The science case for the EISCAT_3D radar
- Ian McCrea1Email author,
- Anita Aikio2,
- Lucilla Alfonsi3,
- Evgenia Belova4,
- Stephan Buchert5,
- Mark Clilverd6,
- Norbert Engler7,
- Björn Gustavsson8,
- Craig Heinselman9,
- Johan Kero4,
- Mike Kosch10, 11,
- Hervé Lamy12,
- Thomas Leyser5,
- Yasunobu Ogawa13,
- Kjellmar Oksavik14,
- Asta Pellinen-Wannberg4, 15,
- Frederic Pitout16, 17,
- Markus Rapp18,
- Iwona Stanislawska19 and
- Juha Vierinen20
© McCrea et al. 2015
Received: 28 October 2014
Accepted: 3 July 2015
Published: 29 July 2015
The EISCAT (European Incoherent SCATer) Scientific Association has provided versatile incoherent scatter (IS) radar facilities on the mainland of northern Scandinavia (the EISCAT UHF and VHF radar systems) and on Svalbard (the electronically scanning radar ESR (EISCAT Svalbard Radar) for studies of the high-latitude ionised upper atmosphere (the ionosphere). The mainland radars were constructed about 30 years ago, based on technological solutions of that time. The science drivers of today, however, require a more flexible instrument, which allows measurements to be made from the troposphere to the topside ionosphere and gives the measured parameters in three dimensions, not just along a single radar beam. The possibility for continuous operation is also an essential feature. To facilitatefuture science work with a world-leading IS radar facility, planning of a new radar system started first with an EU-funded Design Study (2005–2009) and has continued with a follow-up EU FP7 EISCAT_3D Preparatory Phase project (2010–2014). The radar facility will be realised by using phased arrays, and a key aspect is the use of advanced software and data processing techniques. This type of software radar will act as a pathfinder for other facilities worldwide. The new radar facility will enable the EISCAT_3D science community to address new, significant science questions as well as to serve society, which is increasingly dependent on space-based technology and issues related to space weather. The location of the radar within the auroral oval and at the edge of the stratospheric polar vortex is also ideal for studies of the long-term variability in the atmosphere and global change. This paper is a summary of the EISCAT_3D science case, which was prepared as part of the EU-funded Preparatory Phase project for the new facility. Three science working groups, drawn from the EISCAT user community, participated in preparing this document. In addition to these working group members, who are listed as authors, thanks are due to many others in the EISCAT scientific community for useful contributions, discussions, and support.
Introduction to EISCAT_3D
Why do we need EISCAT_3D?
The interaction between the Sun and the Earth is vital to every aspect of human existence. As well as providing us with heat and light, the Sun supplies the energy which powers the motion of the Earth’s atmosphere and oceans, governing our weather and climate. In addition, the Sun produces the solar wind—a stream of energetic particles which permeates the solar system, carrying with it a magnetic field which interacts with the internally generated magnetism of the Earth and other planets. The science of solar-terrestrial physics (STP) is concerned with understanding all aspects of the relationship between the Earth and the Sun. In particular, it seeks to understand all the different ways that energy from the Sun is deposited in the environments of the Earth and other solar system bodies, the processes by which that energy is converted from one form to another, and the combined effects of all these processes on our environment.
Because of this broad remit, STP overlaps with many other areas of science, including atmospheric physics, solar physics, and plasma physics. It also has many practical goals, including the better prediction and mitigation of space weather to safeguard space-based technology, improved modelling of the Earth’s ionised atmosphere for communications and global positioning applications, and a deeper understanding of the contribution of natural variability to long-term and short-term global change. In a world ever more dependent on space-based systems, and in which an improved understanding of our environment is at the top of the scientific and political agenda, solar-terrestrial physics has become a key science area for the twenty-first century.
