern polar cap

We study the solar dependence of the thermospheric dynamics based on more than 20 years Fabry–Perot interferometer O 6300 Å emission observation of polar cap thermospheric wind from three stations: Thule (76.53°N, 68.73°W, MLAT 86N), Eureka (80.06°N, 86.4°W, MLAT 89N), and Resolute (74.72°N, 94.98°W, MLAT 84N) in combination with the National Center for Atmospheric Research Thermosphere Ionosphere Electrodynamics General Circulation Model (NCAR-TIEGCM). All three stations showed a dominant diurnal oscillation in both the meridional and zonal components, which is a manifestation of anti-sunward thermospheric wind in the polar cap. The three-station observations and the TIEGCM simulation exhibit varying degree of correlations between the anti-sunward thermospheric wind and solar F10.7 index. The diurnal oscillation is stronger at Eureka (∼150 m/s) than that at Resolute (∼100 m/s) according to both observations and TIEGCM simulation. The semidiurnal oscillation is stronger at Resolute (∼20 m/s) than that at Eureka based (∼10 m/s) on data and model results. These results are consistent with a two-cell convection pattern in the polar cap thermospheric winds. The Thule results are less consistent between the model and observations. The simulated meridional wind diurnal and semidiurnal oscillations are stronger than those observed.     

A primitive equation,solar driven,perturbation model of the thermospheres of mars and venus

Abstract

A primitive equation, solar driven, thermospheric model is derived which has applications to the neutral gas components on Mars and Venus. The full effects of molecular viscosity and thermal conductivity are included, necessitating the development of a combined analytic and numerical solution technique. The model is applied to Venus in order to understand how thermospheric rotation, if present, would affect the dynamics. Results indicate that rotation periods of eight days or less should be observable. Application of the model to Mars indicates that the perturbation solar heating and the atmospheric response have primarily a diurnal component for which typical temperature and zonal wind maximum amplitudes are 20 K and 30 m/sec respectively. Because of uncertainty in the solar heating efficiency, calculations were made varying this parameter by an order of magnitude. The results imply that the response due to solar forcing alone is probably too small to account for observed concentrations of the minor constituents CO and O. An upper limit estimate is made of the upward propagation of wave energy from the lower atmosphere and the resulting response of the thermosphere.     

高层大气测风用地基F-P干涉仪的数值模拟

热层大气风场、温度场对热层-电离层耦合研究、热层环流特性研究以及太阳活动和地磁活动研究等有着重要意义,同时其也是航天器飞行环境预报的重要物理基础.目前,由于热层所处位置较高,大气非常稀薄,风场探测难度较大,因此针对热层大气风场的探测手段非常少.Fabry-Perot（FP）光学干涉仪可通过观测气辉来进行风场探测,其对成像系统像质要求不高,在设计中无需过分追求像质,已经成为热层风场测量的重要工具.由于风场观测气辉的辐射强度非常微弱,因此必须进行FP干涉仪测量系统优化,获得相对较强的辐射强度,以提高风场测量精度.但目前,对FP干涉仪系统优化方面的研究较少,且在测风误差评价方面的工作也不充实.本文通过热层测风用固定间距标准具地基FP干涉仪数值模型的建立,解决FP干涉仪设计过程中各参量的优化问题,并提出一种新的测风误差估算方法.数值模型结果分析表明,在目前探测器观测技术水平下,采用全部干涉环参与计算并结合像元合并技术进行风速反演可最大限度地提高测量精度.此外,由于气辉辐射强度是影响热层大气风场测量精度的重要因素,因此在仪器测风精度性能评价时需确定观测对象强度,即气辉的辐射强度.     

Comparison of ionospheric parameters calculated with UAM and measured at Voeykovo observatory

The measurements of the critical frequencies of the ionospheric F2 layer based on vertical radiosounding, which was performed with a CADI digital ionosonde at the Voeykovo magnetic–ionospheric observatory in February 2013, have been considered. The observations have been compared with the upper atmosphere numerical model (UAM) data for three days that differ in the amplitude and the character of solar and magnetic activity and correspond to quiet and moderately disturbed states of the ionosphere. The work was performed in order to improve the methods for determining the ionospheric state by vertical sounding ionograms. The time variations in the F2 layer critical frequency, electric field vector zonal component, and thermospheric wind velocity meridional component have been analyzed. Calculations were performed with three UAM variants. The UAM version providing the best agreement with the CADI ionosonde data was the version in which the neutral temperature, neutral composition, and pressure gradients are calculated according to the MSIS empirical model and the horizontal neutral wind velocity is determined by the equation of motion with pressure gradients from MSIS. The calculated values corresponded to the measurements, except those for the evening, because the electron density at the ionospheric F2 layer maximum depends more strongly on electric fields and thermospheric wind velocities during this period. Thus, the indicated UAM version with the above limitations can be used to determine the state of the subauroral ionosphere.     

