Sq（Y）的季节变化和场向电流

本文对中国东部地磁台站链地磁静日变化东向分量进行了分析,有结果表明,在冬、夏季清晨,南北半球之间存在着电离层发电机驱动的场向电流,其方向是从夏季半球到冬季半球;在黄昏,也可能存在方向相反的电流。     

电离层电场半年变化的模拟研究

利用一个中低纬电离层电场理论模式，模拟太阳活动低年、地磁活动平静情况下，中低纬地区电离层电场全年的变化情况．结果显示，单独计算南、北半球(去耦合)得到电离层电场具有明显的周年变化特征，且两个半球电场的相位相差半年左右．而同时计算南、北半球(计及耦合)时，电场则是以半年变化为主，且这种半年变化的幅度和相位随地方时和地磁纬度有变化．提出一个南、北半球耦合电路的简单物理模型给予解释．电路模型初步计算发现，即使两个半球电离层电场分别具有周年变化，只要它们变化的幅度相当，相位相差半年左右，由于跨越南北半球磁力线的耦合效果，耦合的电离层电场会产生明显的半年变化分量．由于缺少连续的电离层电场观测资料，将模拟结果与Richmond基于非相干散射雷达数据建立的经验模式(ISR Model)相比较，结果符合较好．     

模式化分析F区电离层赤道异常槽

利用二维低纬电离层理论时变模式模拟低纬电离层演化，考察影响赤道异常槽位置的物理因素．计算结果显示赤道槽有明显的季节、地方时和经度变化．以１１０°Ｅ为例，北半球夏季期间赤道槽一般在磁倾赤道北侧，最北达３°-３．５°Ｎ，而在北半球冬季期间一般位于磁倾赤道南侧，最南可达４°－５°Ｓ．进一步分析发现，赤道槽季节变化中光化电离率季节改变的影响很小，主要由水平中性风季节变化贡献．计算以８３天为例，白天赤道槽在地理经度１００°Ｅ附近最南，２８５°Ｅ附近最北，与观测特征基本一致．主要是背景大气水平风场的经度差异导致赤道槽位置的经度变化，而非前人认为直接由磁偏角控制的．     

磁暴期间电离层扰动的GPS台网观测分析

给出了一种利用GPS台网观测获取TEC快速变化的计算方法，并将该方法用于东亚一澳大利亚扇区的GPS台网观测数据，分析了2000年7月14—18H大磁暴期间的电离层响应，揭示出电离层暴期间赤道异常峰的压缩和移动等特性．计算结果表明，在站点分布不均匀、原始观测数据不足且随时间跳变等多种不利因素的影响下，这种新的算法仍能保持很好的计算稳定性，并能快速地提取给定时空范围内的三维TEC短时变化的特征，适用于研究电离层暴等情况下引起的TEC扰动．     

火星磁场产生的原因及其分布

构建了一个可以得到火星赤道面上磁场分布的模型. 模型根据卫星观测数据, 提出了火星电离层、磁层顶和磁尾电流片上都各自通有电流的假设. 由电流的连续性条件可知, 这三种背景条件下的电流之间满足一定关系, 即火星磁层顶上的总电流是电离层上的总电流与磁尾电流片上的总电流之和. 这些电流产生的磁场与太阳风磁场共同构成了火星赤道面上磁场分布. 通过计算发现, 采用这种磁场模型得到的结果与目前卫星所观测的结果以及与采用其他方法得到的结果符合得较好.      

