一种新的中长基线BDS三频模糊度快速解算方法

虽然TCAR能够实现短基线三频模糊度单历元解算,但由于电离层延迟及观测噪声等的影响,中长基线三频模糊度快速解算仍然是导航定位的一大难点。本文提出了一种新的无几何无电离层三频模糊度解算方法。该方法通过对伪距观测值赋予不同的权重,辅助宽巷及窄巷消除电离层残差的影响,使宽巷及窄巷求解只受观测噪声的影响;然后通过多历元的平滑获取宽巷及窄巷模糊度值。通过实测BDS三频长基线数据表明,相比经典TCAR算法,该方法可大大改善中长基线模糊度的求解精度,经过数据平滑并验证基本可以实现中长基线模糊度的快速解算。     

利用主成分分析建立区域对流层延迟时空模型

提出一种基于主成分分析（PCA）的ZTD时空建模方法,并利用GNSS连续运行参考站获取的ZTD数据,建立香港、云南、中国3个区域范围的ZTD时空模型。结果表明,所建立的区域对流层延迟时空模型不仅精度明显高于Saastamoinen、EGNOS和UNB3m模型,而且建模过程简单,模型参数较少,使用方便。     

雾霾对GPS天顶对流层延迟与精密单点定位影响研究

通过计算对流层延迟和精密单点定位的点位坐标,研究雾霾天气对GPS天顶对流层延迟和精密单点定位精度的影响。结果表明,当空气质量持续良好、没有雾霾发生时,空气质量指数(air quality index, AQI)与对流层延迟的相关性很小;当重度雾霾天气持续发生时,雾霾会对天顶对流层延迟产生40~60 mm的影响。但在精密单点定位中,通过对对流层延迟进行参数估计的方法可以消除绝大部分雾霾对定位精度的影响,因此无论重度雾霾天气是否发生,AQI指数与精密单点定位精度的相关性很小。     

动态映射函数对GPS基线解算质量的影响

介绍尼尔映射函数(NMF)、维也纳映射函数(VMF1)和全球映射函数(GMF)3种常用映射函数,讨论评估GPS基线质量的2个指标--基线重复性和平均值的标准偏差。根据中国境内IGS站的观测数据,基于GAMIT软件的数据处理结果,研究3种映射函数对GPS基线重复性和平均值标准偏差的影响。结果表明,在进行GPS基线处理时,动态映射函数的解算精度比经验映射函数要高,其中VMF1模型在解算基线重复性时结果更好,而GMF模型在计算平均值的标准偏差时效果更佳。     

附加相位延迟到弯曲角反演过程中的误差传递模型

为了研究全球卫星导航定位系统无线电掩星探测中的误差传递过程,文中讨论了掩星探测中附加相位延迟到弯曲角的反演过程中,附加相位延迟随机误差对反演弯曲角误差的影响。在对全球卫星导航定位系统和低轨道卫星进行精密定轨的情况下,忽略轨道误差对反演结果的影响,将轨道参数视为常数,考虑附加相位延迟△L存在随机误差δ△L时对反演弯曲角α带来的弯曲角误差δα。利用EGOPS仿真软件,采用数值模拟的方法模拟了无电离层影响的大气附加相位延迟数据,利用CHAMP真实轨道数据,MSIS-90大气模型和全三维射线追踪器进行前向建模,从中选取了一个掩星事件对误差传递模型进行了验证。结果表明:附加相位延迟的变化会给弯曲角的反演带来相应的误差:当随机误差为5 cm左右时,反演的弯曲角误差在±0.2 mrad范围内;当随机误差为1 cm左右时,反演的弯曲角误差在±4μrad范围内;当随机误差为1 mm左右时,反演的弯曲角误差在±40μrad范围内。最后从模拟的掩星事件中随机抽取了20个掩星事件进行统计分析,给出了20个掩星事件存在1 cm附加相位延迟测量误差引起弯曲角误差的均值误差,其误差特性虽略大于个例研究结果,但与模型完全吻合,反演的弯曲角误差也在±40μrad范围内,进一步验证了模型的准确性。     

全球定位系统的新进展(讲座五)——信号时延差对电离层延迟的影响

介绍电离层延迟改正时需要顾及信号时延差影响的原因,同时讨论并推导了采用各种双频信号进行测距时的电离层延迟模型。     

新的区域电离层模型及单频长基线精度分析

电离层延迟是影响GPS精密定位的主要因素,对单频接收机的影响尤为明显。介绍了一种新的基于区域双频观测网构建电离层模型的方法,并选取德国境内平均基线超过300 km(最长基线为461 km)的一个长距离观测网连续10 d的数据对模型进行了检测分析。实验证明,基于该电离层模型,网内单频接收机用户可获得接近双频观测数据的解算精度,即使对于200 km的长距离基线,单频数据的基线解算结果都能够达到平面方向6 mm,高程方向2.5 cm。区域电离层延迟模型构造方法可被有效应用于GPS、GLONASS和GALILEO等各类卫星导航定位系统,满足事后、实时或准实时单频接收机精密数据处理的需要。     

单频RTK动态解算的卡尔曼滤波算法研究

本文针对单频RTK提出了一种快速动态定位卡尔曼滤波算法,该方法使用C码和L1观测值,用模型改正对流层干延迟,双差大气延迟分解为测站大气天顶延迟和投影函数,与流动站位置以及站间单差模糊度组成观测方程进行卡尔曼滤波,得到单差模糊度浮点解及方差阵,通过星间求差得到双差模糊度浮点解及方差阵,结合MLAMBDA方法实时动态确定模糊度。经实测数据和IGS站数据验证该算法具有较好定位结果。     

网络RTK对流层拟合模型分析

为了拟合网络RTK中用户端双差对流层延迟,本文分析了基于距离的线性内插模型(DIM)、线性内插模型(LIM)原理,提出了指数拟合模型:以主参考站为原点,系数项与用户端和辅参考站间夹角成反比,指数底数值为0.35,用户端到主参考站与辅参考站到主参考站间距离比值被1减为指数。通过分析上述模型的误差系数给出了模型优缺点,试验验证了指数模型的有效性和稳定性:卫星拟合精度一般优于2cm,实现了单历元平面定位精度优于2cm,高程精度优于3cm。     

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.