中纬热层大气质量密度经向结构差异研究

本文利用CHAMP卫星以及全球电离层-热层模型(GITM)来研究太阳活动低年(2007—2009年)中纬热层大气质量密度(ρ)的经度结构变化.结果如下:(1)ρ存在明显的经度单波结构(单峰和单谷),且南北半球反相,波峰和波谷随着地方时增加而向东移动;(2)模拟表明离子拖曳效应在ρ结构差异的形成中起到了重要的作用,欧亚地区电子密度经度差异性较弱,不足以影响ρ经度分布,导致该地区ρ经度差异不明显;(3)在磁中纬地区,太阳天顶角的经度差异可达20°~30°,太阳光加热的经度不均匀性是导致ρ经度差异的另一个主要原因.     

顶部电离层离子密度经度结构的特征及其随季节、太阳活动和倾角的变化

本文利用DMSP卫星测量数据和傅里叶分解和重构方法,研究了地磁平静期顶部电离层总离子密度(Ni)经度结构的多重波数特征及波数4的年变化、逐年变化、地方时差异和随倾角的变化.傅里叶分解和重构的结果表明,顶部电离层平均Ni的经度结构中同时含有以波数1至波数4为主的多重分量,不同波数分量的幅度和相位各不相同.对波数4分量的分析表明,波数4的幅度在春秋季最强,北半球夏季高于冬季;随太阳活动水平增强,波数4分量的幅度增高,至太阳活动高年幅度达到最高,此后随太阳活动水平降低而减小,与F10.7呈正相关;春秋季和北半球夏季波数4分量在傍晚最强,晚上和上午次之,黎明最弱,从09LT到21LT,波数4的相位依次滞后,暗示向东移动.分析还发现,日落期间波数4幅度依赖倾角,春秋季随倾角的变化呈双峰结构,两个极大出现在倾角±18°附近,暗示赤道等离子体喷泉效应对顶部电离层经度结构的控制作用.     

利用COSMIC低轨卫星对GPS信号的顶部TEC观测资料研究等离子体层电子含量的变化特征

本文尝试利用COSMIC低轨卫星对GPS信号的顶部TEC观测资料研究等离子体层电子含量(简称PEC)的变化规律.首先介绍从低轨卫星对GPS的顶部TEC观测资料提取等离子体层垂直电子含量的方法,然后利用该方法提取2008年全年的PEC数据,进而研究了2008年这一太阳活动低年PEC随地磁纬度(MLAT)、磁地方时(MLT)以及不同季节的变化规律.此外,还利用提取的120°E和300°E经度链上的数据对比研究了PEC的经度变化情形.研究结果表明:(1)PEC主要集中分布在磁赤道±45°之间的一个绕地球的环带状区域中;(2)PEC表现出以下的昼夜变化规律特征:白天时段之值高于夜间,约在12—16MLT之间达到最高峰值,而最小PEC值出现在日出前大约4—5MLT左右的时段;(3)相比其他季节月份而言,PEC在北半球夏季月份(5—8月)具有最小值;(4)PEC存在明显的经度变化,不同经度链上的PEC存在不同的季节变化特征.     

关于暴时电离层电流分布的南北半球不对称性

采用国际上广泛认可的高层大气和电离层经验模式提供的各种参数, 通过电离层电流连续方程, 计算出强磁暴条件下6月至日和12月至日内, 磁纬±72°和磁地方时00:00～24:00之间电离层电场、电流等的分布. 计算中考虑了地磁和地理坐标间的偏离; 除中性风场感生的发电机效应外, 还包含了磁层耦合(极盖区边界的晨昏电场和二区场向电流)的驱动外源. 结果表明, 6月至日时, 磁层扰动自极光区向中低纬的穿透情况在南、北半球内基本接近, 北半球内略强; 但12月至日时, 呈现明显的不对称性, 南半球的电流穿透远强于北半球, 而电场的穿透则是在北半球更强. 无论南北半球, 在中高纬地区, 午夜至黎明时段出现较强的东向电场分量, 其[WTHX]E×B[WTBZ]的向上漂移效应, 正是解释我们以往不少研究现象中所期盼的物理机制.     

