Worldwide features of the strength of recurrent geomagnetic activity

Variation of the strength of recurrent geomagnetic activity, which occurs just before a sunspot minimum, with local time is studied for a network of observatories covering different latitude and longitude zones. For this purpose, hourly averages of horizontal intensity(H) for each UT hour for 173 days, which are totally free of disturbances due to solar transients, have been subjected to spectral analysis. Well-defined spectral peaks associated with periodicities of 28, 14 and 9 days were present in almost all the spectra. The pattern of daily variation of the strength of the 27-day signal changes from a diurnal one at low latitudes to a semi-diurnal one near the Sq focus and in this region, the 14-day signal appears to have an independent origin irrespective of the longitude zone. A study of 27-day oscillation in mean dailyH field also indicates that apart from ring current modulation, both Sq and electrojet fields also undergo 27-day oscillations during the declining phase of a solar cycle possibly through the ionospheric wind system.     

146-day signal in the geomagnetic field—a probable association with the periodicity of the solar flare index

Results on the spectral analysis using geomagnetic field at three low latitude stations and the planetary magnetic activity index have shown peaks in the power densities in a broad band centred around 146-day period. This periodic behaviour appears to be close to that shown by the solar flare activity index for the same interval. It is suggested that the geoeffectiveness of the flare activity signal in different phases of the solar cycle can be better worked out using long series of ground-based geomagnetic data.     

North-south asymmetry in response of geomagnetic activity to different solar events

Study of the response of geomagnetic activity to five different kinds of solar events reveals that an average north-south asymmetry of about 15% exists which diminishes with enhanced geomagnetic activity. The response of the geomagnetic field is quite significant only when high speed solar wind stream in association with sector boundary of interplanetary magnetic field (IMF) or solar proton streams near sector boundary sweeps past the earth. When the frequency of occurrence of indices of geomagnetic activity is considered, the index zero shows a marked difference in its response characteristics for the southern hemisphere. This appears to be a real feature and not attributable to any artefact of the index or its derivation.     

A model for solar quiet day variation at low latitude from past observations using singular spectrum analysis

Singular spectrum isolates significant principal components in a time series from the embedded noise. This tool-kit is used to reconstruct trend-free individual time series, formed by restricting the mean monthly hourly values of geomagnetic field to one hour at a time at a low latitude station Alibag (dipole latitude 9.5°N). Each reconstructed component is extrapolated over the next 12 values using an autoregressive model based on Burg’s maximum entropy algorithm. Details of a numerical approach to increase the reliability of extrapolation are highlighted. The extrapolated reconstructed components are then combined to generate predicted monthly values for each hour. The mean diurnal variation for any month obtained from the extrapolated individual hourly time series compares favorably with the observations. This approach to Sq(H) modelling incorporating both long and short term variations will be beneficial in the derivation of Dst index.     

The interplanetary magnetic field: Radial and latitudinal dependences

Results of the analysis of spacecraft measurements at 1–5.4 AU are presented within the scope of the large-scale interplanetary magnetic field (IMF) structure investigation. The work is focused on revealing of the radial IMF component (B _r ) variations with heliocentric distance and latitude as seen by Ulysses. It was found out that |B _r | decreases as ～r ^?5/3 in the ecliptic plane vicinity (±10° of latitude), which is consistent with the previous results obtained on the basis of the analysis of in-ecliptic measurements from five spacecraft. The difference between the experimentally found (r ^?5/3) and commonly used (r ^?2) radial dependence of B _r may lead to mistakes in the IMF recalculations from point to point in the heliosphere. This can be one of the main sources of the “magnetic flux excess” effect, which is exceeding of the distantly measured magnetic flux over the values obtained through the measurements at the Earth orbit. It is shown that the radial IMF component can be considered as independent of heliolatitude in a rough approximation only. More detailed analysis demonstrates an expressed |B _r | (as well as the IMF strength) increase in the latitudinal vicinity of ±30° relative to the ecliptic plane. Also, a slight increase of the both parameters is observed in the polar solar wind. The comparison of the B _r distributions confirms that, at the same radial distance, B _r values are higher at low than at high latitudes. The analysis of the latitudinal and radial dependences of the B _r distribution’s bimodality is performed. The B _r bimodality is more expressed at high than in the low-latitude solar wind, and it is observed at greater radial distances at high latitudes. The investigation has not revealed any dependence between B _r and the solar wind speed V. The two-peak distribution of the solar wind speed as measured by Ulysses is a consequence of a strong latitudinal and solar cycle dependence of V. It is shown that the solar wind speed in high latitudes (above ±40°) anti-correlates with a solar activity: V is maximum during solar-cycle minima and minimum at the maximum of solar activity.     

