ACE飞船观测的行星际磁场准27天重现周期和结构

 ACE飞船发射于1997年8月15日,将维持到2024年,位于日地连线重力平衡点L1。本文采用ACE飞船行星际磁场观测数据,基于GSE坐标系统,确定L1点的行星际磁场主体方位,进而将行星际磁场观测数据转换为极性符号序列。对于序列中的任一时间点,通过改变以它为中心的子序列探测行星际磁场的准27d重现周期和结构,再应用模板匹配方法识别重现结构,最后采用分段常值函数拟合获得分段稳定的周期和结构。得到的主要结果如下：(1) 1999—2008年间,IMF重现周期绝大多数在(27±2)d范围内,只有1个例外,即2001年10月27日10:00—11月28日12:00时间内,重现周期为21d14h;(2) 2001年1月8日12:00—2004年7月17日04:00,IMF为2扇瓣结构,2004年7月17日05:00—2007年6月30日23:00,IMF为4扇瓣结构,2007年7月1日00:00—2008年12月31日23:00,IMF为2扇瓣结构。     

热层大气赤道异常的研究进展

热层大气赤道异常是指热层大气存在类似电离层赤道异常的驼峰结构,但其南北驼峰出现于磁纬±20~30°区域.热层赤道现象早在40年前就被发现,然而其形成机制一直是电离层学界研究的热点问题.前人陆续提出了化学加热及纬向风场拖曳作用等假说来解释热层赤道异常的形成,但基于这些假说得到的低纬热层结构与观测不符.最近研究发现,热层赤道异常槽与电离层驼峰的形成原因不同,离子与中性大气的场向拖曳作用形成热层赤道槽,且离子与中性气体相互碰撞引起的能量交换是热层赤道异常驼峰的形成机制.本文简述热层大气赤道异常的研究进展以及存在的科学问题.     

磁尾等离子体片边界层场向电流与行星际磁场时钟角的关系

根据ClusterII卫星的探测数据,对1 839个磁尾等离子体片边界层场向电流事件与行星际磁场(IMF)时钟角Φ的关系进行了统计分析。结果显示等离子体片边界层场向电流的发生率明显受到IMF时钟角的调控:当0°<|Ф|<90°,场向电流发生率随IMF时钟角的变化曲线为一"V"型结构。当90°<Ф<180°时场向电流发生率保持在很高的水平上;当-180°<Ф<-90°时,场向电流的发生率先减小后增大,其拐点在Ф=-130°附近。这说明场向电流不仅受行星际Bz的影响,也受行星际磁场By的影响。     

不同大气稳定度分类方法的比较研究

根据河北海兴核电厂址气象站2015年1月1日～2015年1月15日期间10 m和100 m高度处风速和温度观测气象资料,分别用温度梯度分类法(ΔT/ΔZ),温度梯度—风速法(ΔT-u)、理查森数(Ri)法、莫宁-奥布霍夫长度(L)法判定大气稳定度,结果表明:主导风都处于SW-WSW风向上,ΔT/ΔZ法与ΔT-u法出现稳定类天气最多,中性天气次之; Ri法与L法稳定类天气最多,不稳定性天气次之。对四种大气稳定度分类方法做对比分析,ΔT/ΔZ法与ΔT-u法的测量比较简单,能够快速的判定大气的稳定度。Ri法与L法对观测资料要求较多,能够较准确的判定大气稳定度。     

子午面磁层顶位形结构的MHD模拟研究

本文基于太阳风-磁层-电离层耦合的全球磁流体力学(MHD)数值模拟,研究几种典型的太阳风动压和行星际磁场条件下,地球子午面上方磁层顶的位置和形状特征,以及磁层顶位形参数日下点距离和磁层顶张角随行星际条件的变化规律。模拟结果表明:正午午夜子午面磁层顶位形具有内凹结构,当行星际磁场为南向时,随磁场强度增强,日下点距离减小;行星际磁场为北向时,随磁场强度增强,日下点距离增大。动压增大,日下点距离减小。南向磁场强度增强,磁层顶张角变大。这些模拟结果与基于卫星数据的高纬经验模型(B00)以及(Schield)模型的经验结论相吻合,说明MHD模拟是研究磁层顶位形的有效工具。特别是在高纬穿越数据的获得受限时,基于对磁层顶位形的物理理论研究构建的数值模拟数据是解决这一问题的有效途径。     

