GPS掩星大气探测中弯曲角电离层残差仿真研究

介绍GPS掩星技术在气候监测和数值天气预报中的应用及其电离层误差改正的研究现状。弯曲角双频线性组合电离层改正法是目前应用最广泛的掩星电离层误差改正方法,而对弯曲角电离层残余误差鲜有研究。本文用MSIS90大气模式和3DNeUoG电离层模式模拟背景大气,用射线追踪法初步仿真研究了弯曲角电离层残差。研究表明:弯曲角电离层残差随太阳活动强度增加而增大;北半球中纬度夏天午后掩星事件的弯曲角电离层残差可达到1.8 urad。     

电离层延迟高阶项对GPS精密单点定位精度影响分析

随着GPS卫星轨道、钟差及各种误差修正模型的不断精化,静态精密单点定位(PPP)定位精度达到mm级,进行电离层延迟高阶项较小量级的误差改正研究,对改进PPP数据处理策略具有重要的参考价值。本文利用分布在不同地理纬度的5个IGS跟踪站3天的观测数据,对比分析了电离层延迟二阶项、三阶项对GPS观测值精度及静态PPP定位精度的影响。分析结果表明,电离层延迟二阶项、三阶项对GPS观测值精度的影响分别为cm级和mm级,对低纬度地区PPP定位精度的影响大于3 mm,但对中高纬度的测站观测值、定位精度的影响比低纬度地区小很多。      

电离层干扰对GPS掩星弯曲角和温度精度的影响

以MSIS90大气模式和3DNeUoG电离层模式为背景大气,仿真模拟了电离层暴、电离层行扰和电离层槽对GPS掩星弯曲角电离层残差及温度精度的影响。结果表明,在太阳活动活跃期,弯曲角电离层残差在35~50km高度范围内可达1.5μrad,其标准差可达0.9μrad;在15~35km高度范围内可达4μrad,其标准差可达1.4μrad。电离层暴和电离层槽可使弯曲角电离层残差标准差增大20多倍;电离层行扰可使弯曲角电离层残差标准差增大数倍。电离层干扰引起的电离层残差可使15~35km高度范围内温度反演误差高达8K,这样的温度误差会对掩星观测的日平均温度和月平均温度产生显著影响。因此,需要发展新的电离层修正方法;在掩星气候监测中,需加强电离层监测,并结合监测结果剔除电离层干扰误差。     

2011年电离层和太阳活动指数的准21.5天振荡分析

利用傅里叶变换,对2011年电离层总电子含量、太阳黑子相对数、太阳远紫外线0.1~50 nm波段和26~34 nm波段辐射数据、地磁场Kp指数和Dst指数进行功率谱分析,研究了2011年日地空间的准27 d周期振荡。发现在电离层和太阳活动指数中存在偏离27 d的21.5 d准周期振荡,同一时间内地磁活动指数没有发现这一现象,推断这可能是由太阳活动区演变引起的。对近几个太阳活动周的分析表明,21~23 d的准周期信号会在太阳活动上升期重复出现。利用太阳中央子午线左右[-10°,10°]经度范围内的太阳活动区面积,进一步证实2011年地球电离层和太阳指数数据中的21.5 d准周期振动可能是太阳活动区的演变与太阳较差自转的综合影响。利用全球电离层格网数据,研究了地球电离层准27 d周期振荡的全球分布。     

GNSS／LEO无线电掩星电离层探测仿真研究

无线电掩星是实现全球电离层探测的重要手段之一。针对GNSS／LEO掩星探测电离层的特点,基于电离层掩星的判决条件,通过NeQuick模型实现了电波弯曲角和绝对总电子含量的数据仿真,利用阿贝尔变换法（Abel Transform）和穿刺法实现了电离层电子密度剖面的有效反演,统计分析结果验证了NeQuick模型用于GNSS／LEO无线电掩星电离层探测仿真的可行性。     

不同电离层映射函数对导航精度的影响分析

介绍广播星历映射函数、投影映射函数、几何映射函数和椭球映射函数4种不同的电离层映射函数,基于Klobuchar电离层模型分析不同电离层映射函数对导航精度的影响。结果表明,不同电离层映射函数对导航精度的影响在厘米级到分米级;在不同太阳活动期,椭球映射函数和几何映射函数对导航精度影响基本相同;在太阳活动活跃期,导航精度由高到低依次为几何映射函数、投影映射函数、广播星历映射函数;在太阳活动平稳期,导航精度由高到低依次为广播星历映射函数、投影映射函数、几何映射函数。建议在导航定位中,电离层映射函数在太阳活动活跃期时采用几何映射函数,在太阳活动低谷期时采用广播星历映射函数。     

