Multiple-frequency studies of the high-latitude summer mesosphere : implications for scattering processes

The characteristics of polar mesosphere summer echoes (PMSE) are studied at 53.5 and 224 MHz. Observations at 2.78 MHz, simultaneous with the ones at the other two frequencies, were carefully compared for indications of PMSE, but no obvious relation was found. Relationships between relative scattering cross-section, spectral width and vertical velocity are studied for the 224 MHz radar, and observations at 53.5 MHz are compared with those at 224 MHz. Results of aspect sensitivity measurements at 53.5 MHz are presented. The implications of these characteristics for several possible scattering mechanisms are discussed. We rule out incoherent scatter and chemically induced fluctuations from the evidence that we have. In view of the extremely low temperatures near the high-latitude mesopause in summer, we discuss several scenarios involving heavy cluster ions and charged aerosol particles.     

The effect of atmospheric screening on the visible border of noctilucent clouds

The noctiiucent cloud display of 10/11th July 1979 was observed from two sites in Scotland: Clinterty near Aberdeen, using a low light level TV camera, and Milngavie near Glasgow, using a photographic camera. Coincident observations of the display were made from 23.55 UT until 00.50 UT.By projecting the image of the noctilucent cloud structure as seen by one camera into the field of view of the other camera, the height of the clouds was found to be 82 ± 1 km. Using this result, the effect of atmospheric screening on the visible border of the noctilucent clouds was determined. Taking account of the refraction on the solar grazing rays illuminating the clouds at the visible border and the finite angular diameter of the sun's disc, the altitude of the screening layer was determined to be 7 ± 1 km. Thus, on this occasion, the screening effect of the atmosphere was confined to the troposphere and was probably caused by atmospheric haze and/or tropospheric cloud.This result contrasts markedly with the high values of screening height, ~ 30 km, deduced from measurements made earlier this century, also using the visible boundary of the clouds. The analysis presented herein indicates that these large values were probably in error, due to the poor dynamic range of the photographic films employed.     

Intense turbulence in the polar mesosphere : rocket and radar measurements

Simultaneous observations of polar mesospheric summer echoes (PMSE) have been made with two different frequency radars during the launch of a sounding rocket designed to measure the fluctuations in the electron density in the same height range. The cross-section for radar backscatter deduced from the rocket probe data under the assumption of isotropic turbulence is in reasonable agreement with the measured signals at both 53.5 MHz with the mobile SOUSY radar and 224 MHz with the EISCAT VHF radar, which correspond to backscatter wavelengths of about 3 and 0.75 m, respectively. Some controversy exists over the relative roles of turbulent scatter vs specular reflections in PMSE. A number of characteristics of the data obtained in this experiment are consistent with nearly isotropic, intense meter-scale turbulence on this particular day. Since equally compelling arguments for the importance of an anisotropic-type mechanism have been presented by other experimenters studying PMSE, we conclude that both isotropic and anisotropic mechanisms must operate. We have found the inner scale for the electron fluctuation spectrum, which corresponds to the diffusive subrange for that fluid, and have compared it to the inner scale for the neutral gas. The latter was found from the Kolmogorov microscale, which in turn depends on the energy dissipation rate in the gas. We found the dissipation rate from the spectral width of the 53.5 MHz backscatter signal and from the rocket electron density fluctuation data. The diffusive subrange was found to occur at a wavelength a factor of about 10 times smaller than the viscous subrange. This corresponds to a Schmidt number of about 100. High Schmidt numbers have been reported in recent measurements of the diffusion coefficient of the electrons in this height range made with the EISCAT incoherent scatter radar. About 15 min after the rocket flight an extremely high radar reflectivity was found with the SOUSY system. We have been able to reproduce this high level theoretically by scaling the rocket data with an increase in the neutral turbulence energy dissipation rate by a factor of 14 as deduced from the SOUSY spectral width, an increase in the electron density which is consistent with riometer data, and a 33% decrease in the electron density gradient scale length which is hypothesized. We also estimate the radar reflectivity at 933 MHz and conclude that signals in excess of thermal scatter levels would have occurred at the peak of the event studied, provided that the electron fluctuation spectrum decreases as k⁻⁷ in the viscous subrange. If the spectrum has an exponential form, however, a turbulent source cannot explain the enhanced 933 MHz echoes reported by EISCAT.     