Progress in STP is largely driven by observations. Because the solar-terrestrial system is continuously varying, and the interplay between the various processes is so complex, current theoretical models by themselves can only bring us a certain distance in understanding how the Earth’s environment responds to solar influences. Hence, there is a major requirement for high-quality data from continuous, multi-point observations of all the key regions of the Sun-Earth system, from the solar photosphere and corona to the solar wind and magnetosphere, through the ionosphere and thermosphere, and down to the middle and lower atmosphere. This requires a number of different instruments, including satellites, radars, optical imagers, and ground-based magnetic measurements, working in combination to observe different aspects of the coupled system and provide the input data for the development of sophisticated modelling and forecasting techniques. Science on this scale can only be done by international collaboration, and, although some observing instruments are relatively cheap, the development of leading-edge instruments, such as spacecraft and radars, in most cases requires multi-national funding and the coordinated effort of a worldwide research community.
The EISCAT (European Incoherent SCATer) Scientific Association has played a key role in providing world-leading radar systems for use by the whole international research community over the past 30 years. As well as carrying out its own independent experiments, EISCAT has run extensive observing programmes to support a variety of spacecraft and collaborated closely with the other incoherent scatter radars around the world, particularly with those funded and operated by the US National Science Foundation, as part of a global observing programme based around the Geophysical World Days, including the International Polar Year of 2007–2008.
To solve the existing questions related to the upper, partly ionised, atmosphere and its coupling to the lower atmosphere, as well as to the Sun and the solar wind, a new type of incoherent scatter radar must be constructed. This new radar system, EISCAT_3D, will exploit the twenty-first century phased array technology to provide the kind of observations that have never been possible with the existing EISCAT radars.
What is EISCAT_3D?
EISCAT_3D is designed to use several different measurement techniques which, although they have each been used elsewhere, have never been combined together in a single radar system:
The design of EISCAT_3D allows large numbers of antennas to be combined together to make either a single radar beam or a number of simultaneous beams, via a process known as beam forming. In phased array radars, the properties of the beam forming can be changed very rapidly, so that the direction of the radar beams can change every few milliseconds. These capabilities, possible because there are no moving parts, are a huge advantage compared to the traditional kinds of radar using large dishes. They allow the radar either to look in multiple directions simultaneously or to “paint the sky”, repeatedly scanning a single beam through a range of directions, to build up quasi-simultaneous images of a wide area of the upper atmosphere in three dimensions. While radar systems with a single, slow-moving, beam can only show us what is happening in a single profile of the upper atmosphere at any one time, volumetric imaging allows us to see geophysical events in their full spatial context and to distinguish between processes which vary spatially and those which vary in time.
Aperture synthesis imaging
Most radars suffer from the limitation of not resolving any structure smaller than the width of their narrowest (transmitter or receiver) beam, typically of order a kilometre for ionospheric radars. In EISCAT_3D, this limitation is overcome by dividing the core site into a number of sub-arrays, the signals from which will be continuously cross-correlated in a technique similar to the very long baseline interferometry approach used by radio astronomers, except that the baselines here are only a few hundred metres. The result of inverting the cross-correlations is a brightness function showing the distribution of backscatter down to very small scales, less than the width of a normal receiver beam, distinguishing between situations where the beam is evenly filled with electrons and those where the scatter comes from a few discrete intense structures, the study of which could produce exciting new science.
Several of the EISCAT_3D sites will be passive receivers, located at distances between 50 and 250 km from the core site. Like the core site, each remote site will be capable of generating multiple simultaneous beams, and this will enable the transmitter beam from the core site to be imaged simultaneously over a large range of altitudes from a variety of different observing directions. This will make it possible to construct continuous height profiles of parameters such as vector velocity and ionospheric current density, or to look for anisotropic scattering mechanisms, in a manner that cannot be achieved by conventional radars in a way compatible with typical geophysical coherence times.
Scanning, tracking, and adaptive experiments
Because EISCAT_3D is so flexible compared to traditional ionospheric radars, it will allow several new operating modes including the capability to track moving objects such as meteors and space debris or to respond intelligently to changing conditions, for instance by changing the parameters of a scanning experiment. While some existing radars are beginning to use these techniques, they are often limited by factors such as inertia-bound steering. Other novel techniques, including passive radar measurements and active control of the beam shape, for instance to control the shape of phase fronts in the near field, should also be possible with EISCAT_3D.