(二)北级星方位角表

北半球地区一般都采用北极星测定方位角,这是因为：（1）北极星的北极距不到1°,它是一颗不落星,总在地平之上,因而可以最大限度地利用它;（2）北极星的亮度适宜,易于辨认;（3）根据恒星时角法测定方位角的理论研究,所观测的恒星越是靠近北极,它的方位角越是靠近0°或180°,测站经、纬度的误差对所求方位角的影响越小;北极星不仅是靠近北极,它的方位角在任何时刻都是很小的,最大也不超过1°×secψ（ψ是测站纬度）。     

基于多源数据的电离层异常监测及GNSS影响效应研究

电离层是日地空间环境的重要组成部分,电离层异常对无线电通讯和人类空间活动的影响不容忽视.电离层异常监测,在高精度GNSS PNT 服务与深空探测误差修正、空间天气预报预警及日地空间环境动态监测等方面具有重要科学意义和实用价值.海量地基、天基多源电离层观测数据,为电离层异常监测及电离层精细化时空变化反演提供了丰富的数据源.论文利用全球约250个Multi-GNSS站和COSMIC掩星观测数据,采用并行计算10 m in内实现全球数据处理,近实时构建了三维电子密度模型,融合掩星数据使得海洋地区的精度明显改善;搭建了天地联合多源电离层观测数据融合处理试验平台,在线提供近实时三维电离层产品,可为地球空间飞行器的空间环境信息支持、空间环境异常监测及预报、导航系统全球电离层延迟修正等提供服务.基于近实时三维电子密度模型,开展了电离层异常的立体监测,较IRI模型能够更好地监测磁暴期间电离层异常与演化过程,实现了全球大尺度、区域精细化电离层动态监测.同时,论文针对电离层异常对GNSS影响效应展开了较为全面的研究,分析了磁暴、太阳耀斑对GNSS信号、电离层模型精度、服务性能的影响.     

SAMI2物理模型与东亚扇区GPS TEC数据 比较研究

SAMI2 (Sami2 is Another Model of the Ionosphere)是美国海军实验室开发的电离层物理模型.利用该物理模型,模拟了东亚扇区不同太阳活动强度、不同纬度地区三个站的电离层电子浓度总含量 (TEC). 通过模拟结果与GPS观测站 TEC 数据的比较,检验 SAMI2 在此扇区的电离层 TEC 计算精度. 结果表明,物理模型输出的电离层 TEC 具备与观测数据一致的周日变化、季节变化,太阳活动变化. 周日分布上,上午时段SAMI2? TEC 与观测数据吻合度优于午后时段;季节分布上,SAMI2 TEC 在冬季与观测值偏差小于其他季节;SAMI2? TEC 与GPS TEC 相关系数各站均达到0.87以上,与赤道地区Guam站相关性最好;太阳活动低年计算结果优于太阳活动高年;多数情况下,SAMI2 TEC 相对GPS TEC 偏大. 本文结果为基于SAMI2模型构建背景误差分布特征,开展该区域电离层数值预报研究可行性提供了理论支持.      

地方时的全球电离层格网精度评价

针对IGS发布的电离层格网产品的精度(均方根)在不同区域受太阳辐射影响不同的问题,该文提出基于地方时的全球电离层格网精度分析,通过地方时能较好地分析近似太阳辐射条件下的电离层精度。研究结果显示,电离层精度明显受地面基准站分布疏密的影响,基准站密集区域均方根随太阳辐射变化的波动较小,并且在太阳辐射较高时也能很好地保证电离层产品的精度;而基准站稀疏的区域均方根随太阳活动的影响较大,电离层精度较差。     

Ionospheric F-layer global scintillation index variation using COSMIC during the period of 2007–2013

The three-dimensional global morphology and seasonal characteristics of the ionospheric scintillation index of the F-layer between 150 and 550 km altitudes are analyzed using the GPS radio occultation measurements from the Constellation Observing System for Meteorology, Ionosphere and Climate during the 7-year period of low and high sunspot activity from 2007 to 2013. The results show that the prominent scintillation intensity, which is confined within ±30° geomagnetic latitude, starts at post-sunset, reaches a maximum at around pre-midnight, and often persists until postmidnight. Moderate scintillation activity can be observed in the high-latitude region almost at any time, whereas weak scintillation prevails in the midlatitude region. The noticeable scintillation peak near midnight occurs at an altitude of approximately 250 km in most cases. However, the peak of the scintillation activity during the solar maximum extends to higher altitudes than observed during the solar minimum. Additionally, the local variation in time and altitude of the scintillation intensity is closely correlated with ionospheric HmF2. Statistical analysis indicates that an increase in solar activity or geomagnetic activity enhances the occurrence rate of scintillation and results in intense scintillation. The current research is beneficial for directly studying global ionospheric irregularities at GHz frequency based on high-rate L1 data and constructing a global scintillation model.     