一个低纬电离层理论模式

建立一个改进的低纬F层时变理论模式．采用沿磁力线分布的固定网格点，利用算子分裂方法求解离子连续性和动量方程，给出O＋、N2＋、O2＋和NO＋密度随纬度、高度变化的二维分布．对太阳活动高年的春分季节东亚区赤道异常日变化进行的模拟计算，较好地再现了赤道异常的典型特征．计算结果也表明HWM90模式给出的低纬夜间风速可能偏大；东亚区垂直漂移速度可能比美洲区的要小．     

极区顶部电离层离子上行的太阳活动依赖性研究

利用第23太阳活动周DMSP F12,F13和F15卫星数据,分别对南北半球极区顶部电离层离子上行的太阳活动依赖性进行了研究.结果表明,南北半球上行事件对太阳活动的响应特征基本一致,即高（低）太阳活动时,离子上行通量以及上行数密度较大（小）,但是上行速度及上行发生率较低（高）.以南半球高纬为例,计算得到离子上行通量、数密度、速度及发生率在高低太阳活动条件下的比值分别约为2.26,3.35,0.71,0.51.对离子上行太阳活动依赖性的可能原因进行了分析.不同太阳活动水平下,光致电离及高能粒子沉降的差异会导致电离层离子密度的不同,而电离层离子密度的变化会改变离子elax-elax中性大气之间的碰撞频率,这是影响离子上行发生率的一个重要原因.      

1993年9月12—14日磁暴期间磁层—电离层耦合分析

采用具有明确物理意义的多个地磁指数，以及地面台站链观测的地磁和电离层参数，对一次典型磁暴期内从极光区到赤道附近电离层电流、电场演化发展的耦合过程作了具体分析．结果表明，地磁指数和观测参数能较好地说明磁层－电离层耦合理论结果的主要特征．     

大尺度行星波跨赤道传播的E—P通量诊断

利用Nimbus－7卫星温度探测资料，计算了平流层和中间层的风场、位势高度扰动场，进行了行星波E－P通量分析．结果表明，中层大气中的准定常行星波，其定常分量不能跨过赤道上空的零风线，由于其幅度的起伏和相位的变化，激发的瞬变行星波分量不受赤道零风线的限制，可以从冬半球向夏半球传播，也可以从夏半球向冬半球传播．这种跨赤道传播为夏半球行星波的能量来源提供了一种解释．     

低纬电离层f0F2夜间增强的模拟研究

以太阳活动低年冬季为代表,利用二维中低纬电离层理论模式模拟低纬电离层ｆ０Ｆ２夜间增强现象,探索在赤道异常驼峰纬度附近形成该现象的可能因素或物理机制,模式在给定磁子午面内解等离子体输运方程,给出电子及各离子的浓度,速度的时空分布。在所考察条件下,低纬驼峰纬度附近ｆ０Ｆ２模式值夜间出现了明显的增强特征。     

赤道异常峰区电离层的某些特点

由于赤道异常北峰覆盖我国整个南部地带,因此对峰区电离层特征的研究就成为掌握中国电离层特点的关键之一。本文试图对以下六个问题作些介绍和评述:1.逐日起伏和子夜前极大;2.峰位置的移动;3.赤道异常的经度效应;4.不均匀结构引起的强闪烁和快速法拉第衰落;5.顶部电离层的离化突起和中性赤道异常;6.粒子沉降的双峰分布.      

A theoretical model for the magnetic helicity of solar active regions

Active regions on the solar surface are known to possess magnetic helicity, which is predominantly negative in the northern hemisphere and positive in the southern hemisphere. Choudhuri et al. [Choudhuri, A.R. On the connection between mean field dynamo theory and flux tubes. Solar Phys. 215, 31–55, 2003] proposed that the magnetic helicity arises due to the wrapping up of the poloidal field of the convection zone around rising flux tubes which form active regions. Choudhuri [Choudhuri, A.R., Chatterjee, P., Nandy, D. Helicity of solar active regions from a dynamo model. ApJ 615, L57–L60, 2004] used this idea to calculate magnetic helicity from their solar dynamo model. Apart from getting broad agreements with observational data, they also predict that the hemispheric helicity rule may be violated at the beginning of a solar cycle. Chatterjee et al. [Chatterjee, P., Choudhuri, A.R., Petrovay, K. Development of twist in an emerging magnetic flux tube by poloidal field accretion. A&A 449, 781–789, 2006] study the penetration of the wrapped poloidal field into the rising flux tube due to turbulent diffusion using a simple 1-d model. They find that the extent of penetration of the wrapped field will depend on how weak the magnetic field inside the rising flux tube becomes before its emergence. They conclude that more detailed observational data will throw light on the physical conditions of flux tubes just before their emergence to the photosphere.     