EISCAT_3D will allow remote continuous operations, limited only by power consumption and data storage. This is important for monitoring the state of the atmosphere, especially as a function of solar variability, as well as capturing unexpected events that appear suddenly and are hard to predict. EISCAT_3D will be an essential tool for validating short- and long-term models for predicting the state of the space environment as well as global change. As the population of the Earth grows and demands on natural resources increase, and as our dependence on space assets continues to grow, the need for accurate forecasting increases.
EISCAT_3D key capabilities
Resolution of space-time ambiguity: EISCAT_3D will have simultaneous multiple-beam capability. This will resolve outstanding issues of spatial-temporal ambiguity (e.g. the dynamics of dusty plasmas in the mesopause region and rapidly moving auroral structures, tracking space debris and meteors).
3D volumetric capability: EISCAT_3D will have 3D volumetric imaging capability throughout its field of view. Such capability is important for studying the variability, coupling, and energy dissipation between the solar wind, magnetosphere, and atmosphere (e.g. Joule heating and field-aligned currents) as this coupling is a function of altitude, latitude, and longitude.
Sub-beam width measurements: The spatial scale of micro-physical processes is much less than the current EISCAT UHF radar beam half-width of 0.5° (e.g. NEIALs, small-scale and black auroras, meteor head echoes, PMSE). EISCAT_3D will have the needed capability to perform interferometry with multiple baseline angles and lengths, a technique already proven by the EISCAT Svalbard Radar, which can be used to investigate these phenomena.
Increased sensitivity and the resulting temporal resolution: With its improved sensitivity and temporal resolution, EISCAT_3D will be able to reach down to the sub-second timescales that are known to exist in auroral features from optical measurements. As Appendix B of Lehtinen et al. (2014) makes clear, EISCAT_3D will be able to measure auto-correlation functions at sub-second time resolutions, under high-SNR conditions, at accuracies better than a few tens of percent errors in multi-parameter fits. Being able to measure multiple plasma parameters at such high time resolutions may provide a key to unraveling some of the cause/effect relationships in auroral forms.
Continuous monitoring of solar variability on terrestrial atmosphere and climate: EISCAT_3D will allow remote continuous operations, limited only by power consumption and data storage. This is important for monitoring the state of the atmosphere, especially as a function of solar variability, and essential for capturing unexpected events that appear suddenly and are hard to predict.
Model validation for space weather and global change: EISCAT_3D will be an essential tool for validating models of the upper atmosphere and space environment, which can be expected to have increasing societal relevance over the coming years.
Atmospheric physics and global change
The global circulation of the middle atmosphere tends to produce polar vortices in the winter hemisphere (Brewer 1949; Dobson 1956; Dunkerton and Delisi 1986; Schoeberl et al. 1992; Fisher et al. 1993), isolating the polar air from that at lower latitudes—the reason, for example, that the ozone holes form preferentially over the poles. While downwelling air dominates the middle atmosphere in the winter hemisphere, the summer hemisphere is dominated by upwelling (see Fig. 2). Adiabatic cooling of the rising air in the polar summer mesosphere produces the lowest temperatures found anywhere in the Earth’s environment (Reid 1989; Lübken 1999; Singer et al. 2003).
In addition to coupling by waves, tides, winds, solar radiation, energetic particles, and chemical composition changes (which can be initiated from either direction), the upper and lower regions of the atmosphere are electrically coupled via a current circuit (Roble and Tzur 1986; Rycroft et al. 2000, 2002) which includes ionospheric currents, thunderstorm activity, and the “clear air” electric field of the lower atmosphere. This electrical coupling is presently very poorly understood. The coupled atmospheric system has a large number of feedbacks, whose importance is presently uncertain and needs to be much better established. It is believed that cosmic rays may be able to modulate cloudiness (Svensmark 1998; Carslaw et al. 2002; Tinsley 2008), that the strength of the polar vortex can be modulated by solar cycle effects (Haigh 1996, 1999, 2003; Labitzke 1987, 2001, 2003, 2004, 2005), and that this may relate to the unexplained correlations between solar wind dynamic pressure and middle atmosphere parameters such as stratospheric wind speed and temperature (Tinsley and Heelis 1993; Arnold and Robinson 2001; Pudovkin 2004).