Theory for preliminary negative impulse in storm sudden commencement inH at equatorial stations

It is shown that the storm sudden commencement (SSC) inH field at low latitude station consists of only a positive excursion when the interplanetary shock due to the solar plasma impinging on the magnetosphere is associated with a southward excursion of the interplanetary magnetic field (IMF). When the signature of SSC at low latitude station consists of a preliminary negative excursion preceding the main positive excursion of theH field, the solar plasma causing the compression is associated with a northward excursion of the IMF. It is suggested that the signature of SSC(H) at equatorial stations is the result of combined effect of the compression of magnetosphere by the solar plasma as well as due to the electric field effects associated with the velocity of the solar plasma (v) interacting with the northward component (Bz) of the interplanetary field (i.e.,E =−v _x Bz).     

Variations in solar and geomagnetic activity with periods near to 1.3 year

It is known that solar wind velocity fluctuates regularly with a period of about 1.3 years. This periodicity (and other signals with periods near to 1.1 and 0.9 years) has also been observed in biological data. The variation is a temporary feature, mostly being observed in the early 1990s. Here, the occurrence of these periodic signals in solar and geomagnetic activity between 1932 and 2005 has been investigated. The signal with 1.3 year period is present in geomagnetic activity only in a short interval after 1990 and to a lesser extent around 1942. At other times the signal is very weak or not present at all. Other periods are much lower amplitude and appear only sporadically throughout the time investigated. A connection between these periods and solar cycles (e.g. different even or odd cycles) has not been proven. It is possible that there is a long-term periodicity in the occurrence of the 1.3 year period but the time series data available is insufficient to confirm this. There are no such periodicities in solar activity. In order to gain a greater understanding of these periodic signals, we should search for their origin in interplanetary space.     

地磁总强度梯度的计算与分析

不仅要知道地磁场的分布规律,而且要知道地磁场梯度的分布规律。本上根据地磁场的高斯理论和地磁场的球谐模型,计算出中国及其邻近地区地磁总强度的水平梯度(南北方向和东西方向)和垂直梯度,绘制出相应的等值线图,并分析了总强度梯度的分布规律。地磁总强度的水平梯度和垂直梯度,主要随纬度变化,与经度关系不大。值得注意的是在我国的中心地区,地磁总强度的水平梯度值最大。     

Fairweather atmospheric electricity at Antarctica during local summer as observed from Indian station,Maitri

Surface measurements of the atmospheric electrical parameters like Maxwell current, electric field and conductivity studied at the Indian station, Maitri (70.75° S, 11.75° E, 117 m above mean sea level), Antarctica, during austral summer have been analyzed for the years 2001 to 2004. A total of 69 days were selected which satisfied the ‘fairweather’ conditions, i.e., days with absence of high winds, drifting or falling snow, clouds, and fog effects. The diurnal variation curve of electric field and vertical current averaged for 69 fairweather days is a single periodic with a minimum at 03:00 UT and a maximum near 19:00 UT, which is very similar to the Carnegie curve. The correlation coefficient between these measured parameters has a high value (more than 0.9) for all the days. During fairweather days the measured current and field variations are similar and hence it is clear that the conductivity is more or less stable. During magnetically disturbed days, the dawn-dusk potential drop has clear influences on the diurnal variation and it modifies the conductivity. Apart from the day-to-day variation in low latitude thunderstorm activity, there are diurnal, seasonal, inter-annual variations in the electric potential and the currents, as well as solar influences on the measured parameters. This study will help us to examine the impact of solar and geophysical phenomena like solar flares, geomagnetic storms and substorms on the global electric circuit.     

Variation of the 0+ ion density during low and high solar activity as measured by the SR0SS-C2 satellite

The O⁺ ion density measured by the SROSS-C2 satellite during solar minima (year 1995, F_10.7 = 77) and maxima (year 2000, F_10.7 = 181) has been analyzed for studying diurnal, seasonal, latitudinal and geomagnetic variations. The study region covers an area encompassed between 5-3 5° N latitude and 65-95° E longitude over India at a ~500 km altitude (F2 region). The year 2000 shows significant enhancement in the annual average of O⁺ ion density and attainment of post sunset secondary enhancement compared to 1995. Attributed to photoionization, daytime shows a maximum ionization compared to nighttime. However, attainment of post sunset secondary maxima is attributed to the strong pre-reversal enhancement in the vertical E x B drift. The effect of geomagnetic activity Kp through the E x B drift dynamic movement on O⁺ ion density distribution studies indicates periodicities of seven and nine days in 1995 and 2000, respectively, and polynomial dependency of the O⁺ ion density on geomagnetic activity Kp. Further on, stratification of the O⁺ ion density according to latitude (5-35° N) indicates high density in mid-latitudes (12-24° N) compared to high and low latitudes, except in the winter of 1995, which shows a distinct trend (i.e., density decreases with increasing latitude).     

