地壳运动速度场插值方法研究

分析了构建速度场的统计模型和函数模型法,提出利用两种模型逼近原始观测速度的综合逼近法,以减少剩余误差。计算和比较了各种方法,结果显示,综合法优于单独利用统计模型和函数模型法。     

Modeling errors in upward continuation for INS gravity compensation

Accurate upward continuation of gravity anomalies supports future precision, free-inertial navigation systems, since the latter cannot by themselves sense the gravitational field and thus require appropriate gravity compensation. This compensation is in the form of horizontal gravity components. An analysis of the model errors in upward continuation using derivatives of the standard Pizzetti integral solution (spherical approximation) shows that discretization of the data and truncation of the integral are the major sources of error in the predicted horizontal components of the gravity disturbance. The irregular shape of the data boundary, even the relatively rough topography of a simulated mountainous region, has only secondary effect, except when the data resolution is very high (small discretization error). Other errors due to spherical approximation are even less important. The analysis excluded all measurement errors in the gravity anomaly data in order to quantify just the model errors. Based on a consistent gravity field/topographic surface simulation, upward continuation errors in the derivatives of the Pizzetti integral to mean altitudes of about 3,000 and 1,500 m above the mean surface ranged from less than 1 mGal (standard deviation) to less than 2 mGal (standard deviation), respectively, in the case of 2 arcmin data resolution. Least-squares collocation performs better than this, but may require significantly greater computational resources.     

UKF在基于地磁场的自主导航中的应用

本文研究了基于地磁场的自王导航,建立了以卫星轨道动力学方程为基础的系统状态方程,并详细推导了以地磁场矢量为观测量时的观测方程;为了解决系统的非线性问题把常用来解决非线性问题的UKF引入到基于地磁场的自主导航系统中;最后,用Matlab对基于地磁场的自主导航系统进行了仿真,仿真结果表明UKF有很好的收敛性和稳定性.     

用神舟三号中分辨率成像光谱仪数据反演大气水汽

2002年3月中国神舟三号飞船发射成功，所携带的中分辨率成像光谱仪获取了一批940nm波段的遥感数据。本文用其中的部分资料做了反演水汽的试验，给出一些结果和分析。     

空间大地测量技术实测台站速度场精度分析

利用国际上3个著名的数据分析处理中心CSR、JPL和GSFC给出的3种空间大地测量技术实测的台站运动速度场数据,解算不同空间技术速度场之间的转换参数,即速度场之间的系统差。在扣除两两技术之间速度场的系统差后,用速度场残差计算了空间技术速度场之间的不符值加权中误差作为衡量不同空间技术实测台站速度场的外部检核指标,即外符精度。计算结果表明,VLBI和GPS实测台站地心速度已经达到1 mm/a的精度;SLR实测台站地心速度已经达到2 mm/a的精度。     

基于大视场光学测量设备的多星观测和解算天文经纬度研究

本文提出了一种新的基于大视场光学测量设备和GPS测量点位天文坐标的方法,即测量多个星体方位角相对于主光轴方位角的增量,然后通过非线性最小二乘法解算出点位的天文坐标。采用该方法不仅可以避免讨论大气蒙气差的修正问题,而且能够满足高精度天文坐标的测量要求。     

基于2.5维面的气象数据可视化技术——以风场数据显示为例

根据2.5维面的设计思想及曲面可视化的方法,结合部分气象数据信息具有相同的经纬度范围和海拔高度的特点,构造了基于温度和可降水量的2.5维面,并重点提出在2.5维面上进行风场流线可视化的方法。实践证明,应用2.5维面分析气象数据在一定程度上平衡了运算量和可视化结果之间的矛盾,对地理环境气象数据的分析和比较有帮助作用。     

基于卫星加速度恢复地球重力场的去相关滤波法

基于加速度法恢复地球重力场时,卫星加速度是由卫星轨道数值微分得到,而数值微分会放大高频误差,进而降低了重力场解算结果的精度.针对数值微分导出的加速度误差具有有色噪声的特性,提出利用去相关算法构造白化滤波器对加速度有色噪声进行滤波处理,并根据去相关的基本原理分别构造了基于三点差分和ARMA模型的白化滤波器.采用不同噪声背景的CHAMP卫星模拟轨道数据进行解算,结果表明:基于去相关滤波解算的重力场模型精度均要比等权解算的重力场模型精度高,初步验证了去相关滤波方法的有效性.     

基于网络服务的地类遥感影像样本检索系统的设计与实现

为了有效地辅助第二次全国土地调查,对土地覆盖情况和地类遥感影像判读提供辅助,运用ASP.NET和网络服务技术,以多源遥感影像为数据源,构建了基于网络服务的地类遥感影像样本检索系统。本文重点研究了基于网络服务的地类遥感影像样本检索系统的结构、流程和功能,提出了系统的数据库表结构设计方法,为网络化遥感样本检索服务提供了解决方案。     

Progressive Transformation of a Flux Rope to an ICME

The solar wind conditions at one astronomical unit (AU) can be strongly disturbed by interplanetary coronal mass ejections (ICMEs). A subset, called magnetic clouds (MCs), is formed by twisted flux ropes that transport an important amount of magnetic flux and helicity, which is released in CMEs. At 1 AU from the Sun, the magnetic structure of MCs is generally modeled by neglecting their expansion during the spacecraft crossing. However, in some cases, MCs present a significant expansion. We present here an analysis of the huge and significantly expanding MC observed by the Wind spacecraft during 9 – 10 November 2004. This MC was embedded in an ICME. After determining an approximate orientation for the flux rope using the minimum variance method, we obtain a precise orientation of the cloud axis by relating its front and rear magnetic discontinuities using a direct method. This method takes into account the conservation of the azimuthal magnetic flux between the inbound and outbound branches and is valid for a finite impact parameter (i.e., not necessarily a small distance between the spacecraft trajectory and the cloud axis). The MC is also studied using dynamic models with isotropic expansion. We have found (6.2±1.5)×10²⁰ Mx for the axial flux and (78±18)×10²⁰ Mx for the azimuthal flux. Moreover, using the direct method, we find that the ICME is formed by a flux rope (MC) followed by an extended coherent magnetic region. These observations are interpreted by considering the existence of a previously larger flux rope, which partially reconnected with its environment in the front. We estimate that the reconnection process started close to the Sun. These findings imply that the ejected flux rope is progressively peeled by reconnection and transformed to the observed ICME (with a remnant flux rope in the front part).