The ionospheric trough dynamics in the northern and southern hemispheres: the longitudinal and IMF effect

A study was made of the dynamics of the main ionospheric trough in the northern and southern hemispheres using data of ion density winter measurements on the Kosmos-900 satellite from 1977 to 1979. Significant longitudinal variations of the trough position have been found which prove to be different in the different hemispheres: in the northern hemisphere they have the shape of a double wave (period 180° longitude) with an amplitude of 4–6° of latitude by both day and night whereas, in the southern hemisphere, they exhibit a simple wave (period 360° longitude) with amplitude of about 6° in the night hours and 10–12° of latitude in the day hours.The analysis of the IMF influence on the trough position by day and night has shown both B_Z and B_Y to affect the shift of the ionospheric trough. It has been found that in the northern hemisphere the vertical and azimuthal IMF components act in opposite phase while in the southern hemisphere the effects of the two components are added. Analytic relationships between the trough shift magnitude and the values of B_Z and B_Y are discussed.     

On the global atmospheric electrical circuit

A model of global atmospheric electric circuit has been developed, which incorporates the pollution due to aerosol particles of anthropogenic and volcanic origins and the ionization caused by the coronal discharges due to intense electric field beneath thunderclouds in the atmospheric layers close to the earth's surface. Also the effects of solar activity and of Stratospheric Aerosol Particles (SAP) on the parameters of the circuit have been studied. The global distribution of Aerosol Particles (AP) of man-made origin has been assumed on the basis of world population density and that of volcanic origin on the basis of global distribution of volcanic activities. The thunderstorms are assumed to be the current generators of the global circuit. The latitudinal, longitudinal and height variations of atmospheric conductivity have been calculated from the known variations of ionization caused by cosmic rays, the radio-active emanations and intense electric fields beneath thunderclouds (over continents), along with the assumed variation of AP concentration.On increasing the AP concentration over the northern hemisphere by about 5 times that of the southern hemisphere, the ionospheric potential increases to about 6% and electric field increases in non-mountainous regions more than that in the high mountain regions. A large increase in SAP serves to increase the global resistance while both global current and ionospheric potential decrease. However, for low SAP concentration, the ionospheric potential increases. The SAP affect the electrical structure of the stratosphere without much influencing the troposphere except in the volcanically active regions, where conductivity is low due to high AP concentration. The major influence on the global atmospheric electric circuit occurs in response to solar activity. In the absence of local effects, the calculated variation of ionospheric potential is 14%. However, in real atmosphere (where both local and global processes act simultaneously), the ionospheric potential is found to vary by only about 3%. This has little effect on the ground electrical properties where more than 30% of the variations have been found to be caused by the local effect.     

Modelling studies of the conjugate-hemisphere differences in ionospheric ionization at equatorial anomaly latitudes

The relative importance of the equatorial plasma fountain (caused by vertical E x B drift at the equator) and neutral winds in leading to the ionospheric variations at equatorial-anomaly latitudes, with particular emphasis on conjugate-hemisphere differences, is investigated using a plasmasphere model. Values of ionospherec electron content (IEC) and peak electron density (Nmax) computed at conjugate points in the magnetic latitude range 10–30° at longitude 158°W reproduce the observed seasonal, solar activity, and latitudinal variations of IEC and Nmax, including the conjugate-hemisphere differences. The model results show that the plasma fountain, in the absence of neutral winds, produces almost identical effects at conjugate points in all seasons; neutral winds cause conjugate-hemisphere differences by modulating the fountain and moving the ionospheres at the conjugate hemispheres to different altitudes.At equinox., the neutral winds, mainly the zonal wind, modulate the fountain to supply more ionization to the northern hemisphere during evening and night-time hours and, at the same time, cause smaller chemical loss in the southern hemisphere by raising the ionosphere. The gain of ionization through the reduction in chemical loss is greater than that supplied by the fountain and causes stronger premidnight enhancements. in IEC and Nmax (with delayed peaks) in the southern hemisphere at all latitudes (10–30°). The same mechanism, but with the hemispheres of more flux and less chemical loss interchanged, causes stronger daytime IEC in the northern hemisphere at all latitudes. At solstice, the neutral winds, mainly the meridional wind, modulate the fountain differently at different altitudes and latitudes with a general interhemispheric flow from the summer to the winter hemisphere at altitudes above the F-region peaks. The interhemispheric flow causes stronger premidnight enhancements in IEC and Nmax and stronger daytime Nmax in the winter hemisphere, especially at latitudes equatorward of the anomaly crest. The altitude and latitude distributions of the daytime plasma flows combined with the longer daytime period can cause stronger daytime IEC in the summer hemisphere at all latitudes.     