第一个进入星际空间的人造物体——旅行者1号

2013年9月13日凌晨2:00(北京时间),美国国家航天局(NASA)正式确认旅行者1号(Voyager 1)探测器已于2012年8月25日飞出太阳系,进入星际空间。这是目前离地球最远的人造飞行器,也是第一个进入星际空间的人造物体,是人类太空探索史上的壮举。旅行者号科学团队认为,旅行者1号在2012年8月25日就进入了星际空间。这一结论是基于两个方面的证据,首先,2012年8月25日获得的数据显示,     

平流层风场的火箭观测及其与模式风场的比较

美国西北研究机构(NWRA:NorthWest Research Associates)发布了1963-1992年期间在Kwajalein岛礁(8°N,167°E)上共计1862次火箭探测的平流层风场和温度剖面.本文选取测量较为连续的1969-1972年期间共计345个风场剖面来研究平流层月平均风场及其两年变化、年变化和半年变化的特征.同时与目前应用较为广泛的风场模式HWM07(Horizontal Wind Model:2007)和CIRA86(COSPAR International Reference Atmosphere:1986)进行了比较.火箭测量的4年逐月平均纬向风在夏季为西向风,并在8月41km处达到最大值45ms-1;在冬季变为东向风,并在3月57km处达到最大值47ms-1.全年的经向风在60km以下基本上是北向风且风速低于10ms-1.纬向风在20~35km之间以两年变化为主,振幅在10~17ms-1之间;在45~55km之间以半年变化为主,振幅是16~25 ms-1之间;在5km以上以年变化为主,振幅在16~25 ms-1之间.测量风场与HMW07相比,HWM07的西向风在7月46km处达到最大值38ms-1,东向风在2月60km处达到最大值37ms-1,均小于测量风场的峰值.测量风场与CIRA86相比,CIRA86的西向风在7月49km处达到最大值36ms-1,东向风在3月60km处达到最大值43ms-1,仍小于测量风场的峰值.测量风速稍大于模式风速的可能原因之一是测量风场包含了背景风场和各种波动成分,而模式风场是气候学平均的结果;此外,HWM07和CIRA86虽然包含了不少探空火箭数据,但并没有包含在Kwajalein岛礁的测量资料.     

钠激光雷达对中间层顶大气温度和风场的探测

中高层大气温度和风场是研究中高层大气波动的重要参数.钠高光谱分辨率激光雷达能够对中间层顶(80-105km)大气温度和风场进行高精度观测.2011年中国科学技术大学成功研制了我国首台高光谱分辨率钠测温测风激光雷达系统.文中对该激光雷达系统进行了详细介绍,其中包括探测的基本原理,发射机,接收机和采集控制部分的设计.给出了钠测温测风激光雷达于2011年12月9日晚同时探测的大气温度、纬向风、经向风和钠原子密度的结果.结果发现中间层顶区域大气温度、纬向风、经向风变化范围较大,分别是175K~235K,-70~60m/s,-100~110m/s,有明显的半日或周日潮汐振荡的成分.探测结果表明中国科学技术大学钠测温测风激光雷达可对中间层顶区域温度和大气风场进行高时空分辨率的探测,其探测数据对于研究中高层大气动力学具有重要的意义.     

地电荷的电容结构发电机制研究

由地电荷与地球自转运动发电原理及国际参考地磁场(IGRF)标准模型所确定的地球磁场能量的分布,经分析、推论,建立了地电荷的电容结构发电机制,并由此而建立了全球电磁场结构和等效电路.此电磁场发电机制由磁场和电路双正交结构组成,磁场正交结构为偶极子场和非偶极子场,电路正交结构为地电荷运动的等效发电环电流和电源及负载电阻组成的全球等效电路.电荷运动的等效发电环电流产生的是偶极子场;电源及负载电阻组成的全球等效电路产生的是非偶极子场.地电荷的电容结构发电机制所确定的地磁场结构模型,与现地磁场结构模型完全不同,特别是极区拱形地磁场及其双向地磁场边界特性.此模型对极光、极光椭圆区、极区双向电集流和极区离子上行,对大气电场、大地自然电位的形成和变化趋势,对行星际磁场BZ及其南、北分量BS和BN的生成,及行星际南向分量BS与磁暴的关系,以及对地震与偶极子场、非偶极子场之间的关系等,都作出了较合理的阐释.     