Mechanisms of stratification of the <Emphasis Type="Italic">F</Emphasis>2 layer and formation of the <Emphasis Type="Italic">F</Emphasis>3 and <Emphasis Type="Italic">G</Emphasis> layers in the equatorial ionosphere

The paper is dedicated to the studies of formation mechanisms of additional layers in the equatorial ionosphere carried out using numerical simulations with use of the Global Self-Consistent Model of the Thermosphere, Ionosphere, and Protonosphere (GSM TIP) modified in the part of the solution of the electric field equation in the Earth’s ionosphere. Calculations were preformed for quiet geomagnetic conditions using the MSIS-90 model for the calculation of thermospheric parameters. The obtained spatio-temporal pattern of thermospheric circulation and the variations in the dynamo electric field obtained on its basis make it possible to reproduce the stratification effect of the F2 layer and the appearance of the F3 layer in the equatorial ionosphere due to the action of the nonuniform in height zonal electric field at the geomagnetic equator. On the basis of the earlier presented results of calculations using the modified GSM TIP model, the appearance of a maximum in the vertical profile of the electron density at a height of ∼1000 km formed by H+ ions, which we called the G layer, has been predicted. Numerical simulations showed that this layer is formed by the meridional component of the thermospheric wind and is related to the formation of the nighttime midlatitude maximum at heights of the ionospheric F region.     

热层风场的理论模拟与分析

通过求解中性大气Navier Stokes动量方程建立了一个时变的三维风场理论模式，利用目前新版的中性大气模式NRLMSISE 00及国际电离层参考模式IRI2000作为输入参数给出热层风场. 基于该模式，计算得到中等太阳活动年磁静日风场的变化形态及其受电场和离子曳力的影响. 同时，将Navier Stokes动量方程作不同形式的简化，并利用简化模式与本文的模式计算结果的对比，分析中性大气Navier Stokes动量方程中黏性项以及非线性项(U·Δ)U的作用. 结果表明，本文所建立伪三维风场模式给出的结果更为合理，而简化模式在某些地区尤其在低纬和赤道区不适用，黏性项及非线性项的作用不可忽略. 本文所建立的风场模式将对研究电离层动力学过程、电离层与热层的耦合过程以及空间天气学研究都有着重要意义.     

Motion of Ionospheric Plasma: Results of Observations above Kharkiv in Solar Cycle 24

The equipment and methodical characteristics of determining the vertical component of the ionospheric plasma motion velocity V_z based on an incoherent scatter radar of Institute of Ionosphere, National Academy of Sciences and Ministry of Education and Science of Ukraine (Kharkiv), which is the only radar of such type in Central Europe, are described. Based on the radar data, the patterns of altitude and diurnal variations in V_z near the maximum of solar cycle 24 for the typical geophysical conditions (around the summer and winter solstices, the spring and fall equinoxes) at low geomagnetic activity and the specifics of these changes during ionospheric storms are presented. The results of modeling of the dynamic processes in ionospheric plasma under the conditions of the undisturbed ionosphere, including the determination of altitudetime variations in the thermospheric wind velocity, are presented. It has been established that this velocity can significantly differ from the thermospheric wind velocity calculated by the known empirical global models. This difference is likely related to the regional features of thermospheric wind that are not shown in the global models.     

Gravity wave generation and propagation during geomagnetic storms over Kiruna (67.8°N, 20.4°E)

Atmospheric gravity waves, detected over Kiruna (67.8°N, 20.4°E) during geomagnetic storms, are presented and analysed. The data include direct measurements of the OI 630.0 nm emission line intensity, the x-component of the local geomagnetic field and thermospheric (meridional and zonal) wind velocities derived from the OI 630.0 nm Doppler shift observed with an imaging Fabry-Perot interferometer (IFPI). A low pass band filter technique was used to determine short-period variations in the thermospheric meridional wind velocities observed during geomagnetic storms. These short-period variations in the meridional wind velocities, which are identified as due to gravity waves, are compared to the corresponding variations observed in the OI 630.0 nm emission line intensity, x-component of the local geomagnetic field and the location of the auroral electrojet. A cross-correlation analysis was used to calculate the propagation velocities of the observed gravity waves.     

Equatorial Plasma Bubbles: Effect of Thermospheric Winds Modulated by DE3 Tidal Waves

A hypothesis about the effect of the tropospheric source on the longitudinal distributions of the equatorial plasma bubbles observed in the topside ionosphere was proposed earlier. It was supposed that this influence is transferred mainly by the thermospheric winds modulated by the DE3 tropospheric tidal waves. This conclusion was based on the discovered high degree correlation (R ? 0.79) between the variations of the longitudinal distribution of the plasma bubbles and the neutral atmospheric density. In this work, the hypothesis of the effect of the thermospheric tidal waves on the plasma bubbles at the stage of their generation is subjected to further verification. With this purpose, the longitudinal distributions of the frequency of the plasma bubble observations at the different ionospheric altitudes (~600 km, ROCSAT-1; ~1100 km, ISS-b) are analyzed; their principal similarity is revealed. Comparative analysis of these distributions with the longitudinal profile of the deviations of the zonal thermospheric wind (~400 km, CHAMP) modulated by the DE3 tidal wave is carried out; their considerable correlation (R ? 0.69) is revealed. We conclude that the longitudinal variations of the zonal wind associated with DE3 tidal waves can effect the longitudinal variations in the appearance frequency of the initial “seeding” perturbations, which further evolve into the plasma bubbles.     

垂直切变风场中声重波的Burgers-KdV方程研究

本文从可压缩流体的原始动力学方程出发,利用二维约化摄动方法推导出垂直切变风场中考虑曳引效应的二维声重波的Burgers-KdV方程,并对其非线性性态作了一些研究.主要结果:1.声重波在远场处能激发起孤波和多周期波列等非线性波动;2.给出上述非线性波动与大气背景风场、密度等的制约关系;3.进一步推测大气风剪切是E_s形成的可能机制.从本文推导出的方程出发,可进一步研究声重波远场处的相互作用、能量转换、不稳定性和定源等问题.