Diurnal and seasonal variability of the southern-hemisphere main ionospheric trough from differential-phase measurements

A differential-phase technique utilizing the radio transmissions of NNSS satellites was used to make measurements of the latitudinal variations of ionospheric vertical total electron content (TEC) in the southern mid-latitude trough region from the location of Macquarie Island (a cis-auroral site; geographic coordinates 54.5°S, 154.95°E, geomagnetic coordinates 64.5 S, 177.67 E, L = 5.38) for a period of 14 months during 1987–1989. The differential-phase method provided a means of observing a relatively large expanse of ionosphere whilst centered on the cis-auroral region which was well suited for trough studies. By monitoring the two transmitted radio signals at 150 and 400 MHz from the Navy Navigation Satellite System (NNSS) polar orbiting satellites it was possible to deduce the latitudinal variation of ionospheric vertical TEC for the duration of the satellite pass. The absolute TEC was derived from Faraday-rotation and ionosonde data obtained during the same period.The main findings of this work have been the high incidence of daytime troughs for all seasons and the relative low incidence of night-time troughs. Both summer and vernal equinox seasons display a greater occurrence frequency of daytime troughs than the winter and autumnal equinox seasons. Winter-time troughs at any time are less frequent than for any other season. Comparisons with the northern-hemisphere trough display a marked difference in occurrence frequency and distribution of troughs. An attempt to explain some of these features in the light of the high-latitude convection theory is offered. Case studies are given for all seasons to highlight these findings.     

Mean airstreams of Australia

Streamline analyses of mean monthly resultant surface winds over Australia are presented. Mean confluences represent either cyclone trajectories, or modal fronts. These analyses suggest that Australia's annual airstream climate is of two regimes: that of September to March inclusive, and April to August inclusive. The winter half-year is exemplified by a continental airstream source in southern Australia which diverges over virtually the entire continent. It continues into September and October, although dominating only the southern third to half of Australia, and is absent from November to March. During the summer half-year a new pattern emerges, with three maritime air stream sources represented over the continent: first, air from the Southern Ocean penetrates the south coast reaching its furthest northward extension from December to March inclusive; a second source originating over the Pacific Ocean dominates eastern and northern Australia; and a monsoon source originating over the Indian Ocean which flows overland affecting northern Western Australia. Two modal confluences are noted, one over northwestern Australia from November-February separating monsoon flow from that emanating from the east, and another extending from the west central coast east-southeastward to the southeast coast from November-March separating Southern Ocean air from that originating over the Pacific Ocean.     

Auroral riometer absorptions and the F-region disturbances observed over a wide range of latitudes

Standard riometer data from a southern auroral station were compared with ionograms obtained at five stations positioned from sub-auroral to equatorial latitudes. The rapid onset in riometer absorption, during intense substorm activities in an equinoctial period, was associated with a sequential propagation of ionospheric disturbances deduced from the F-region parameters h′F and range spread-F. The time shift between absorption maxima and extrapolated commencement times of the disturbances was consistent with the presence of large-scale travelling ionospheric disturbances (TIDs), propagating equatorwards with velocities lying typically in the range 600–900 m s⁻¹, and with a median velocity of 720 m s⁻¹. It is suggested that the onset of TIDs is associated with high-energy particle precipitation, manifested by the occurrence of auroral absorption events. Similarity of absorption increases at the southern and northern conjugate points, found from a previous riometer study, would indicate that large-scale TIDs are simultaneously generated in both hemispheres.     

On abnormal quiet day Sq(Z) ranges in the Indian region

Solar quiet day variations of the vertical geomagnetic component Sq(Z) have been studied. These show abnormal variations from day to day. The study for the period 1961 to 1976 indicates that, for quite a number of days, the Sq(Z) phase reverses completely. It is concluded that changes in phase of Sq(Z) could be explained by the movement of the Sq current system and the penetration of the Sq southern current system into the northern hemisphere.     

The polarisation of whistlers received on the ground near L = 4

The observed polarisation of the horizontal magnetic components of whistler mode signals received at Halley, Antarctica (L≈ 4.3), is in many cases that expected from a simple model of the transionospheric and sub-ionospheric propagation in the southern hemisphere; i.e. right-hand elliptical (field vectors rotate clockwise, looking towards the source) for ionospheric exit points close to the receiver, tending towards linear for more distant exit points. This suggests it may be possible to use the observed polarisation to estimate the propagation distance. However, in other cases, in certain frequency ranges, left-hand elliptically polarised signals have been observed. More realistic models do predict polarisation reversals at certain frequencies and exit point to receiver distances, but not over such a wide frequency range as has sometimes been observed. Also, in some cases, signals with nearly right-hand circular polarisation have been observed for exit points at large distances where linear polarisation would be expected.     