Further effects of charged aerosols on summer mesospheric radar scatter

In an earlier paper, we showed that charged aerosols play a crucial role in enhancing radar echoes from the summer polar mesosphere through reduced diffusion turbulent scatter and dressed aerosol scatter (Cho et al., 1992a). Here, we explore the effects of charged aerosols on radar scatter through ‘fossil’ turbulence and electron density depletion layers. We find that the former can produce radar scatter even after the decay of neutral gas turbulence, while the latter, which are probably produced by the scavenging of free electrons by ice particles, are a candidate for causing partial reflection or Fresnel scatter. Furthermore, we examine the mutual aerosol interaction restriction on dressed aerosol scatter more closely. We find that a high ambient electron density and low aerosol number density are needed for effective dressed aerosol scatter to occur. We then show that very small (less than 1 nm radii), negatively charged aerosols enhance electron diffusivity, and thus inhibit radar scatter. Also, ice aerosol sedimentation, in the light of the reduced diffusion theory, leads us to conclude that the statistical peak in Polar Mesospheric Summer Echoes (PMSE) power should be located between the mean mesopause and the average noctilucent cloud (NLC) height, which agrees with observations. Finally, we invoke time lags in the ice particle formation cycle to account for the observed non-correlation between PMSE and NLC occurrence.     

Measurements of noctilucent cloud heights: a bench mark for changes in the mesosphere

Recent studies of noctilucent clouds indicate a secular increase in their frequency of occurrence which may be associated with changes either in the water vapour concentration or in the mean temperature of the mesopause. Noctilucent clouds are expected to be seen very close to the level where the relative humidity is 100% and changes in temperature of the mesosphere or in its water vapour content might be expected to alter the height at which the clouds occur. Comparison of our height measurements with those obtained over the past 100 yr shows that the suggested changes since 1885 in temperature (a decrease of approximately 7°C) and water vapour mixing ratio (an increase of approximately 1.7 ppmv) have not been sufficient to affect the height of the clouds by an observable amount. Future height measurements of noctilucent clouds may provide a practical indicator of changes taking place in the mesosphere which could be associated with global-scale alterations of the lower atmosphere.     

The analysis of hydroxyl rotational temperatures to characterize moving thermal structures near the mesopause

Hydroxyl (OH) rotational temperatures near 85 km altitude have been monitored at Calgary, Alberta, Canada (51°N, 114°W) since 1981 with the objective of determining velocities, wavelengths and periods associated with moving temperature structures. A technique is described whereby the velocity of moving patterns in two dimensional data sets can be accurately determined and used as a parameter for a global smoothing algorithm. Velocities of the structures in the meridional direction were found to be directed poleward. Corresponding Doppler bulk wind velocities measured near the 95 km height region were directed equatorward indicating the presence of filtering of internal gravity waves by the background wind. Two coherent wave structures were often observed simultaneously during a night. The smaller of the two structures had true wavelengths less than 15–30 km and may be related to billow clouds often reported in noctilucent cloud observations. The second wave has a period on the order of an hour and meridional wavelengths ranging from 100 to 2000 km.     

