地磁偏角测量GPS基准点误差分析

从地磁偏角测量原理与方法入手,针对GPS基准点选取不同对地磁偏角观测带来的影响进行误差模型构建和相关误差分析,绘制地磁偏角误差随GPS基线长度变化曲线图,根据误差模型实例分析评估结果,得到地磁偏角实测GPS基准点设定的误差变化规律与GPS设点方法,根据此方法可以有效控制GPS基准点误差落在预定的误差区间内,使地磁偏角观测满足规范的精度要求。     

海面之上法中海面反射率和观测几何模拟研究

测量离水辐亮度的水面之上测量方法中最大的不确定性因素是太阳耀斑的污染和海面反射率的估算。文章根据Cox和Munk研究结果,利用大量随机数模拟海面波浪倾斜,估算不同仪器观测方向与风矢量几何以及不同仪器视场角下的海面反射率,并估算出不同太阳天顶角及相对风矢量方位角的太阳耀斑基本分布。     

基于太阳角度的全自动海洋光谱采集控制系统研究

针对海洋水色反演进行人工光谱采集时所存在的采集不连续、数据量少、覆盖海域面积小等问题,研究完成了一种基于太阳角度的全自动海洋光谱采集控制系统。该系统利用数据采集接收模块接收的位置、时间、角度信息进行太阳角度的精准计算,依据得到的太阳角度实时自动调整仪器观测平面的位置和光纤探头的指向角度,并根据光谱采集要求自动控制光纤探头转动,实现对天空光下行辐亮度、参考板上行辐亮度和海水上行辐亮度的采集,实现了海洋光谱采集的全自动控制。仿真分析了中国近海海域太阳方位角的变化情况,得到了中国近海海域太阳方位角的变化规律,保证了仪器观测平面位置调整的时效性和准确性。     

HY-1C卫星影像中太阳耀斑区域的预测技术研究

对卫星影像太阳耀斑区域的预测是保障船-星同步观测有效实施的基础性工作。本文在对HY-1C卫星影像各像元观测几何分析的基础上,简化构建卫星影像各像元的网格化模型,介绍了利用卫星轨道报估算的卫星-太阳-像元位置的观测几何,进而估算卫星影像中太阳耀斑区域的技术方法。经与HY-1C实际卫星影像的应用比对,表明本文预测的像元位置、太阳位置以及卫星观测天底角/方位角均与实际影像数据具有很好的重合度,预测的太阳耀斑区域与实际影像耀斑掩码区重合度良好,验证了该方法能够预测影像中太阳耀斑区域,保障船-星同步观测的能力。     

射向标定测量中角度平差方法探讨

射向标定测量只需要提供方位角成果,为了消除测距误差对方位角的影响,在数据处理时只对观测水平角进行平差。比较各种平差方法,并通过实例分析得出,对观测水平角进行间接平差最为方便实用。对多次实测数据进行统计,通过闭合差估计出:射向标定测量中测角中误差为1″左右,基准方位角的精度水平在1.2″左右。     

海岛礁磁偏角测量原理与方法

如何在海岛礁上进行地磁测量是当前海洋测量领域面临的技术难题。基于较为成熟的陆上流动地磁测量模式,结合海岛礁磁偏角测量的特殊性,提出了较完整的海岛礁磁偏角测量技术流程,包括工作原理、测量仪器、数据采集和处理过程、指标要求等关键环节,初步构建了海岛礁地磁测量技术基础框架。     

GMI亮温资料RFI信号影响因子分析

利用全球降水测量(Global Precipitation Measurement,GPM)卫星上搭载的微波成像仪(GPM Microwave Imager,GMI)的一级亮温数据,通过谱差法识别被无线电频率干扰(radio frequency interference,RFI)污染的典型陆地地区,确定欧洲、东亚和南美作为主要研究区域,进一步分析RFI与卫星方位角、太阳方位角和太阳天顶角之间的关系,讨论RFI的影响因子。结果表明:水平极化方式下受RFI影响的区域范围比垂直极化方式下的范围更广;相对于强RFI信号分布对应的较宽的卫星方位角区间,存在RFI的像素点对应的太阳方位角和太阳天顶角角度区间范围较为集中;当RFI强度较弱时,垂直极化方式下的RFI的像素点远多于水平极化方式下的RFI像素点,但随着RFI强度的增强,水平极化方式下的RFI像素点多于垂直极化方式下的RFI像素点,且强度越大则两种极化方式下的RFI像素点数量差距越大。     