基于SWARM双星观测的场向电流的经度变化

本文利用SWARM A和C双星高精度的矢量磁场数据研究了不同季节高纬地区场向电流(FACs)随地磁经度和地方时的变化情况.研究发现:在南北半球,FACs存在明显的经度变化,南半球FACs的变化强度大约是北半球的1.2～3.2倍.利用潮汐谱分析法我们发现FACs中占主导的非迁移潮汐分量为DW2和D0.在春秋和夏季半球,DW2波更为明显.D0波可用太阳光照的经度变化来解释,向阳侧靠近磁极的经度带比远离磁极的经度带有更强的太阳光照射.DW2波则与地磁场强度和地磁倾角等因素有关.全球电离层与热层模型计算的FACs中D0波占主导,且中性风和对流电场对D0波的贡献几乎相当.     

基于三亚VHF雷达的场向不规则体观测研究:4.太阳活动低年夏季F区回波

太阳活动低年夏季,低纬电离层F区场向不规则体表现出与太阳活动高年和其他季节明显不同的特征.本文利用我国三亚站(18.4°N,109.6°E,地磁倾角纬度dip latitude 12.8°N)VHF雷达、电离层测高仪、GPS闪烁监测仪和美国C/NOFS卫星观测数据,研究了太阳活动低年夏季我国低纬电离层F区场向不规则体的基本特征.分析发现无论磁静日还是磁扰日,夏季电离层F区不规则体回波主要出现于地方时午夜以后,回波出现的时间较短,高度范围较小,伴随着扩展F出现,但没有同时段的L波段电离层闪烁.太阳活动低年夏季午夜后的低纬电离层F区不规则体回波,可能并不总是与赤道等离子体泡沿磁力线向低纬地区的延伸相关,而可能由本地Es等扰动过程引起.     

磁偏角和热层风对中纬电离层TEC经度分布的影响

本文利用北美、南美和大洋洲三个地区的电离层TEC数据,分析了磁偏角为零的经度线两侧中纬电离层TEC的差异.结果表明,在2001年至2010年的几乎所有季节,在磁偏角为零的经度东西两侧,北美、南美和大洋洲中纬电离层TEC都存在规则性的差异;中纬电离层TEC的这种经度差异显著地依赖地方时,对季节和太阳活动水平也有不同程度的依赖.地磁场影响下电离层与热层动力学耦合的分析表明,磁偏角的经度变化和热层风的地方时变化两者的共同作用是引起磁偏角为零的经度两侧中纬电离层TEC差异的重要原因之一.     

通量管积分瑞利-泰勒不稳定性的半球不对称和随经度变化的研究

本文利用通量管积分方法,对磁南北半球分别沿磁力线积分,研究背景电离层南-北半球不对称以及中性风场和磁偏角随经度的变化对广义瑞利-泰勒不稳定性和电离层不规则结构生成和发展的影响.结果表明,通量管积分广义瑞利-泰勒不稳定性线性增长率存在显著的半球不对称,南北半球不对称的中性风场是导致电离层不规则结构呈南北分布不对称的重要因素;随经度变化的中性风场和磁偏角对瑞利-泰勒不稳定性的经度变化有重要影响,它们可能是导致不规则结构出现率经度变化的主要控制因素.     