Annual variations in the electron content and height of the F layer in the northern and southern hemispheres,related to neutral composition

Total electron content (TEC) data is presented for similar sites at ±35° latitude, and conjugate sites at ±20°, for several years near solar maximum. Comparison with the MSIS atmospheric model shows that the large seasonal anomaly at 35°N (an increase of 80% in TEC from October to April) is fully explained by changes in neutral composition. The small seasonal anomaly at 35°S also agrees with the MSIS model. Composition changes fail to account for the generally higher TEC in the northern hemisphere; this suggests the presence of an overall south-to-north atmospheric wind. Eastern declinations also contribute to enhanced TEC in the northern hemisphere, in the Pacific zone. The MSIS model predicts a semiannual variation of about ±25% in TEC at all sites, while observed changes are only about ±8%; thus we require some enhanced loss process near the equinoxes, particularly in September and October.Peak height calculations assuming a constant pressure level give a large semiannual variation in the F2 region: this is replaced by an annual variation when h_m F2 is calculated from diffusion theory. Heights calculated from the MSIS model are similar to observed values at ±35° latitude on summer days. A decrease of about 20km in observed heights on winter days is attributed to a poleward neutral wind; this wind also reduces the observed TEC. At night the height changes correspond to an equatorial wind, which is largest in summer and equinox. Observed day time TEC is greater at 20°N than at 20°S at all times of year, suggesting a northward transequatorial wind which is strongest near January and gives increased TEC and decreased peak height at 20°N.     

A comparison of northern and southern hemisphere TEC storm behaviour

Changes in total electron content during magnetic storms are compared at stations with similar geographic and geomagnetic latitudes and eastward declinations in the northern and southern hemispheres.Mean patterns are obtained from 58 storms at ±35° and 28 storms at ± 20° latitude. The positive storm phase is generally larger (and earlier) in the southern hemisphere, while negative storm effects are larger in the north. These changes reduce the normal asymmetry in TEC between the two hemispheres. Composition changes calculated from the MSIS86 atmospheric model agree well with the maximum decreases in TEC in both seasons (when changes in the F-layer height are ignored). Recovery occurs with a time constant of about 35 h; this is 50% longer than in the MSIS86 model. There is a marked diurnal variation at 35°S, with a rapid overnight decay and enhanced values of TEC in the afternoon. This pattern is inverted (and weaker) at 35°N, where night-time decay is consistently slower than on undisturbed nights. These results require a diurnal change in composition of opposite sign in the two hemispheres, or enhanced westward winds at night changing to eastward near sunrise. There is some evidence for both these mechanisms. Following a night-time sudden commencement there is a large annual effect with daytime TEC increasing for storms near the June solstice and decreasing near December. Storms occurring between November and April tend to give large, irregular increases in TEC for several days, particularly at low latitudes. In summer and winter at both stations, the mean size of the negative phase does not increase for storms with K_p> 6. The size of the positive phase is proportional to the size of the change in a_p in winter, while in summer a positive phase is seen only for the larger storms.     

Grossly-distorted isoionic contours associated with spread-F occurrence at mid-latitudes

A directional ionosonde has been used to investigate a mid-latitude travelling ionospheric disturbance which passed over Brisbane, Australia, on the night of 31 July/1 August 1981. The analyses have revealed what appears to be a large-scale frontal height rise (about 300 km wide) travelling in a north-west direction with a speed of 93 ms⁻¹. Smaller-scale frontal structures with wavelengths of some tens of kilometres appeared near the crest of this large-scale upwelling and have the same frontal orientations. These are responsible for the spread-F seen on ionograms during the passage of the disturbance. Also, associated with the disturbance was a tongue of ionization which extended down from the crest of the upwelling more than 100 km. It appeared to be drifting with the same speed and in the same direction as the upwelling. Near the lowest extremity of the tongue the ionization density was at least 35% greater than elsewhere in the ionosphere. The lowest extremity of the tongue was located 240 km from the recording station as the large-scale frontal structure passed overhead. Statistical analyses using 19 tongue events in 1979 have shown that ionospheric height rises seem to be generally associated with these events not only at the recording station, but also in the conjugate hemisphere. Certain characteristics of the mid-latitude disturbance which have been investigated in this paper are compared with the characteristics of similar disturbances in equatorial regions.     