Mean solar quiet daily variations in the earth’s magnetic field along East African longitudes

Solar quiet daily (Sq) variation in the earth’s magnetic field along the East African meridian was studied using data of the H, D and Z components recorded with Magnetic Data Acquisition System of SERC. One year data recorded at ten African geomagnetic observatories was used in the analysis of worldwide solar quiet daily variation (Wsq). The study revealed that the focus of Sq (H) in the southern hemisphere lies at the boundary of low and middle latitude region. Noon-time enhancement of Sq (H) was generally noticed at all stations along the meridian, though it is latitudinal dependent in terms of magnitude as it reduces with distance from dip equator. In addition, night-time variations also occur in small magnitude along African meridian in Sq (H) and Sq (Z) which could be attributed to non-ionospheric sources. Semi-diurnal variation was noticed in Sq (D) at all stations except in AAB that is under the influence of electrojet current. Dusk sector calm condition of Sq (D) current was notice in some stations and the same condition was also noticed at dawn sector in some other stations. The usual sunrise maximum and sunset minimum for D component at stations north of dip equator as well as sunrise minimum and sunset maximum was found to increase with distance away from dip equator. Day-time perturbation of Sq current was noticed to be more pronounced in all the three field elements. Mass plots of annual mean hourly value show contrasting phase pattern about the focus in H element and the results of the variations at each region with the associated standard error. It was concluded from the result of correlation coefficients computed that different currents system flowing in opposite directions could be responsible for contrasting patterns.     

The magnetic fields of Mercury,Venus and Mars

Just as clearly as Mariner 10 established that Mercury has an intrinsic magnetic field, the Pioneer Venus orbiter has established that Venus has no significant intrinsic field. This is perhaps the opposite of what might be expected. Mercury, a small planet might be expected to cool rapidly and its internal dynamo to cease, while Venus, which is almost as large as the Earth, should not have lost much heat. On the contrary the source of energy of the Mercury dynamo appears to be extant whereas that of Venus appears to be extinct.The existence of a Martian magnetic field is controversial. No unambiguous signature of a Martian magnetic field has been reported. If the field on the nightside of Mars is of planetary rather than solar origin the Russian Mars spacecraft observations indicate the Martian dipole lies near the planetary equator rather than its pole.     

磁层亚暴时环电流的局部加速机制

本文讨论了一种使环电流增强的局部湍流发电机过程。由于磁层内部的磁场很强,其位形基本满足无作用力磁场近似。另一方面,磁场的涨落值与其平均值相当。当涨落场电动势局部增强时,可以使平均场以及平均电流密度增强,形成环电流的增强。这时,亚暴过程中维持环电流所需要的能量是由湍流或波动的涨落场提供的,这是一种使粒子局部加速的过程。本文还具体讨论了一种α2湍流发电机模型,求出了具有随时间增长特性的本征模式。将分析结果应用于讨论亚暴时的环电流过程,并进行了定量估计。      

用经验模式参数研究电离层发电机效应

本文利用MSIS-86和IRI-86模式的基本参数,求得热层风系和电导率的三维分布;继而从发电机理论得到了电离层电位及层电流密度在北半球的分布和变化。本研究将大量数据统计平均的大气模式参数与热层、电离层理论研究联系了起来。     