卫星遥感大气订正的参数化模式及其模拟应用

发展了一个用于卫星大气订正的参数化模式,包括一个新的程辐射亮度模式和一个参数化的朗伯地表一大气辐射耦合引起的亮度增量模式.应用最小二乘法,程辐射亮度被参数化为大气总光学厚度、一次散射反照率、太阳天顶角、视天顶角、方位角、大气不对称因子的函数.应用这一参数化的亮度模式进行大气订正应用的数值模拟,即进行卫星遥感地表光谱反照率的模拟试验.数值检验结果表明对于865 nm,670nm,550nm和412nm 4个MODIS通道,在0°-70°的太阳天顶角、0°-60°视观测角以及0.05-0.8的地表反照率条件下,参数化的向上辐射亮度的标准差小于4%,由该参数化亮度模式引起的地表反照率解的标准差小于0.03.     

FORMOSAT-3/COSMIC observations of the ionospheric auroral oval development

The ionospheric radiance and electron density observed by the tiny ionospheric photometer (TIP) and GPS occultation experiment (GOX) payloads on FORMOSAT-3/COSMIC satellites are applied to determine the boundaries of the auroral oval and its width in the winter nighttime ionosphere for both hemispheres. The TIP collects ionospheric emission at 135.6 nm due to electron impact excitation, while the GOX offers ionospheric electron density profiles with radio occultation (RO) technique. Comparison between them shows similar patterns of the plasma structure in the polar caps. The mean width of the auroral bands ranges between about 2 and 11° latitude in the winter nighttime and it varies with longitudes. The comparison by month suggests that the mean radius of the auroral ovals varies with the intensity of the auroral radiance.     

Electron density profiles in the equatorial ionosphere observed by the FORMOSAT-3/COSMIC and a digisonde at Jicamarca

We examine for the first time the ionospheric electron density profiles concurrently observed by the GPS occultation experiment (GOX) onboard the FORMOSAT-3/COSMIC (F3/C) and the ground-based digisonde portable sounder DPS-4 at Jicamarca (12°S, 283°W, 1°N geomagnetic) in 2007. Our results show that the F3/C generally underestimates the F2-peak electron density NmF2 and the F2-peak height hmF2. On the other hand, when the equatorial ionization anomaly (EIA) pronouncedly appears during daytime, the total electron content (TEC) derived from the radio occultation of the GPS signal recorded by the F3/C GOX is significantly enhanced. This results in the NmF2 at Jicamarca being overestimated by the Abel inversion on the enhanced TEC during the afternoon period.     

利用掩星技术研究南极地区顶部电离层特性

掩星观测能够提供地面到低轨卫星轨道高度处的整个电离层电子密度剖面,对于顶部电离层的研究有重要的作用。本文利用COSMIC(constellation observing system for meteorology ionosphere and climate)掩星数据反演了电子密度剖面,提取了F₂层峰值高度(hmF2)、F₂层峰值密度(NmF2)、垂直标尺高(vertical scale height,VSH)等电离层参数,研究了南极地区的F₂层在太阳活动周期内的变化、年际变化、周日变化等,并且重点分析了南极地区的顶部电离层的垂直结构特征,尤其是威德尔海异常在垂直方向上的变化。结果表明,整个南极的hmF2每日均值在250~300 km左右,NmF2每日均值在1~8×10¹¹ el/m³之间,VSH每日均值在100~250 km,威德尔海异常主要表现在顶部电子密度的增强和底部电子密度的减少。     

Analysis of inversion errors of ionospheric radio occultation

The retrieved electron density profile of ionospheric radio occultation (RO) simulation data can be compared with the background model value during the simulation and the inversion error can be obtained exactly. This paper studies the inversion error of ionospheric RO through simulation. The sources of the inversion errors are analyzed. The impacts of measurement errors, such as the errors in phase measurements and satellite orbits, are very small and can be neglected. The approximation of straight-line propagation introduces errors at the height of the F1 layer under solar maximum condition. The spherical symmetry approximation of the electron density distribution is found to be the main source of the inversion error. The statistical results reveal some characteristics of the inversion errors. (1) The relative error increases with enhanced solar activity. (2) It is larger in winter than in equinox season, and it is smallest in summer. (3) For all seasons, it is smaller at middle latitude than at other latitudes. (4) For all seasons and geomagnetic latitudes, it is smaller at daytime than at other times. The NmF2 of the ROs from COSMIC are compared with the measurements of ionosondes, and the relative differences show the same dependencies on season, geomagnetic latitude and local time, as the relative errors of the simulated ionospheric ROs.