High-latitude tidal behavior in the mesosphere and lower thermosphere

The high-latitude structure of the mean winds and tides is described in this paper using climatologies prepared from radar data during the Atmospheric Tides Middle Atmosphere Program. The monthly evolution of the amplitude and phase of the tides is discussed. Comparison between the southern and northern hemispheres indicate that the diurnal tide is stronger in the southern hemisphere and that the antisymmetric diurnal tidal modes are dominant. The semidiurnal tide is larger than the diurnal tide. The vertical wavelength structure is significantly different between the southern and northern hemisphere. Comparisons with recent tidal models show several discrepancies.     

Equatorwards limits of the southern scintillation oval

Radio signals in the VHF range were recorded and compared with ionograms over a wide range of southern latitudes during a few equinoctial months for which a large variation in the magnetic disturbance level was observed. It is evident that the equatorwards edge of the auroral scintillation oval extends well into mid-latitudes for high values of magnetic K-index. The range-spreading type of spread-F and scintillation-producing irregularities show a high degree of spatial coincidence from the polar cap to mid-latitudes. It is suggested that the inhomogeneities responsible for both ionospheric phenomena are associated with the equatorwards propagation of travelling ionospheric disturbances (T1Ds) generated in the auroral zone.     

Ionospheric and atmospheric disturbances around Japan caused by the eruption of Mount Pinatubo on 15 June 1991

The disturbances observed by the Japanese ionospheric observation network following the explosions of Mount Pinatubo on 15 June 1991, are presented. Remarkable ionospheric fluctuations with periods of about 20 min appeared in the records of HF Doppler and total electron content (TEC) data. Traveling wave fronts of ionospheric disturbances scaled from these data give a northward horizontal velocity of 290 m/s. The surface pressure fluctuations due to the passage of atmospheric waves were confirmed by the microbarograph chain data in Japan. There existed three kinds of northward traveling pressure fluctuations; short-period (2–5 min) fluctuations with a horizontal velocity of 290 m/s, long-period (8–10 min) fluctuations with 300 m/s, and 17-min fluctuations with 281 m/s. It is concluded that the ionospheric and surface pressure waves were caused by the eruption of Mount Pinatubo.     

Comparison of equatorial electrojet characteristics at Huancayo and Eusébio (Fortaleza) in the South American region

The H, D and Z average daily variations for five international quiet days are compared for Huancayo (12°S, 75°W, dip +1.9°) and Eusébio near Fortaleza (4°S, 39°W, dip −3.5°) in the South American region, for the 12 successive months, October 1978-September 1979. The H range shows that the electrojet is weaker in the Fortaleza region. Also, the electrojet center has latitudinal excursions from month to month at both the locations, but not in a similar way. The D variations indicate excursions of northern hemisphereS_q current systems into the southern hemisphere (or vice versa) but in a dissimilar way at Eusébio and Huancayo. Also, significant ΔD magnitudes are noticed even at midday, indicating possibility of meridional currents. It seems that the overhead S_q current pattern changes in form, while moving over from the Fortaleza region to the Huancayo region.     

Geomagnetic field variation and the equivalent current system generated by an ionospheric dynamo at the solstice

The geomagnetic field variation and equivalent current system produced by an asymmetrical ionospheric dynamo action under a solstitial condition are simulated and compared with the observational results. Results of our simulation reproduce well most of the observational features of the solstitial Sq system. For example, the latitude of the current vortex center is higher in summer than in winter and the local time of the center in the summer hemisphere is located earlier than that in the winter hemisphere. In the morning and afternoon sector the current vortex in the summer hemisphere invades the winter hemisphere. The first feature is attributed to the ionospheric currents, but the second and third features are due to the field-aligned currents generated by the asymmetry of the ionospheric dynamo.     

Ionospheric plasma convection in the southern hemisphere

The first ionospheric plasma convection maps ordered by the y- and z-components of the IMF using only data from the southern hemisphere are presented. These patterns are determined from line-of-sight velocity measurements of the Polar Anglo-American Conjugate Experiment (PACE) located at Halley, Antarctica, with the majority of the observations coming from 65°–75° magnetic latitude. For IMF Bz positive and negative conditions, the observed plasma motions are consistent with a standard two cell pattern. For the periods from dusk through midnight to dawn, flow speeds are at least twice as large for Bz negative component compared with Bz positive. The observations about noon are significantly different from each other. For Bz positive, little ordered plasma motion is observed. For Bz negative, there are large anti-sunward flows the orientation of which is ordered by IMF By. These By orientated flows are consistent with theoretical predictions, and are anti-symmetric to those reported from the northern hemisphere. The two most significant differences from previous observations are that the convection reversal in the late morning sector for By negative conditions occurs at about a 4° lower latitude than the Heppner and Maynard (1987) model. This may be due to a seasonal bias in the PACE dataset. Also, the separatrix between eastward and westward flow near midnight has a very different shape dependent upon the orientation of IMF By. For positive By conditions, the separatrix is observed at progressively lower latitudes at later local times, but for By negative conditions, the separatrix appears at increasingly higher latitudes at later times.     