Andes上空中间层和低热层中大气惯性重力波的激光雷达观测

利用Andes观测站(30. 3°S,70. 7°W)激光雷达2016年6月8～9日共11. 6 h的风场、温度以及钠原子数密度的观测数据,研究了一个在中间层顶区域惯性重力波活动事件。谱分析表明,这个惯性重力波的周期约6. 6 h,垂直波长约7. 5 km,水平波长约826 km。根据矢端曲线法分析发现,此惯性重力波的传播方向大约为西偏北38. 6°。计算出它的垂直群速度约0. 2 m·s~(-1),水平群速度约22. 9 m·s~(-1)。射线追踪结果表明,上传惯性重力波可能来自于平流层的急流区域。虽然该惯性重力波不能达到不稳定性的阈值,但是理查德森数和浮力频率显示,由于不同扰动分量的叠加,导致了在一些高度和时间上,动力学的发生和对流不稳定性的存在。因此,叠加效应引起的不稳定性可能会对中间层-低热层中波的饱和度和幅度约束有显著影响。同时利用重力波偏振关系和惯性重力波纬向风扰动,计算出了经向风、温度和大气密度扰动,同时观测的经向风和温度扰动与计算的结果一致,表明观测到的准单色惯性重力波能很好满足重力波偏振关系。另外,计算得到的大气密度扰动与观测的钠原子数密度扰动相位一致,证实了中间层-低热层区域的钠原子可以作为重力波的示踪物。     

Reduced drag coefficient for high wind speeds in tropical cyclones

The transfer of momentum between the atmosphere and the ocean is described in terms of the variation of wind speed with height and a drag coefficient that increases with sea surface roughness and wind speed. But direct measurements have only been available for weak winds; momentum transfer under extreme wind conditions has therefore been extrapolated from these field measurements. Global Positioning System sondes have been used since 1997 to measure the profiles of the strong winds in the marine boundary layer associated with tropical cyclones. Here we present an analysis of these data, which show a logarithmic increase in mean wind speed with height in the lowest 200 m, maximum wind speed at 500 m and a gradual weakening up to a height of 3 km. By determining surface stress, roughness length and neutral stability drag coefficient, we find that surface momentum flux levels off as the wind speeds increase above hurricane force. This behaviour is contrary to surface flux parameterizations that are currently used in a variety of modelling applications, including hurricane risk assessment and prediction of storm motion, intensity, waves and storm surges.     

Observations of thermospheric vector wind over Yellow River Station during auroral substorm events

Strong disturbances associated with auroral substorms originate from the ionosphere–magnetosphere owing to the effects of the solar wind, and the wind field in the ionosphere is related to such substorm activity. Here, we describe the analysis of four auroral substorm events, for which we employed an all-sky Fabry–Perot interferometer to observe the two-dimensional horizontal wind field and combined the results with data from an all-sky charge-coupled device imager, a fluxgate magnetometer installed at Yellow River Station, and the Super Dual Auroral Radar Network. The results demonstrate that, during auroral substorms, the vector wind field is related closely to variations in the ion drift and geomagnetic field. Moreover, we observed a changing wind field of approximately 300 m/s in response to variations in the electric and magnetic fields (likely caused by ion drag) and a disturbance of about 200 m/s that we attribute to the interaction of Joule heating and ion drag.     