Ionospheric electron density observed by FORMOSAT-3/COSMIC over the European region and validated by ionosonde data

This research is motivated by the recent IGS Ionosphere Working Group recommendation issued at the IGS 2010 Workshop held in Newcastle, UK. This recommendation encourages studies on the evaluation of the application of COSMIC radio occultation profiles for additional IGS global ionosphere map (GIM) validation. This is because the reliability of GIMs is crucial to many geodetic applications. On the other hand, radio occultation using GPS signals has been proven to be a promising technique to retrieve accurate profiles of the ionospheric electron density with high vertical resolution on a global scale. However, systematic validation work is still needed before using this powerful technique for sounding the ionosphere on a routine basis. In this paper, we analyze the properties of the ionospheric electron density profiling retrieved from COSMIC radio occultation measurements. A comparison of radio occultation data with ground-based measurements indicates that COSMIC profiles are usually in good agreement with ionosonde profiles, both in the F2 layer peak electron density and the bottom side of the profiles. For this comparison, ionograms recorded by European ionospheric stations (DIAS network) in 2008 were used.     

Global ionosphere map constructed by using total electron content from ground-based GNSS receiver and FORMOSAT-3/COSMIC GPS occultation experiment

Effects of rapidly changing ionospheric weather are critical in high accuracy positioning, navigation, and communication applications. A system used to construct the global total electron content (TEC) distribution for monitoring the ionospheric weather in near-real time is needed in the modern society. Here we build the TEC map named Taiwan Ionosphere Group for Education and Research (TIGER) Global Ionospheric Map (GIM) from observations of ground-based GNSS receivers and space-based FORMOSAT-3/COSMIC (F3/C) GPS radio occultation observations using the spherical harmonic expansion and Kalman filter update formula. The TIGER GIM (TGIM) will be published in near-real time of 4-h delay with a spatial resolution of 2.5° in latitude and 5° in longitude and a high temporal resolution of every 5 min. The F3/C TEC results in an improvement on the GIM of about 15.5%, especially over the ocean areas. The TGIM highly correlates with the GIMs published by other international organizations. Therefore, the routinely published TGIM in near-real time is not only for communication, positioning, and navigation applications but also for monitoring and scientific study of ionospheric weathers, such as magnetic storms and seismo-ionospheric anomalies.     

Galileo single frequency ionospheric correction: performances in terms of position

For GPS single frequency users, the ionospheric contribution to the error budget is estimated by the well-known Klobuchar algorithm. For Galileo, it will be mitigated by a global algorithm based on the NeQuick model. This algorithm relies on the adaptation of the model to slant Total Electron Content (sTEC) measurements. Although the performance specifications of these algorithms are expressed in terms of delay and TEC, the users might be more interested in their impact on positioning. Therefore, we assessed the ability of the algorithms to improve the positioning accuracy using globally distributed permanent stations for the year 2002 marked by a high level of solar activity. We present uncorrected and corrected performances, interpret these and identify potential causes for Galileo correction discrepancies. We show vertical errors dropping by 56–64 % due to the analyzed ionospheric corrections, but horizontal errors decreasing by 27 % at most. By means of a fictitious symmetric satellite distribution, we highlight the role of TEC gradients in residual errors. We describe mechanisms permitted by the Galileo correction, which combine sTEC adaptation and topside mismodeling, and limit the horizontal accuracy. Hence, we support further investigation of potential alternative ionospheric corrections. We also provide an interesting insight into the ionospheric effects possibly experienced during the next solar maximum coinciding with Galileo Initial Operation Capability.     

一个植被双向反射模式的反演控制试验

利用地面遥感观测数据,对一个浑浊介质假定下的植被双向反射模式,增加了对太阳漫射辐射因素处理,在可见光波段上,进行了系列模式反演试验。这些试验有助于完善植被双向反射模式中物理过程的描述,了解模式反演过程的控制和选择合适遥感观测数据进行模式反演。分析试验结果发现：（１） 对 Ｌ Ａ Ｉ进行初值预估有利于获得较好的植被双向反射模式反演结果。（２） 加入植被对太阳漫射辐射的反射过程描述,可以使植被双向反射模式的反演结果更加合理。（３） 使用在太阳天顶角不太大（ ＜ ４５°） 和太阳方位角偏离１８０°不多（ ＜ ４５°） 观测条件下得到的遥感数据,可以使植被双向反射模式的反演结果较好。（４） 在３１°—６１°的太阳天顶角范围和１３６°—２５８°的太阳方位角范围内,多角度观测使太阳天顶角和方位角因素对 Ｌ Ａ Ｉ反演结果的影响不显著。（５） 当太阳漫射辐射的份额不大时,对 Ｌ Ａ Ｉ反演结果的影响不显著。如果只针对 Ｌ Ａ Ｉ,那么对反演植被双向反射模式所应用的地面遥感数据可以不进行大气校正处理,这样的结果虽然是从对地面遥感数据的处理中获得的,仍然对卫星遥感的观测时段选择和卫星遥感数据的选取和分析有一定的价值。