基于方位/多径时延的水下目标运动参数估计

讨论了基于方位角、俯仰角及多径时延 TMA 的水下目标运动参数估计方法。采用声基阵测量水下运动目标相对于观测平台的方位角、俯仰角,并测量水下目标的一次水面反射相对于直达波的多径时延差, 根据水下目标方位角、俯仰角与多径时延差的变化,通过目标运动分析(TMA)方法预测目标的航迹、航速及航向,为攻击水下目标提供决策信息。计算机仿真验证了方法的可行性。     

中国海区磁偏角查询与显示应用系统的设计与实现

基于高密度、高精度的实际测量数据,建立了中国海区地磁基本场数学模型,研制开发了中国海区磁偏角查询与显示应用系统,从根本上改变了只能从外版图件上手工量取磁偏角获取数据的现状。对保证船舶安全航行和保障装备的安全运行有着重大意义。     

基于MISR多角度光学遥感影像的海面风速估算实验

太阳耀光是来自粗糙海面的直接太阳反射光,其强度与海面粗糙度密切相关,而海面粗糙度主要受海面风场影响。因此,包含太阳耀光信息的光学遥感影像在海洋动力过程和海面风速探测中具有积极意义。本文利用2016年2月到2017年3月期间成像的25幅Terra卫星MISR(Multi-angle Imaging Spectro Radiometer)传感器的多角度遥感影像,分别提取了太阳的高度角和方位角、正视和后视影像的卫星观测角、方位角等信息,校正获得正视和后视影像的太阳耀光辐射强度,进一步反演海表面粗糙度信息,进而计算海面风速。最后利用ECMWF(European Centre for Medium-Range Weather Forecasts)的模式风速数据与反演获得的风速结果进行对比验证。结果表明,两者的相关系数较高(R=0.745),均方根误差和平均绝对偏差值分别为1.514 m·s^-1和1.319 m·s^-1。初步实验结果表明,利用MISR多角度光学遥感影像估算海表面风速是可行性的。     

Geomagnetic Models and Edge Recognition of Hydrothermal Sulfide Deposits at Mid-ocean Ridges

Near-bottom magnetic prospecting is considered to be an efficient method for investigating inactive hydrothermal areas and the study of the spatial structure of hydrothermal systems. Furthermore, geophysical forward modeling is widely used to simulate the anomalous characteristics of geological bodies. To understand the magnetic and magnetic structure features of hydrothermal sulfide deposits at mid-ocean ridges, we built 3D forward models for both mafic- and ultramafic-hosted hydrothermal sulfide deposits to simulate the near-bottom magnetic field. Our modeling results showed a low amplitude magnetic anomaly above the mafic-hosted hydrothermal sulfide deposits, and a high amplitude magnetic anomaly above the ultramafic-hosted deposits. These features allow us to identify and classify the host rocks of hydrothermal sulfide deposits. Moreover, we can recognize the edge of the magnetic anomalies using the intensity of the spatial differential vector method, considering variables such as the width of the alteration zone, the height of the observation platform, and the magnetic inclination and declination. Therefore, we propose the intensity of the spatial differential vector method as an effective approach to define the boundaries of hydrothermal sulfide deposits.     

Magnetohydrodynamic models of the upper atmosphere of Earth and some applications thereof

The earlier developed monotonous conservative variant of a net-characteristic method of the second- and third-order approximation based on 3D equations of magnetic gasodynamics with consideration for the magnetic field diffusion is expanded for the solution of dynamic problems on the flow of the upper atmosphere of the Earth by solar plasma. It is modified, which results in support for the solenoidality of the magnetic field and the removal of the magnetic charge. Calculations are carried out and preliminary results of using software complexes to simulate the passage of the leading edge of solar plasma through the upper atmosphere of the Earth are given. Unlike existing studies in this direction, the dynamics of the passage of the leading edge upon a strong burst in the intensity of solar wind over the entire altitude range from the surface of the Earth to the upper magnetosphere is considered.     