Low latitude auroras: the storm of 25 September 1909

Visual auroras at low latitudes are rare, documented for only five occasions since 1859. They are important from a theoretical point of view in terms of the lowest latitude at which particle precipitation can been observed. One of the great magnetic storms of the past 150 yr occurred on 25 September 1909, during the prolonged solar activity minimum around the beginning of the present century. A report of an auroral sighting at Singapore, not far from the magnetic equator, the lowest latitude ever reported for a visual aurora. has focussed attention on this event. This paper compiles and discusses the solar, magnetic, auroral, and telegraphic disturbance data related to the event. The data show that the lowest credible magnetic latitude for this event was between 30° and 36°. I conclude that the report of a visual auroral observation at Singapore, based on a single Australian newspaper item, was almost certainly not auroral at all, but rather resulted from cable disturbances, known to be associated with auroras, and confused with the aurora itself. Furthermore, consideration of the height at which particle precipitation would be observed leads to an estimate of a threshold magnetic latitude for a visual auroral event of the order of 15°, greater than that of 'Singapore. This result removes the necessity of theories of major storms to account for such a low latitude sighting.     

Scintillation at high latitudes during winter magnetic storms

Scintillation observations are described which were made at Kiruna in northern Sweden during three magnetic storm periods in the winter of 1984–1985. The results were obtained using transmissions from the multisatellite NNSS system, so that it has been possible to chart the development of scintillation activity over some 20° of geomagnetic latitude as a function of time for several days throughout each storm. A region of strong scintillation at the highest latitudes near magnetic noon is a common feature on all but the quietest days. This feature, probably associated with soft particle precipitation into the cusp, shows an abrupt boundary which moves equatorwards as the disturbance develops. In the magnetic midnight sector two latitudinally separate zones of scintillation are found, patchy at high latitudes although more sustained in the auroral zone. An absence of auroral scintillations around midnight UT can be followed by prolonged intense scintillation activity at auroral latitudes during the early morning hours on some disturbed days.     

Storm after-effects observed at Ushuaia and Kerguelen

D-region disturbances have been detected at mid-latitudes after intense magnetic storms by means of a wide range of radiowave signals. Two different mechanisms have been suggested to account for these storm ‘after-effects’: one implies precipitation of energetic electrons from the radiation belt; the other, transport of neutral constituents from the auroral zones.This paper presents observations of abnormal enhancements of ionospheric absorption arising after two major magnetic storms occurring in March and April 1976. The measurements were made at Ushuaia (54.8°S, L = 1.7) and at Kerguelen (49.4°S, L = 3.7). The former were obtained by means of the pulse reflection method (A1) at MF and the latter by the riometer technique. It is shown that electron precipitation can explain the effects observed at Kerguelen but not those at Ushuaia which also depart significantly from the ‘winter anomaly’ trend observed at that site. The abnormal ionization at Ushuaia is attributed to transport from the southern auroral zone.     

Middle atmosphere and lower thermosphere processes at high latitudes studied with the EISCAT radars

The middle and upper atmosphere and the ionosphere at high latitudes are studied with the EISCAT incoherent scatter radars in northern Scandinavia. We describe here the investigations of the lower thermosphere and the E-region, and the mesosphere and the D-region. In the auroral zone both these altitude regions are influenced by magnetospheric processes, such as charged particle precipitation and electric fields, which are measured with the incoherent scatter technique. Electron density, neutral density, temperature and composition are determined from the EISCAT data. By measuring the ion drifts, electric fields, mean winds, tides and gravity waves are deduced. Sporadic E-layers and their relation to gravity waves, electric fields and sudden sodium layers are also investigated with EISCAT. In the mesosphere coherent scatter occurs from unique ionization irregularities. This scatter causes the polar mesosphere summer echoes (PMSE), which are examined in detail with the EISCAT radars. We describe the dynamics of the PMSE, as well as the combination with aeronomical processes, which could give rise to the irregularities. We finally outline the future direction which is to construct the EISCAT Svalbard Radar for studying the ionosphere and the upper, middle and lower atmosphere in the polar cap region.     

Energetic electron precipitation at the South Atlantic Magnetic Anomaly: a review

This paper reviews the status of knowledge concerning energetic electron precipitation at the South Atlantic Magnetic Anomaly (SAMA). The main purpose is to place recent results in the context of the long-standing problems about energetic electron precipitation at the SAMA region. A synopsis of results achieved in the last two decades, in relation to the various physical mechanisms responsible for precipitating energetic electrons, are also presented. The major uncertainties in the understanding of the energetic electron precipitation at the SAMA include: (1) temporal and spatial precipitation changes from magnetically quiet to disturbed periods; (2) the role of wave-induced precipitation processes.     

