地球磁场微波遥感探测方法研究进展

地磁场是地球的重要物理场之一, 地磁学在地球与空间物理以及地质等领域具有极为重要的作用. 强便利性、低成本、广空间范围的磁场测量方法与高精度、多维度的地磁测量数据的获取, 是地磁学等领域科学与应用研究得以深入的重要依据. 为解决基于高精度磁强计的原位磁场测量方法在效率和探测范围等方面的局限, 遥感探测已经逐渐开始成为一个新的磁场探测研究领域. 本文基于微波辐射计遥感手段的地磁场遥感探测方法, 综合分析了地磁场微波遥感技术方法的基本原理、研究进展与应用现状, 并在此基础上讨论了其在探测能力等方面的需求、技术难点及未来的发展趋势, 进而对未来磁场遥感探测研究, 例如行星磁场遥感探测等提出了新的展望.     

"神舟三号"大气成分探测器探测结果--2002年4月磁暴期间大气成分的异常变化

"神州三号"(SZ-3)大气成分探测器搭载在SZ-3留轨舱上于2002年3月26日发射入轨,正遇2002年4月发生的连续两次地磁扰动事件,SZ-3大气成分探测器测得了轨道舱运行高度上(330-350 km附近)大气成分的响应变化和异常现象.探测数据表明,在地磁扰动期间,不仅发生了大气中主要成分O和N2的数密度值增变的响应变化,而且在进入地磁扰动峰期开始后6h左右在较高纬度处出现了N2的异常增变和O的异常降变.4-5h后,这种异常增变峰和降变谷由纬度42°N左右逐渐推移向纬度较低地区,直至消失.     

Effects of space weather on the ionosphere and LEO satellites’ orbital trajectory in equatorial,low and middle latitude

We study the effects of space weather on the ionosphere and low Earth orbit (LEO) satellites’ orbital trajectory in equatorial, low- and mid-latitude (EQL, LLT and MLT) regions during (and around) the notable storms of October/November, 2003. We briefly review space weather effects on the thermosphere and ionosphere to demonstrate that such effects are also latitude-dependent and well established. Following the review we simulate the trend in variation of satellite’s orbital radius (r), mean height (h) and orbit decay rate (ODR) during 15 October–14 November 2003 in EQL, LLT and MLT. Nominal atmospheric drag on LEO satellite is usually enhanced by space weather or solar-induced variations in thermospheric temperature and density profile. To separate nominal orbit decay from solar-induced accelerated orbit decay, we compute $r\text{,}h$ and ODR in three regimes viz. (i) excluding solar indices (or effect), where $r=r_0\text{,}h=h_0$ and $\mathit{ODR}={\mathit{ODR}}_0$ (ii) with mean value of solar indices for the interval, where $r=r_m\text{,}h=h_m$ and $\mathit{ODR}={\mathit{ODR}}_m$ and (iii) with actual daily values of solar indices for the interval ($r\text{,}h$ and ODR). For a typical LEO satellite at h?=?450?km, we show that the total decay in r during the period is about 4.20?km, 3.90?km and 3.20?km in EQL, LLT and MLT respectively; the respective nominal decay ($r_0$) is 0.40?km, 0.34?km and 0.22?km, while solar-induced orbital decay ($r_m$) is about 3.80?km, 3.55?km and 2.95?km. h also varied in like manner. The respective nominal ${\mathit{ODR}}_0$ is about 13.5?m/day, 11.2?m/day and 7.2?m/day, while solar-induced ${\mathit{ODR}}_m$ is about 124.3?m/day, 116.9?m/day and 97.3?m/day. We also show that severe geomagnetic storms can increase ODR by up to 117% (from daily mean value). However, the extent of space weather effects on LEO Satellite’s trajectory significantly depends on the ballistic co-efficient and orbit of the satellite, and phase of solar cycles, intensity and duration of driving (or influencing) solar event.     