Studies on sedimentary events in Mariana Trough and characteristics of geomagnetic field change

Ｓｔｕｄｉｅｓ　ｏｎ　ｓｅｄｉｍｅｎｔａｒｙ　ｅｖｅｎｔｓ　ｉｎ　Ｍａｒｉａｎａ　Ｔｒｏｕｇｈ　ａｎｄ　ｃｈａｒａｃｔｅｒｉｓｔｉｃｓ　ｏｆ　ｇｅｏｍａｇｎｅｔｉｃ　ｆｉｅｌｄ　ｃｈａｎｇｅＣｏｎｇＹｏｕｚｉ；ＨａｎＧｕｏｚｈｏｎｇ；ＣｈｅｎｇＧｕｏ...     

船载海水温度观测研究

通过研究国家相关海洋观测标准对海水温度观测的规约,结合当前船载水温观测的现状,提出了基于总线的船载磁吸附温度链式观测方法,并对其在结构设计、理论模型、算法等多方面进行了阐述.通过多个竖直分布的温度传感器实时观测,采用自适应参数化算法,有效减少了风浪、海流、热辐射等方面的影响,具有观测层深相对固定、精度高等特点,可实现船...     

船载表层水温观测研究

通过研究国家相关海洋观测标准对海水温度观测的规约,结合当前船载水温观测的现状,提出了基于总线的船载磁吸附温度链式观测方法,并对其在结构设计、理论模型、算法等多方面进行了阐述。本方法通过多个竖直分布的温度传感器实时观测,采用自适应参数化算法,有效减少了风浪、海流、热辐射等方面的影响,具有观测层深相对固定、精度高等特点,可实现船载全航次的自动观测。同时,设计制造了相关的模拟实验装置进行现场实验,验证了船载磁吸附温度链式观测方法的可行性和有效性。     

利用北斗多频观测进行舰船姿态测量

讨论了利用北斗二代卫星定位系统进行舰船姿态测量的可行性,并利用多频观测进行电离层折射误差的消除;使用TCAR和矩阵变换法进行模糊度的解算;最后利用姿态矩阵的正交特性进行模糊度有效性的分析。经仿真计算可知,利用北斗多频观测进行舰船姿态测量具有很高的精度和效率。     

Solar and interplanetary sources of geomagnetic storms: Space weather aspects

The current notions of the solar-terrestrial relations responsible for the transport of solar disturbances and for the generation of magnetic storms on the Earth are briefly reviewed. The probability of generating magnetic storms by different solar and interplanetary phenomena is quantitatively estimated. The efficiencies of generating magnetic storms by different types of solar wind streams are compared.     

Prediction of the total cycle 24 of solar activity by several autoregressive methods and by the precursor method

As follows from the statement of the Third Official Solar Cycle 24 Prediction Panel created by the National Aeronautics and Space Administration (NASA), the National Oceanic and Atmospheric Administration (NOAA), and the International Space Environment Service (ISES) based on the results of an analysis of many solar cycle 24 predictions, there has been no consensus on the amplitude and time of the maximum. There are two different scenarios: 90 units and August 2012 or 140 units and October 2011. The aim of our study is to revise the solar cycle 24 predictions by a comparative analysis of data obtained by three different methods: the singular spectral method, the nonlinear neural-based method, and the precursor method. As a precursor for solar cycle 24, we used the dynamics of the solar magnetic fields forming solar spots with Wolf numbers Rz. According to the prediction on the basis of the neural-based approach, it was established that the maximum of solar cycle 24 is expected to be 70. The precursor method predicted 50 units for the amplitude and April of 2012 for the time of the maximum. In view of the fact that the data used in the precursor method were averaged over 4.4 years, the amplitude of the maximum can be 20–30% larger (i.e., around 60–70 units), which is close to the values predicted by the neural-based method. The protracted minimum of solar cycle 23 and predicted low values of the maximum of solar cycle 24 are reminiscent of the historical Dalton minimum.