Participation and Representation in ATSIC Elections: A 10 Year Perspective

This paper examines participation and representation in ATSIC elections over the 10 year period since 1990. It attempts to identify patterns of participation and representation that seem to be emerging and what these might suggest about ATSIC's operation. By examining numbers of nominees compared to positions available, the paper suggests that ATSIC elected office has been fairly keenly and consistently sought and competed for by Indigenous people, though there may have been some slight initial reticence in the 1990 elections. By examining voter numbers and voter turnout, the paper suggests that voter participation nation-wide rose slightly from 1990 to 1996 and then largely stabilised in 1999. It also suggests that there have been significant variations from this national pattern at State and Territory levels and it explores some reasons for this. The paper also examines voter numbers and voter turnout at the ATSIC regional level since 1993 and finds that there has been much higher voter turnout in the sparsely settled regions of northern Australia and much lower voter turnout in the southern and urban areas. This is explained in terms of ATSIC program and expenditure priorities and in terms of polling place access. The final two sections of the paper examine the representation of women and Torres Strait Islanders among ATSIC elected representatives. Both are seen as significant issues which should be of some ongoing concern within ATSIC, alongside the issue of the southern/northern difference in voter participation.     

Simulations of the behaviour of the polar thermosphere and ionosphere for northward IMF

The dynamics and structure of the polar thermosphere and ionosphere within the polar regions are strongly influenced by the magnetospheric electric field. The convection of ionospheric plasma imposed by this electric field generates a large-scale thermospheric circulation which tends to follow the pattern of the ionospheric circulation itself. The magnetospheric electric field pattern is strongly influenced by the magnitude and direction of the interplanetary magnetic field (IMF), and by the dynamic pressure of the solar wind. Previous numerical simulations of the thermospheric response to magnetospheric activity have used available models of auroral precipitation and magnetospheric electric fields appropriate for a southward-directed IMF. In this study, the UCL/Sheffield coupled thermosphere/ionosphere model has been used, including convection electric field models for a northward IMF configuration. During periods of persistent strong northward IMF B_z, regions of sunward thermospheric winds (up to 200 m s⁻¹) may occur deep within the polar cap, reversing the generally anti-sunward polar cap winds driven by low-latitude solar EUV heating and enhanced by geomagnetic forcing under all conditions of southward IMF B_z. The development of sunward polar cap winds requires persistent northward IMF and enhanced solar wind dynamic pressure for at least 2–4 h, and the magnitude of the northward IMF component should exceed approximately 5 nT. Sunward winds will occur preferentially on the dawn (dusk) side of the polar cap for IMF B_y negative (positive) in the northern hemisphere (reverse in the southern hemisphere). The magnitude of sunward polar cap winds will be significantly modulated by UT and season, reflecting E-and F-region plasma densities. For example, in northern mid-winter, sunward polar cap winds will tend to be a factor of two stronger around 1800 UT, when the geomagnetic polar cusp is sunlit, then at 0600 UT, when the entire polar cap is in darkness.     

The role of electric field and neutral wind direction in the formation of sporadic E-layers

The effect of an electric field and a homogeneous neutral wind on the vertical ion motion in the ionospheric E-region is investigated. An electric field pointing, in the northern hemisphere, in the quadrant between geomagnetic north and west is found to he capable of driving plasma towards a certain height from both above and below. A homogeneous neutral wind blowing in a direction between east and north has a similar effect. Unlike in the wind shear model, the resulting plasma sheet may be created within a quite limited height interval only. It seems possible that the midnight occurrence maximum of mid-latitude type E_s-layers, observed at high latitudes, is caused by electric fields in the Harang discontinuity region. It is also suggested that the flat type E_s-layers often observed before a substorm onset are caused by electric fields. The wind shear theory is investigated using a screw-like neutral wind profile. The effects of right- and left-handed wind screws are compared and rules are derived which define the conditions leading to convergent and divergent nulls in the vertical ion velocity. In the northern hemisphere, a right-handed screw is found to be more effective than a left-handed one with equal pitch in compressing plasma into thin sheets.