北半球电离层中纬槽发生率及其槽极小位置变化的统计研究

本文利用2014年9月到2017年8月全球高时空分辨率TEC数据对北半球四个经度带电离层中纬槽的发生率和槽极小位置的变化进行了统计研究.基于Kp指数,我们引入了一个包含地磁活动变化历史效应的地磁指数(Kp 9)来分析中纬槽位置变化与地磁活动水平的关系.通过与其他地磁活动指数的对比,发现槽极小纬度与Kp 9指数的相关性最好.此外,本文重点分析了中纬槽发生率及槽极小纬度的经度差异、季节变化、地方时变化以及与地磁活动强度等的关系.结果表明,中纬槽的发生率与经度关系不大,主要受到季节、地方时与地磁活动的影响.午夜中纬槽发生率在夏季较低,其随地方时的变化则呈现出负偏态分布的特点,在后半夜发生率更高,而地磁活动增强对中纬槽的发生具有明显的促进作用.对于槽极小纬度,其在四个经度带的分布差异不大,但月变化各不相同,其中-120°经度带呈单峰分布,在夏季槽极小纬度更高,而0°经度带夏季槽极小纬度更低.槽极小的位置显著依赖于地磁活动、地方时以及季节变化.一般说来,地磁活动越强,中纬槽纬度越低.中纬槽位置随地方时的变化有明显的季节差异,冬季昏侧槽极小纬度随地方时变化较快,弱地磁活动条件下22∶00 LT前即达到最低纬度,其后位置几乎保持不变,而两分季槽极小纬度从昏侧至午夜都在降低,夏季槽极小纬度从昏侧连续下降至03∶00 LT左右.     

外源S_q等效电流体系电流涡中心电流强度与太阳活动关系

本文选取了INTERMAGNET地磁台网2001年到2012年的地磁数据,对其进行世界时(UT)到地方时(LT)的转换后利用自然正交分量法(NOC)从所选资料中提取出太阳静日变化Sq成分,再通过球谐分析方法建立模型分离内、外源Sq成分,逐日反演出内、外源Sq等效电流体系,并得到外源Sq等效电流体系南北电流涡中心电流强度.本文将外源Sq等效电流体系南北电流涡中心电流强度与同一时期的Dst指数进行了对比分析,研究表明它们之间具有同步变化的规律,且北半球电流涡中心电流强度在磁暴发生时的异常现象远高于南半球.对F10.7cm太阳射电流量与外源Sq等效电流体系南、北半球电流涡中心电流强度的长短周期分析发现,Sq等效电流表现出明显的11年周期特点,与太阳活动周期一致.外源南、北半球电流涡中心电流强度和F10.7cm年均值的相关系数分别达到了0.93和0.90,说明太阳活动是导致外源Sq电流体系变化的最直接也最主要的因素,这可能与电离层电导率受控于太阳的电磁辐射相关.     

The correlation between the variation in ionospheric conductivity and that of the geomagnetic Sq field

Effects of the solar activity on the geomagnetic Sq field were studied by examining the correlation of the Sq amplitude in the Y-component with the sunspot number or height integrated Pedersen and Hall conductivities of the ionosphere at Kakioka, Chambon La Foret and Port Moresby for a period of 21 years. It was found that solar activity dependence of the Sq amplitude is almost explained by the effect of the local ionospheric conductivity if the month is fixed. That is, the solar activity dependence in each month is mainly caused by the local conductivity. However, the amplitude is clearly small in winter for the same conductivity value. This is probably due to the seasonal difference of the neutral winds driving ionospheric dynamo currents or to the magnetic effect of the field-aligned currents connecting both hemispheres driven by the asymmetric dynamo action in the ionosphere.     

太阳磁场磁性指数异常变化对南北半球中纬度气候的影响

本文参照太阳黑子相对数特征建立了太阳黑子磁场磁性指数时间序列. 大气温度场谱分析结果显示,南北半球中纬度平流层和对流层大气温度场普遍存在22年变化周期. 分析认为,大气温度场的22年变化周期是太阳活动22年磁性周期所激发.     