Daily variation of geomagnetic field at low latitudes associated with stable solar wind flow

Mean diurnal variation ofH at low and equatorial latitudes is computed for days in the vicinity of passage of ‘quiet’ solar wind. It is shown that the prepassage magnitude of the diurnal variation is appreciably larger when compared to post-passage intervals at low latitudes but the difference vanishes in the electrojet region. It is suggested that the Sq current system moves towards dip equator immediately following quiet wind conditions relative to earlier periods. It is also shown that during conditions of stable solar wind, the solar wind proton density is inversely related to the electrojet strength, while at low latitudes outside the jet influence, there is no clear association.     

Spectral characteristics of low latitude Pc3 geomagnetic pulsations in south-east Australia

Geomagnetic pulsations in the Pc3 period range (10–45 sec) were recorded simultaneously in south-east Australia using an array of four low latitude induction coil magnetometers over a longitudinal range of 17° atL=1·8 to 2·7. Geomagnetic data from March 25 to September 21, 1982 were digitized and spectral studies were carried out from Grey scale digital (GSD) dynamic spectra and contour sonagrams. Similar wave spectra were generally seen at the three stationsWM, BH andNC in the same latitude with Pc3 waves mostly being observed in the 40–45 mHz band. In addition the higher latitude station (LN) also showed lower frequency Pc4 bands (≈ 10mHz) on some days but higher frequency bands (60–80mHz) on others. Sometimes completely different wave frequencies were observed on theX andY components with the stations in the same latitude generally showing similar spectra on the corresponding components. Dynamic spectra also indicated that wave energy often turned off and on abruptly over short intervals of time implying solar wind control and Pc3 pulsation activity. A band harmonic structure was occasionally seen in wave spectra at the azimuthal stations mainly on theX component during the local afternoon with a harmonic spacing (Δf) of ≈ 10 mHz.     

Validate global mapping of internal lunar magnetic field

In this work, we report a global mapping of vector lunar magnetic field based on new method of separation of internal and external fields. The magnetic measurements collected during the lifetime of lunar prospector (LP) extended mission during 1999 were strongly disturbed by the solar wind, a period which coincided with a maximum of the 23 cycle activity. The multiscale wavelength external fields were analyzed using spherical harmonic transform. The external field determined by inversion was then removed from each magnetic field component for each half orbit. To map the vector magnetic crustal anomalies, all LP magnetometer data collected at low altitudes in the three different lunar environments: (1) geomagnetic tail, (2) solar wind, and (3) geomagnetic sheath were processed using this new approach. The results obtained using these selection criteria allow us to get a global coverage of the lunar surface by the vector magnetic field at variable spacecraft low altitudes. To validate our mapping, we have developed and applied a method based on properties of potential fields functions. This method can be used to determine both horizontal north and east components using only vertical component. The validated lunar internal magnetic measurements obtained at variable spacecraft altitudes were then continued to a common altitude of 30 km using an inverse method. This mapping confirms firstly the nature of the crustal sources of lunar magnetic field and clearly shows that the strongest concentrations of anomalies are associated with high albedo and/or located antipodal to large young basins (Orientale, Serenitatis, Imbrium, and Crisium) of age about 3.9 Ga.     

银河旋臂、地核环流与地球大冰期

地球在其约４６亿年的生命史中，多次出现大冰期，关于其形成原因是地球科学家研究的热门课题。促使地球系统演化的力源主要来自哪一圈层？气体具有最大的激活能，但大气圈仅占地球总质量的１０－６，它不可能是主要圈层。固态的激活能最低，下地幔和地内核亦不大可能在地球系统演化中扮演主要角色。地球外核是液态，具有较高的激活能，它约占现代地球系统总质量的３０％，故可认为它是地球系统演化的主要活动圈层。作为旋转地球上的流体，外核环流存在着两种极端流型：一是“地转流型”，其速度场是二维场，垂直运动很弱（以下简称为Ｇ型）；二是“强对流型”，当Ｅｌｓｓａｓｅｒ数≥１时，流场的二维几乎完全被Ｌｏｒｅｎｚ力所破坏，对流充满整个地核（以下简称Ｃ型）。文章在事实分析的基础上提出了地球大冰期形成的如下假说：当地球背景磁场与银河旋臂磁场极性符号相同时，外磁场将激发地球外核环流转为Ｃ型，引起地壳和地幔强烈的垂直运动（强造山运动），致使大气热机效率亦大为提高，高纬地区强降温，这是大冰期形成的根本原因。这一假说的逆表述，即当地球背景磁场与银河旋臂磁场极性相反时，地核环流将转向Ｇ型，地壳表面将主要是“夷平作用”，致使大气热机效率亦降低，行星风系减弱，高纬?     

