资源三号卫星影像纠正的方法研究

影像的应用前提是影像处理,大气校正可消除大气和光照等因素对地物发射的影响。在此基础上,介绍几种常用的几何纠正方法,可消除系统和非系统因素引起的影像几何变形。本文通过对资源三号卫星的基本参数信息和相对应影像数据特点的介绍,先通过大气校正,校正后的影像分别使用几何纠正的几种方法,并通过各种方法的计算量、实用性以及相应的精度,对比分析各种方法在处理这种数据时的优越性。     

SMAP卫星海表盐度产品的检验与校正

In this study, sea surface salinity(SSS) Level 3(L3) daily product derived from soil moisture active passive(SMAP)during the year 2016, was validated and compared with SSS daily products derived from soil Moisture and ocean salinity(SMOS) and in-situ measurements. Generally, the root mean square error(RMSE) of the daily SSS products is larger along the coastal areas and at high latitudes and is smaller in the tropical regions and open oceans. Comparisons between the two types of daily satellite SSS product revealed that the RMSE was higher in the daily SMOS product than in the SMAP, whereas the bias of the daily SMOS was observed to be less than that of the SMAP when compared with Argo floats data. In addition, the latitude-dependent bias and RMSE of the SMAP SSS were found to be primarily influenced by the precipitation and the sea surface temperature(SST). Then, a regression analysis method which has adopted the precipitation and SST data was used to correct the larger bias of the daily SMAP product. It was confirmed that the corrected daily SMAP product could be used for assimilation in high-resolution forecast models, due to the fact that it was demonstrated to be unbiased and much closer to the in-situ measurements than the original uncorrected SMAP product.     

基于机器学习的海洋环境预报订正方法研究

结合中尺度数值模式 WRF 预报数据和 ERA5 再分析资料,利用机器学习方法对 WRF 预报场的风场、温度、气压进行预报订正。采用 ERA5 作为真值,与原始 WRF 预报相比,利用随机森林模型可以将预报结果整体均方根误差降低 44%以 上,利用深度神经网络模型可以将预报结果整体均方根误差降低 34%以上。通过随机森林模型实验得到不同输入特征对预报要素的影响程度,分析了关键的预报订正因子。     

复杂城区车载激光扫描点云分层路段定位与数据纠正实验研究

高精度的车载点云数据是实现各种城市地物要素提取的前提,但在复杂城市环境下车载作业时信号遮挡、衰减和多径效应频繁发生,进而造成点云数据精度严重降低,如何对复杂环境下的点云数据进行分析和纠正就显得至关重要.现有的质量分析方法多从测距误差、仪器安装误差和数据处理误差方面出发,虽然可以在一定程度上改化数据,但在如何快速定位出分...     

微波照射下火成岩升温特性和升温预测模型研究

微波辅助破岩可有效降低刀具磨损,提高破岩效率,具有广阔的发展前景.文章选取了10种火成岩进行微波加热试验,发现岩石的升温速率主要与岩石所含矿物的种类、含量,及岩石中的Fe元素含量有关.岩石所含矿物越敏感、含量越多,岩石中的Fe元素含量越大时,其升温速率越高.整体而言,火成岩中基性岩的升温速率最高、中性岩次之、酸性岩最低...     

Scaling-laws of Radio Spike Bursts and Their Constraints on New Solar Radio Telescopestwo

Radio observation is one of important methods in solar physics and space science. Sometimes, it is almost the sole approach to observe the physical processes such as the acceleration, emission, and propagation of non-thermal energetic particles, etc. So far, more than 100 solar radio telescopes have been built in the world, including solar radiometers, dynamic spectrometers, and radioheliographs. Some of them have been closed after the fulfillment of their primary scientific objectives, or for their malfunctions, and thus replaced by other advanced instruments. At the same time, based on some new technologies and scientific ideas, various kinds of new and much more complicated solar radio telescopes are being constructed by solar radio astronomers and space scientists, such as the American E-OVSA and the solar radio observing system under the framework of Chinese Meridian Project II, etc. When we plan to develop a new solar radio telescope, it is crucial to design the most suitable technical parameters, e.g., the observing frequency range and bandwidth, temporal resolution, frequency resolution, spatial resolution, polarization degree, and dynamic range. Then, how do we select a rational set of these parameters? The long-term observation and study revealed that a large strong solar radio burst is frequently composed of a series of small bursts with different time scales. Among them, the radio spike burst is the smallest one with the shortest lifetime, the narrowest bandwidth, and the smallest source region. Solar radio spikes are considered to be related to a single magnetic energy release process, and can be regarded as an elementary burst in solar flares. It is a basic requirement for the new solar radio telescope to observe and discriminate these solar radio spike bursts, even though the temporal and spatial scales of radio spike bursts actually vary with the observing frequency. This paper presents the scaling laws of the lifetime and bandwidth of solar radio spike bursts with respect to the observing frequency, which provide some constraints for the new solar radio telescopes, and help us to select the rational telescope parameters. Besides, we propose a spectrum-image combination mode as the best observation mode for the next-generation solar radio telescopes with high temporal, spectral, and spatial resolutions, which may have an important significance for revealing the physical essence of the various non-thermal processes in violent solar eruptions.     