An analysis of interplanetary sources of geomagnetic storm during November 7–8, 1998

We analyzed the properties of the solar wind appeared during November 7–8, 1998. Results show that the spaceship ACE spotted a shock （hereinafter referred to as the first shock） at 07:33 UT, November 7. The sheath appeared from the first shock to 22:00 UT November 7. A magnetic cloud-like （MCL） was observed during the period from 22:00 UT November 7 to 11:50 UT, November 8. Another shock was observed at 04:19 UT, November 8 （the second shock）. It is apparent that the second shock has entered the rear part of the MCL （MCL₂）, though the former part of the MCL （MCL₁） was not affected by the second shock. The main phase of the geomagnetic storm is split into three steps for the convenience of SYM-H index analysis. Step 1 covers the period from the sudden storm commence （SSC） at 08:15 UT, November 7 to the moment of 22:44 UT, November 7. Step 2 starts from 22:44 UT, November 7 and ends at 04:51 UT, November 8. The last step runs from 04:51 UT, November 8 to 06:21 UT, November 8. Step 2 has played a key role in the main development phase of the geomagnetic storm. Analysis of the solar wind properties associated with the main phase shows that the three steps in the main phase have sheath, MCL₁, and MCL₂ as their respective interplanetary source. Specifically, the sheath is covered by the solar wind data from 07:33 UT to 22:00 UT, November 7, MCL1 by the solar wind data from 22:00 UT, November 7 to 04:19 UT November 8, and MCL₂ by the solar wind data from 04:19 UT to 05:57 UT, November 8. MCL₁ had a strong and long lasting so UTh directed magnetic field, allowing it to play a key role in the development of the main phase. MCL₂ made a much smaller contribution to the main development phase, compared with MCL₁.     

First observation of thermospheric neutral wind at Chinese Yellow River Station in Ny-Ålesund, Svalbard

A compact and cost-effective all-sky Fabry-Perot interferometer, which is produced by Wuhan University and used for the observation of the thermospheric neutral wind, was installed at Chinese Yellow River Station in Nylesund, Svalbard in November 2010, and continuously operated in last two winter seasons. The 92-day all-sky interference data acquired from November 1, 2011 to February 26, 2012 were collected to get the velocity of thermospheric neutral wind, which was calculated from the Doppler shift caused by the movement of oxygen atom at the different layers. The database was divided into two periods: (1) The OI 557.7 nm emission was observed from November 1, 2011 to January 12, 2012. Observations showed that the velocity of horizontal wind is normally less than ～40 m/s on the quiet condition, and exceeded 100 m/s on the disturbed condition; and (2) the OI 630.0 nm emission was observed from January 13, 2012 to February 26, 2012. Observations showed that the velocity of horizontal wind is normally less than ～200 m/s, and enhanced to over 300 m/s on strong magnetic activities. It shows that the velocities of meridional and zonal wind are more consistent with the velocities calculated from the model HWM07 at the higher layer, especially for the zonal direction at nightside auroral regions. Ion drag and Joule heating were the two important processes considered in the analysis of the relationship between the wind pattern and aurora, suggesting that wind speed would be increased and accelerated in the direction perpendicular to the aurora arc when the aurora activity becomes strong.     

Comparative study of a substorm event by satellite observation and model simulation

A substorm event has been simulated for the first time by using SWMF (Space Weather Modeling Framework) developed by the University of Michigan. The model results have been validated using Geotail and Cluster satellite observations. The substorm onset occurs at 22:08 UT on September 28, 2004, as identified from FUV WIC observations on the NASA IMAGE spacecraft. SWMF can couple effectively the magnetosphere, inner magnetosphere and ionosphere processes and is driven by the solar wind and IMF (Interplanetary Magnetic Field) parameters, which are measured by ACE satellite and time delayed to the upstream boundary of the model. It shows that (1) SWMF can predict well the large-scale variations of the magnetospheric magnetic field and ionospheric currents during the substorm event; and (2) the accuracy of the time delay of the solar wind from ACE to the outer boundary of the model has great effects on the model results. Finally, the substorm trigger mechanism has been discussed and the way of improvement of the model has been pointed out.     

基于无线电掩星观测的火星电离层观测研究进展

火星电离层早期的观测数据非常少,除了Viking登陆器对火星电离层的在位测量外,火星电离层的主要物理信息是通过掩星观测方法得到的.近年来,Mars Global Surveyor和Mars Express轨道器通过掩星观测的方法对火星的上层大气和电离层进行了长期的观测,得到了大量的火星电离层电子密度廓线资料.火星电离层受到来自太阳EUV和X射线辐射、太阳风、太阳耀斑、中性大气、表面壳磁场、宇宙射线、流星等多种因素的影响,使其结构发生瞬态或季节性的变化.本文介绍了行星无线电掩星探测的基本原理和技术特点,回顾了国内外科学家们基于已有的火星掩星观测数据（主要是Mars GlobalSurveyor和Mars Express）在火星电离层研究中的一些最新科学成果,并详细介绍了火星电离层的结构和火星夜间电离层的主要特征.     