非迁移潮作用下的电离层赤道异常区单峰现象及其经度分布

当喷泉效应较弱而双峰结构发展不充分的时候,可能在赤道异常区仅能够观测到一个电子密度的峰值,称之为单峰现象.本文利用CHAllenging Minisatellite Payload卫星在2001-2010年的电子密度数据给出了单峰的发生规律,单峰在地方时早上08：00-10：00和下午16：00-19：00发生率高,发生位置在经度上呈现多波数分布,尤其在10：00-18：00明显：在分季时多呈现四波,而在冬至季时以三波为主.单峰发生多的经度,正好对应着双峰的结构特征较弱之处.究其原因,是非迁移潮的DE2和DE3分量调制了背景风场和大气发电机电场,在电场和喷泉效应减弱的经度,双峰结构难以形成时,就会表现为单峰结构.本文扩展了对单峰现象的地方时、季节和经度分布等规律的了解,明确了非迁移潮在其中施加的影响,由此,单峰同双峰现象一样可以用于研究非迁移潮对热层-电离层的作用.     

Relation between variations in the characteristics of the high-latitude atmosphere and solar cosmic factors

Daily temperatures at high latitudes of the Northern and Southern hemispheres and the corresponding levels of currents of solar protons and the PC, Ap, and Dst magnetic indices are considered. The character of variations in the surface temperature depending on these indices in different seasons during strong magnetic storms, when the Dst amplitude was smaller than ?50, has been indicated. The relationship of the indices in southern and northern atmospheric oscillations (SOI and NAO) to the Ap indices has been revealed. The monthly average Ap amplitude increases before the El Nino warm period, when the SOI index decreases from 0 to ?1.5 and the NAO index increases from ?0.5 to 0.9. The La Nina cold period, when SOI increases from ?0.1 to 1.3 and NAO decreases from 0.7 to ?0.45, begins after a decrease in the Ap index.     

The equatorial ionospheric anomaly in electron content from solar minimum to solar maximum for South East Asia

Median hourly, electron content-latitude profiles obtained in South East Asia under solar minimum and maximum conditions have been used to establish seasonal and solar differences in the diurnal variations of the ionospheric equatorial anomaly (EIA). The seasonal changes have been mainly accounted for from a consideration of the daytime meridional wind, affecting the EIA diffusion of ionization from the magnetic equator down the magnetic field lines towards the crests. Depending upon the seasonal location of the subsolar point in relation to the magnetic equator diffusion rates were increased or decreased. This led to crest asymmetries at the solstices with (1) the winter crest enhanced in the morning (increased diffusion rate) and (2) the same crest decaying most rapidly in the late afternoon (faster recombination rate at lower ionospheric levels). Such asymmetries were also observed, to a lesser extent, at the equinoxes since the magnetic equator (located at about 9○N lat) does not coincide with the geographic equator. Another factor affecting the magnitude of a particular electron content crest was the proximity of the subsolar point, since this increased the local ionization production rate. Enhancements of the EIA took place around sunset, mainly during the equinoxes and more frequently at solar maximum, and also there was evidence of apparent EIA crest resurgences around 0300 LST for all seasons at solar maximum. The latter are thought to be associated with the commonly observed, post-midnight, ionization enhancements at midlatitudes, ionization being transported to low latitudes by an equatorward wind. The ratio increases in crest peak electron contents from solar minimum to maximum of 2.7 at the equinoxes, 2.0 at the northern summer solstice and 1.7 at northern winter solstice can be explained, only partly, by increases in the magnitude of the eastward electric field E overhead the magnetic equator affecting the [E×B] vertical drifts. The most important factor is the corresponding increase in ionization production rate due to the increase in solar radiation flux. The EIA crest asymmetries observed at solar maximum were less significant, and this is probably due to the corresponding increase in ionization densities leading to an increase of the retarding effect of ion-drag on the daytime meridional winds.     