Formation of complex rotational structures in convective and isothermal magnetized zones

We study the development of a complex rotation law in the magnetized convective and isothermal zones of stars and planetary atmospheres through the decomposition of vector quantities in terms of orthogonal vector spherical harmonics. In the case of a solar-type extended convective zone, it is assumed that (a) the transformation of thermal into magnetic energy is favorable from the viewpoint of energy balance, (b) the state that is supported with minimum energy loss is realized, and (c) the condition of minimum entropy production consistent with the two previous requirements is satisfied. To find the rotation law of a zone, weak interaction between variations in the rotation and magnetic-field distributions is assumed. Two possible zones of generation of the solar magnetic field are considered. The first is located in the lower half of the solar convective zone and possesses a latitude dependence of the rotational velocity similar to that observed. The second zone is located just below the surface, and has a rotational velocity that decreases sharply with height and depends only weakly on latitude. We also study simple equilibrium structures, in particular, those describing the super-rotation of the medium in a convective or isothermal zone. Realization of such super-rotation in an isothermal zone is associated with the outflow of matter and fields toward upper layers.     

Geomagnetic Hazards to Conducting Networks

Geomagnetic disturbances can disrupt the operation of conductingnetworks, such as power systems, pipelines and communication cables. In power systems,geomagnetically induced currents (GIC) flow to ground through power transformers,disrupting their operation and causing transformer heating, increased reactive power demand,and generating harmonics that can cause relay misoperation. In extreme cases these effectscan lead to power blackouts such as occurred on the Hydro-Québec system during a geomagneticstorm in March 1989 leaving 6 million people without power for 9 hours.Geomagnetic disturbances are the result of eruptions on theSun that send high energy particles streaming out into space. When these particles reach theEarth they interact with the magnetic field, generating currents that flow down into the ionosphere.The most intense currents are associated with the aurora and occur in an east-west bandacross Canada. It is the magnetic field produced by these ionospheric currents that is seen on theground as a magnetic disturbance.Prevention of geomagnetic effects on power systems hasfocussed on blocking the flow of GIC in the system. However, such measures are expensive andmany utilities rely on forecasts of geomagnetic activity to help them operate during disturbances.The Canadian Geomagnetic Forecast Service, operated by Natural Resources Canada,has been in operation since 1974 and now provides long term and short term forecasts for threelatitude regions of Canada.Research is needed on all aspects of the problem; from newinformation about solar eruptions for improving forecasting services; to understanding systemresponse to disturbances. Research on geomagnetic disturbances is conducted by the CanadianGeomagnetic Forecasting Centre and a number of active groups at Canadian universities; whileresearch on geomagnetic effects is conducted by affected industries, often in collaborationwith the forecasting centre.     

Relationship between the contrast of coronal holes and parameters of the solar wind streams

It is shown that the contrast of coronal holes (CH) determines the speed of the solar wind streams to the same extent as their area does. We analyzed more than 400 images obtained in the λ284 Å channel. The time interval under examination covers about 1500 days in the declining phase of cycle 23 (from 2002 to 2006). We considered all coronal holes recorded during that interval in the absence of coronal mass ejections (CME). Comparison was also made with some other parameters of the solar wind (e.g., density, temperature, and magnetic field). A fairly high correlation (0.70–0.89) was obtained with the velocity, especially during the periods of moderate activity, which makes this method useful for everyday forecast. The ratio of CH brightness to the mean brightness of the disk in the λ284 Å channel is about 25%.     

Form of the latitude distribution of sunspot activity

The spatial (latitude) distribution of sunspots is studied, including its dependence on solar activity. It is shown that the latitude distributions of sunspots for a given year can be approximately described by the normal law, with its variance being a linear function of the current level of solar activity. Thus, an increase in activity is accompanied by an expansion of the zone of solar activity, in good agreement with earlier results. As the solar activity increases, the width of the zone of sunspot generation and the latitude maximum of the sunspot density grow somewhat more slowly than the number of sunspots, in agreement with observations. The results obtained can be used to reconstruct the spatial distributions of sunspots in the past, interpret the magnetic activity of stars, and address the requirements of the dynamo theory in the form of constraints imposed on models of cyclicity.     

Seasonal and solar cycle variations of night-time anomalous enhancements in total electron content

Seasonal and solar cycle variations of the various characteristics of night-time anomalous enhancements in total electron content (TEC) of the ionosphere are presented for a low latitude station, Hawaii by considering TEC data for a full solar cycle. All the characteristics of the TEC enhancements have seasonal and solar cycle dependence. TEC enhancement characteristics such as frequency of occurrence, amplitude and duration are positively correlated with solar activity. The possible source mechanisms for the observed enhancements are also discussed.