Data comparison of EISCAT and the energetic particle instrument on GEOS 2

Flux variations of high energy (E > 16 keV) electrons, measured by the energetic particle spectrometer onboard the geosynchronous satellite GEOS 2, have been compared to simultaneously observed electron density structures in the lower ionosphere, measured with the incoherent scatter facility EISCAT. The very localized E-region electron density enhancements caused by the precipitation allow a preliminary estimate of the location of the footpoint of the magnetic field line through GEOS 2. Various other results of the intercomparison are discussed.     

Characteristics of polar mesosphere summer echoes (PMSE) observed with the EISCAT 224 MHz radar and possible explanations of their origin

We describe experiments carried out with the EISCAT VHF radar during the MAC/SINE campaign. These experiments included observations of the polar mesosphere summer echoes (PMSE), which were studied with a high spectral resolution program. The fine structure of the spectra imply that very thin and non-random transient structures of reflectivity occur frequently in the mesopause region. We find no clear relation between the echo power and the coherence time which could support the hypothesis of scatter from turbulence or partial reflection. In addition, the estimates of radar reflectivity let us discard incoherent scatter and pure turbulence scatter as the cause of the PMSE. We also discuss the relation of the PMSE and cluster ions, electric fields, charge accumulation and atmospheric gravity waves.     

Plasma convection and auroral precipitation processes associated with the main ionospheric trough at high latitudes

Intervals of F-region electron density depletions associated with the main (mid-latitude) ionospheric trough have been studied using latitude scanning experiments with the EISCAT UHF radar. From 450 h of measurements over a one year period at solar minimum (April 1986–April 1987) the local time of appearance of the trough at a given latitude is observed to vary by up to about 8 h. No seasonal dependence of location is apparent, but troughs are absent in the data from summertime experiments. A weak dependence of trough location on K_p is found, and an empirical model predicting the latitude of the trough is proposed. The model is shown to be more appropriate than other available quantitative models for the latitudes covered by EISCAT. Detailed studies of four individual days show no relationship between local magnetic activity and time of observation of the trough. On all four of these days, however, the edge of the auroral oval, evidenced by enhanced electron densities in the E-region, is found to be approximately co-located with, or up to 1° poleward of, the F-region density minimum. Simultaneous ion drift velocity measurements show that the main trough is a region of strong (> several hundred metres per second) westward flow, with its boundary located approximately 1°–2° equatorward of the density minimum. Within the accuracy of the observations this relationship between the convection boundary, the trough minimum and the precipitation boundary is independent of local time and latitude. The relevance of these results is discussed in relation to theoretical models of the F-reregion at high latitudes.     

Neutral atom precipitation—a review

The production of energetic neutral atoms by charge exchange of ring current ions with neutral hydrogen in the geocorona was predicted many years ago, and there are now a number of measurements of the effect of the impact of these energetic atoms on the thermosphere. Theoretical models of the process have been developed. The latitude variation of the precipitating flux depends very much on the pitch angle distribution of the ions in the ring current, and on the L shell on which they are located.The production of a belt of trapped particles at low altitude near the magnetic equator may occur when neutral atoms re-ionize and become trapped on impacting the thermosphere, and this belt has been found in particle measurements near the equator and is enhanced during periods of magnetic activity.A region of enhanced optical emission due to precipitating neutrals is found in the thermosphere near the magnetic equator in both disturbed and quiet times, implying a low L value and/or pancake pitch angle distribution for the ring current particles that give rise to these neutrals. An isotropic pitch angle distribution is present in parts of the ring current at time during magnetic storms. This gives rise to neutral atom precipitation at all latitudes, and particularly of particles near 90° pitch angle in the region of SAR arc occurrence, about 10° in dip latitude equatorward of the isotropic region.The rate of energy deposition and the rate of production of ionization in the thermosphere depend on the ion species present in the ring current; their energy spectra, and on the distributions of the ions with L value and pitch angle. The rate of energy deposition may at times reach 10⁻² to 10⁻¹ mWm⁻², sufficient for significant heating and wind generation. The rate of production of ionization in the thermosphere at night may be much greater than that of other low latitude night-time ionization sources.     