Magnetospheric physics in China: 2008—2010

In the past two years, most of the works on magnetospheric physics were made by using the data of Double Star Program and Cluster missions. However some works were still conducted by computer simulation or using the data from other space missions and ground geomagnetic observations. This paper briefly review these previous works based on papers selected from the 28 publications from April 2008 to April 2010. The subjects covered various sub-branches of magnetospheric physics, including geomagnetic storm, magnetospheric substorm and etc.     

A new inversion method of plasma density distribution of plasmasphere in the geomagnetic equatorial plane from IMAGE data

The plasma density distribution of plasmasphere in the geomagnetic equatorial plane can help us study the magnetosphere like plasmasphere, ionosphere and their kinetics. In this paper, we introduce a new inversion method, GE-ART, to calculate the plasma density distribution in the geomagnetic equatorial plane from the Extreme Ultraviolet (EUV) data of IMAGE satellite under the assumption that the plasma density is constant along each geomagnetic field line. The new GE-ART algorithm was derived from the traditional Algebraic Reconstruction Techniques (ART) in Computed Tomography (CT) which was different from the several existing methods. In this new method, each value of the EUV image data was back-projected evenly to the geomagnetic field lines intersected by this EUV sight. A 3-D inversion matrix was produced by the contributions of all the voxels contained in the plasmasphere covered by the EUV sensor. That is, we considered that each value of the EUV image data was relative to the plasma densities of all the voxels passed through by the corresponding EUV radiation, which is the biggest difference to all the existing inversion methods. Finally, the GE-ART algorithm was evaluated by the real EUV data from the IMAGE satellite.     

基于IGS电离层TEC格网的扰动特征统计分析

电离层总电子含量（TEC）是研究空间天气特性的重要参量,通过分析电离层TEC,可以了解空间环境的变化特征.利用IGS提供的1999—2016年全球电离层TEC格网数据,按照地磁纬度将全球划分为高、中、中低、低磁纬四个区域,计算不同区域的电离层扰动;利用大量统计数据选取电离层扰动事件的判定阈值,分析电离层扰动与太阳活动、时空之间的关系;计算电离层扰动指数与地磁活动之间的相关系数.结果显示：电离层扰动与太阳活动变化具有较强的正相关特性.在太阳活动低年,电离层扰动事件发生的概率约为1.79%,在太阳活动高年发生扰动的概率约为10.18%.在空间分布上,无论是太阳活动高年还是低年,高磁纬地区发生扰动事件的概率均大于其他磁纬出现扰动事件的概率.计算得到的中磁纬和中低磁纬地区电离层扰动指数与全球地磁指数Ap的相关系数分别为0.57和0.56,说明电离层扰动指数与Ap具有较好的相关关系;高磁纬电离层扰动指数与Ap的相关系数为0.44;低磁纬扰动指数与Ap的相关系数为0.39.以上结果表明,不同区域电离层扰动与全球地磁指数Ap的相关性不同,测定区域地磁指数可能会提高与电离层扰动的相关性.     

一种基于白谱法的电离层天气扰动指数

基于一种电离层扰动提取方法——白谱法,利用IGS提供的电离层TEC网格数据,获得电离层J_s指数、J_r指数和J_p指数,分别反映单站、纬度圈（沿经度积分）及行星际尺度下的电离层天气扰动状态.在2015年3月的一次磁暴过程中,J_s指数、J_r指数及J_p指数均很好地反映出电离层响应地磁暴的过程,磁暴前后J_p指数与Dst指数相关系数达到-0.72;J_s图从二维角度很好地表征了电离层天气的扰动过程.在此基础上,统计分析了2011——2014年J_p指数与Dst指数的相关性,结果表明：限定J_p≥2,J_p指数与对应时间Dst指数的相关系数为-0.67;限定J_p≥3,二者相关系数更高,达到-0.87.通过分析不同J_p指数阈值下不同等级磁暴的次数,发现J_p指数可以很好地反映磁暴下的电离层整体扰动,为指示电离层天气状态提供了可能的参数.