磁暴期间热层大气密度变化

基于CHAMP卫星资料,分析了2002—2008年267个磁暴期间400km高度大气密度变化对季节、地方时与区域的依赖以及时延的统计学特征,得到暴时大气密度变化的一些新特点,主要结论如下:1)两半球大气密度绝对变化(δρa)结果在不同强度磁暴、不同地方时不同.受较强的焦耳加热和背景中性风共同作用,在北半球夏季,中等磁暴过程中夜侧和大磁暴中,夏半球的δρa强于冬半球;由于夏季半球盛行风环流造成的扰动传播速度快,北半球夏季日侧30°附近大气,北(夏)半球到达峰值的时间早于南(冬)半球.而可能受半球不对称背景磁场强度所导致的热层能量输送率影响,北半球夏季强磁暴和中磁暴个例的日侧,南半球δρa强于北半球;春秋季个例中日侧30°附近大气,北半球先于南半球1~2h达到峰值.2)受叠加在背景环流上的暴时经向环流影响,春秋季暴时赤道大气密度达到峰值的时间最短,日/夜侧大气分别在Dstmin后1h和2h达到峰值.至点附近夜侧赤道大气达到峰值时间一致,为Dstmin后3h;不同季节日侧结果不同,在北半球冬季时赤道地区经过更长的时间达到峰值.3)日侧赤道峰值时间距离高纬度峰值时间不受季节影响,为3h左右.在春秋季和北半球冬季夜侧,赤道大气密度先于高纬度达到峰值,且不同纬度大气密度的峰值几乎无差别,表明此时低纬度存在其他加热源起着重要作用.     

Global distribution,seasonal, and inter-annual variations of mesospheric semidiurnal tide observed by TIMED TIDI

Based on TIDI mesospheric wind observations, we analyzed the semidiurnal tide westward zonal wavenumber 1 and 2 (SW1 and SW2) component seasonal, inter-annual variations, and possible sudden stratospheric warming (SSW) related changes. Major findings are as follows: (1) The SW1 has a peak near the South Pole during the December solstice and near the North Pole during the March equinox. (2) The SW2 peaks at 60S and 60N mostly during winter solstices. The SW2 also peaks during late summer and early fall in the northern hemisphere. (3) The QBO effect on the semidiurnal tide is much weaker than that on the diurnal tide. The March equinox northern SW1 zonal amplitude appears to be stronger during the westward phase of the QBO, which is opposite of migrating diurnal tide QBO response. (4) Possible SSW event related changes in the semidiurnal tide are significant but not always consistent. Enhancements in the mid-latitude SW2 component during SSWs are observed, which may be related to the increase of total ozone at mid and high latitudes during SSW events. TIDI observations also show a decrease in the SW2 in the opposite hemisphere during a southern SSW event in 2002. Small increases in the high latitude SW1 in both hemispheres during the 2002 southern SSW event were recorded.     

Longitudinal (UT) effect in the onset of auroral disturbances over two solar cycles as deduced from the AE-index

Statistical study on the universal time variations in the mean hourly auroral electrojet index (AE-index) has been undertaken for a 21 y period over two solar cycles (1957–1968 and 1978–1986). The analysis, applied to isolated auroral substorm onsets (inferred from rapid variations in the AE-index) and to the bulk of the AE data, indicates that the maximum in auroral activity is largely confined to 09–18 UT, with a distinct minimum at 03–06 UT. The diurnal effect was clearly present throughout all seasons in the first cycle but was mainly limited to northern winter in the second cycle. Severe storms (AE > 1000 nT) tended to occur between 9–18 UT irrespective of the seasons whereas all larger magnetic disturbances (AE > 500 nT) tended to occur in this time interval mostly in winter. On the whole the diurnal trend was strong in winter, intermediate at equinox and weak in summer. The implication of this study is that Eastern Siberia, Japan and Australia are mostly at night, during the period of maximum auroral activity whereas Europe and Eastern America are then mostly at daytime. The minimum of auroral activity coincides with near-midnight conditions in Eastern America. It appears that the diurnal UT distribution in the AE-index reflects a diurnal change between interplanetary magnetic field orientation and the Earths magnetic dipole inclination.