椭球谐和球谐系数之间一个简单的转换关系

本文推导的椭球谐系数和球谐系数相互之间转换关系的核心思想是在ε~2量级下利用Legendre函数的正交性,从球谐系数求解的积分表示出发,将积分中的椭球坐标变量与球坐标变量相互转换,从而得出椭球谐系数与球谐系数之间的转换关系。本文导出的转换关系有以下优点:①对于第二类Legendre函数的计算采用Laurent级数表示,使计算第二类Legendre函数更为简单;②保留了ε~2量级下,导出的转换关系相比文献[2]的形式更简单,满足物理大地测量边值问题线性化的要求;③顾及了余纬和归化余纬的区别。     

Jason-2高度计电离层GIM误差分析及修正研究

基于Jason-2高度计2015年地球物理数据集(GDR)38个周期太平洋海域的全球电离层图(GIM)电离层校正值和双频校正值的数据,分不同季度和不同纬度区域比较二者的差异,结果表明:GIM值与双频校正值之间存在明显的差异,GIM校正值普遍高于双频校正值,说明GIM高估了电离层路径延迟,GIM校正值与双频校正值的差异与季节和纬度区间有关。用梯度下降法得到GIM值的修正方程,将修正方程应用于2016年Jason-2的全年数据,修正后的GIM值与双频校正值十分接近,在各年份中均具有良好的适用性。在单频高度计不能使用电离层双频校正算法的情况下,可以利用不同季度和不同纬度区域的修正方程对同等高度的高度计GIM值进行修正以达到双频校正值的精度水平。     

录井校正新方法在东海盆地西湖凹陷的应用

录井检测受井场环境影响较大,主要包括钻井环境与检测环境,钻井环境包括井径、钻时、钻井液排量、是否取心等,检测环境主要是井场自然环境与检测器内部环境。一般情况下检测器内部环境基本一致,而井场自然环境在一定时间内变化不大,故而钻井环境对录井检测的影响较大,钻井环境校正是进行录井解释前的重要工作。常规Tg(全烃含量)校正方法在取心、低异常、多互层等层段使用效果较差,经过分析,将校正方法在取心、钻时、排量、基值方面进行优化,实践验证,新校正方法效果较好,适应了西湖凹陷的地质研究需求。     

实时卫星钟差基准精化方法

在基于精密单点定位(PPP)的授时方法中,卫星钟差产品的高精度时间基准至关重要.针对实时卫星钟差产品时间基准不够稳定的问题,本文采用一组具有原子钟外部输入的国际全球卫星导航系统(GNSS)服务(IGS)跟踪站建立了顾及原子钟变化特性的基准精化方法.该方法首先采用阿伦方差对不同的IGS跟踪站外接原子钟进行稳定度分析,挑选出一组稳定度高的原子钟用以精化时间基准.在此基础上,利用阿伦方差分析各台原子钟的噪声参数特征,并确定不同原子钟之间的权比关系.最终,建立时间基准改正量的随机模型,并计算出精化后的时间基准.通过实例验证表明:与IGS事后精密钟差产品定义的时间基准比较,改正后的实时钟差基准单天内的标准差(STD)优于0.1 ns,相比于改正前最高提升了93%.同时,基准改正后的天内万秒稳达到10^-15量级,实现了一个量级的提高.此外,通过相对钟差精度的分析,表明钟差基准修正不影响PPP的定位精度.