Perspectives of present and future space weather forecasts

Two main targets of space weather forecasts are to, predict solar energetic particles (SEPs) produced by flares and coronal mass ejections CMEs), and the energetic particles or hot plasma injected into the inner magnetosphere during magnetic storms and substorms. For the purpose of constructing models to predict these particle popuplations, we critically review the problems in flares and CMEs, and the problems in magnetic and substorms For flares and CMEs, we point out the importance of distinguishing the effects of flares from the effects of CMEs, because it seems that many physical processes operate commonlyto both phenomena and produce similar effects. Recent studies on SEP events have shown that advanced measurements of SEPs can distinguish between these two acceleration sources. We propose a possible relationship between flare and CMEs based on an idea of dual magnetic field structures of different characteristic scales. It is expected that further progress can be accomplished by vector magnetographs, sold X-ray telescopes, and advanced measurements of solar wind composition as well as SEP composition. Far magnetic storms and substorms, it is found that analysis by the linear filtering technique can give results which are very consistent with theoretical understanding. Therefore, it is strongly recognized that the next step should be fully theoretical studies, or simulations.     

Energetic particles in the environment of the Earth's magnetosphere

This review summarizes the work in the field of magnetospheric energetic particles during the years 1987–1989. Out of a wealth of contributions it concentrates on a few topics. First it follows the path of ions extracted out of the polar ionosphere and their acceleration parallel and perpendicular to the magnetic field, as well as their subsequent transport into the equatorial magnetosphere and tail region. Then it focuses on acceleration of ions in the magnetotail and the related characteristics in the boundary layers including consequences for current substorm modeling. In the ring current region, the AMPTE and VIKING missions have made possible detailed studies of charge state and pitch-angle distributions as well as their variations during magnetospheric storms and substorms, from which conclusions on the transport and loss processes can be drawn. Recently, observations of energetic particles from orbiting nuclear reactors in the magnetosphere, which can be used as tracers for these satellites, have been made public. However, this may also constitute a serious background problem for future γ-astronomy missions with an increased sensitivity of the instrumentation. Finally, leading beyond the boundaries of the magnetosphere, attention is drawn to the still ongoing debate on the source of energetic particles upstream of the Earth's bow-shock and the respective importance of particle leakage and/or acceleration at the magnetospheric boundaries.     

An attempt to derive electron energy spectra for auroral daytime precipitation events

A set of quiet daytime electron density profiles is established on the basis of EISCAT measurements. This set is used as a background correction in the CARD program [Brekke A., Hall C. and Hansen T.L. (1989) Ann. Geophysicae7, 269] in order to derive the energy spectra of precipitating electrons at daytime.For disturbed daytime events on 25–26 June 1985, we find that the particle precipitation typically consists of small fluxes (10⁵ el/cm² sster keV) of high energetic particles (20–30 keV). The Hall: Pedersen conductance ratios for such events are found to be meaningless as an indicator of the energy of the particles, in contrast to nighttime precipitation.     

Morning sector electron precipitation events observed by incoherent scatter radar

Two auroral zone electron precipitation events in the morning sector have been studied in detail using the UHF incoherent scatter radar in northern Scandinavia. The electron density profiles are interpreted in terms of the incoming spectrum of energetic electrons, and it is shown that the spectrum is most energetic at the maximum of the event and softens subsequently. The observations cannot be explained by simple gradient-curvature drift of trapped electrons. It is shown, further, that events appearing to be fresh substorms in magnetometer and riometer data may be no more than intensifications of continuing activity. During a pulsation event the incoming electron spectrum was modulated in energy as well as in intensity. The height and thickness of the resulting radio-absorption layers are derived.