利用TIE-GCM模式计算电离层电流及夜间电离层磁场

电离层电流产生的磁场是地磁场卫星测绘时需要剔除的干扰源.利用电离层热层模式TIE-GCM计算电离层中的中性风、重力驱动和压强梯度等形成的电离层电流的全球分布,分析电流在特定位置产生的磁场及磁场三分量随纬度的变化规律.结果表明,E层尤其是磁赤道和极区的电流密度较大,可达103nA·m-2量级,F层电流密度量级约为10nA·m-2.在磁静日（Kp≤ 1）夜间22:00LT-04:00LT,电离层电流在中低纬度（南北纬50°之间）产生的磁场量级为几个nT,且磁场的南北向分量和径向分量基本大于东西向分量.通过与CHAMP卫星磁测数据分析比较,发现TIE-GCM模式计算电离层干扰磁场在中低纬度可以取得较好的结果,但在高纬度地区的效果不理想,还需进一步改进模式以提高计算精度.      

Variations of the O(D) and O(S) peak volume emission rates without direct solar effects

Airglow volume emission rates of the O(¹D) red line at 630.0 nm and the O(¹S) green line at 557.7 nm were measured by the Wind Imaging Interferometer (WINDII) on the Upper Atmospheric Research Satellite (UARS) during 1991–1997. Focus of this study is on the peak volume emission rates of the two airglows after removing the direct solar effect, which are referred to as the ‘dark’ peak emission rates. The main results are as follows. For the red line emission, at low and mid-latitudes the daytime variation does not have a clear pattern except an enhancement at dusk; during nighttime there is an enhancement in the equatorial region at 20–03 h, which has a semiannual variation with maxima at equinoxes; at solstices the daytime O(¹D) dark emission rate is stronger in winter than in summer. For both the green line E-and F-layers the distribution of the dark peak volume emission rate is symmetric about noon in all seasons, symmetric about the equator at equinoxes, and stronger in summer than in winter. The O(¹S) E-layer is profoundly affected by tides. For the first time the diurnal and semidiurnal amplitudes for the emission rates are derived using 24-h zero-sun data. The amplitude of the diurnal tide can be as large as 20% of the mean peak volume emission rate, and has maxima at the equator and about 40°N/S, and minima at about 20°N/S. The daily diurnal maximum is at noon at the equator but at midnight at 40°N/S. There is a clear semiannual variation of the diurnal amplitude in the equatorial region with maxima at equinoxes. The amplitude of the semidiurnal tide is mostly less than 10% of the mean peak volume emission rate with maximum amplitudes at noon and midnight. There is an annual variation of the semidiurnal amplitude at mid-latitudes peaking in summer. Aurorae appear in all three emission layers day and night. The green aurorae are brighter than the red aurorae, and the green E-layer aurorae are 2–3 times stronger than the F-layer aurorae. The green aurora has a clear midday gap in the F-layer and an afternoon gap in the E-layer. The red aurorae are particularly strong in the so-called cusp region at equinoxes.     

反向赤道电集流与磁层扰动

对印度Trivandrum站第21太阳活动周内地磁H分量分析表明,不仅在磁扰日及其随后的静日内,强磁扰对赤道电集流有显着作用,即使在持续静日期间,较弱的磁扰仍然对赤道电离层有很大影响。磁静日昏侧出现反向(西向)电集流是正常现象,弱磁扰是使此反向电流消失的可能机制。      

Impact of rogue active regions on hemispheric asymmetry

The solar dipole moment at activity minimum is a good predictor of the strength of the subsequent solar cycle. Through a systematic analysis using a state-of-the-art $2\times 2$D solar dynamo model, we found that bipolar magnetic regions (BMR) with atypical characteristics can modify the strength of the next cycle via their impact on the buildup of the dipole moment as a sunspot cycle unfolds. In addition to summarizing these results, we present further effects of such “rogue” BMRs. These have the ability to generate hemispheric asymmetry in the subsequent sunspot cycle, since they modify the polar cap flux asymmetry of the ongoing cycle. We found strong correlation between the polar cap flux asymmetry of cycle i and the total pseudo sunspot number asymmetry of cycle $i+1$. Good correlation also appears in the case of the time lag of the hemispheres of cycle $i+1$.