基于MM5的轮毂高度风场数据获取方法

 从MM5模式垂直坐标定义出发,将大气静力学方程应用于整个大气,并在相邻层之间进行等温大气假设,进行求解层的高度,从而可由MM5的模拟结果中得到不同轮毂高度风场数据。对比验证表明该方法可靠,为从MM5结果获取轮毂高度的风场数据提供了另一种简便而准确计算的方法。     

Enhanced anti-sunward flow near local noon during a period of horizontal IMF and high solar wind velocity <Emphasis Type="Italic">V</Emphasis><Subscript><Emphasis Type="Italic">Y</Emphasis></Subscript>

It is believed that a southward interplanetary magnetic field (IMF) is mainly responsible for the energy input from solar wind into the magnetosphere. This paper presents an unusual case of strong anti-sunward plasma flow (up to 2 km/s) in the polar cap ionosphere and large cross-polar cap potential (CPCP) during a period of horizontal IMF (|B _Z | < 2 nT) observed by both ACE (at the L1 point) and Geotail (on the dusk flank of the magnetosheath). The CPCP is even higher than that under preceding B _Z ≈ −23 nT. Furthermore, GOES8 observed that the magnetosheath field turns northward as the anti-sunward plasma flow and CPCP start to increase, which implies that the magnetosheath field interacting with the Earth’s magnetopause has significantly rotated and differs from the IMF observed by ACE and Geotail. In accordance with previous theoretical work, we suggest that the magnetic field line draping produces a southward magnetosheath field and enhances anti-sunward plasma flow and the CPCP.     

Magnetic Storm Effects in the Auroral Ionosphere Observed with EISCAT Radar -Two Case Studies

Storm-time changes of main plasma parameters in the auroral ionosphere are analyzed for two intense storms occurring on May 15, 1997 and Sept. 25, 1998, with emphasis on their relationship to the solar wind dynamic pressure and the IMF Bz component. Strong hard particle precipitation occurred in the initial phase for both storma,associated with high solar wind dynamical pressure. During the recovery phase of the storms, some strong particle precipitation was neither concerned with high solar wind pressure nor southward IMF Bz. Severe negative storm effects depicted by electron density depletion appeared in theF-region during the main and recovery phase of both storms, caused by intensive electric field-related strong Joule/frictional heating when IMF was largely southward. The ion temperature behaved similarly in E- and F-region, but the electron temperature did quite different, with a strong increase in the lower E-region relating to plasma instability excited by strong electric field and a slight decrease in the F-region probably concerning with a cooling process. The field-aligned ion velocity was high and apparently anticorrelated with the northward component of the ion convection velocity.     

建筑群不均匀性对拖曳力影响的风洞测压实验

针对建筑群不均匀性缺乏系统的研究方法以及多数处于定性研究的现状,从建筑几何结构的形态学角度出发,采用迎风面积指数、平面面积指数、形状指数和综合非直线系数表达建筑群的不均匀性.风洞实验中采用刚性模型测压的方法进行建筑表面压力的测量,并设计了悬浮实验平台直接测量整个区域所受的拖曳力.实验结果表明,分布在较大平面区域内各建筑的单体拖曳力系数沿风向的变化趋势近似为一条热容模式的衰减曲线;利用有代表性的建筑表面压力测量结果求取的整个区域拖曳力系数和基于拖曳力直接测量的拖曳力系数具有相同的趋势,但普遍大10%~20%;对比可知,地面粗糙度改变对模型表面风压差系数的分布影响不显著,综合非直线系数为1.332 5的工况较1.177 5的工况拖曳力系数减小约17.7%,H型建筑表面风压差系数分布与矩形建筑不同,其对气流的强烈作用造成拖曳力系数约34.6%的增加.