The behaviour of the lower atmosphere also modifies the spectrum of waves reaching the upper atmosphere in a way which has not been well described, and considerably more information about these feedback mechanisms is required. Processes leading to the formation and transport of ozone-depleting chemicals such as odd hydrogen and odd nitrogen species (Crutzen 1970; Crutzen et al. 1975; Rusch et al. 1981; Solomon et al. 1981; Callis and Natarajan 1986a, b; Seppälä et al. 2006; Verronen et al. 2006) are of profound importance, since UV absorption by ozone fundamentally affects the heat balance of the middle atmosphere, which in turn affects wave propagation. Understanding these factors is thus fundamental to our understanding of atmospheric chemistry and dynamics.
Two of the main aims for EISCAT_3D are to understand the ways in which natural variability in the upper atmosphere, imposed by the solar-terrestrial system, can influence the middle and lower atmosphere, and to improve the predictive capabilities of atmospheric models by providing higher resolution observations to replace the current parameterised inputs. This kind of “system science” requires other instruments too, including different types of radar, ground-based optics, and satellite instruments such as limb sounders. It also requires good coordination between experimentalists and modellers. EISCAT_3D, by virtue of its extraordinary versatility, will sit at the centre of this network of instruments and models, providing a key underpinning data set for this undertaking.
Dynamical coupling in the atmosphere
Dynamical coupling by winds, waves, and tides is one of the most important mechanisms connecting the different regions of the atmosphere (Fritts and van Zandt 1993; Holton et al. 1995; Hocking 1996; Hamilton 1996, 1999; McLandress 1998; Meriwether and Gardner 2000). Much of this wave energy occurs at mesoscales, in atmospheric gravity waves with periods of less than an hour, speeds of order 100–200 m/s, and wavelengths of hundreds of kilometres, chiefly arising from processes in the troposphere (Hooke 1986). In addition, larger scale tides and Rossby waves, with periods of a few hours, also arise from lower altitudes and propagate upwards into the thermosphere (Rossby et al. 1939; Lindzen 1979; Forbes 1982a, b; Chelton and Schlax 1996).
At mesospheric altitudes, upgoing gravity waves break into turbulence (Fritts and Luo 1995; Prusa et al. 1996), heating the middle atmosphere and depositing their energy and momentum flux into the background mean flow. This turbulence fundamentally affects the global circulation of the atmosphere through the mechanism of gravity wave drag (Holton et al. 1995). These effects are highly variable but are most pronounced in the summer hemisphere. The dissipation of wave energy from below is thought to provide the majority of the momentum flux to the mesosphere and lower thermosphere (Ebel 1984). Under the right conditions, this turbulence can also be associated with the presence of mesospheric thin layers (see “Solar-terrestrial effects on middle atmosphere chemistry”).
In addition to waves propagating upwards, another class of waves is created at ionospheric altitudes by geomagnetic activity (e.g. Richmond 1978; Hunsucker 1982). Some of these waves are at mesoscales, as described above, while some occur as travelling ionospheric disturbances (LSTIDs and MSTIDs) with wavelengths of over a thousand kilometres, periods on the order of an hour or more, and propagation speeds of up to 1000 m/s. These waves generally propagate equatorward from high latitudes, where they are formed by the deposition of energy into the upper atmosphere via Joule heating, particle heating, or mechanical forcing of the neutral atmosphere via the Lorentz force (Brekke 1979). Using the Arecibo radar, Djuth et al. (1997, 2004) have demonstrated how incoherent scatter techniques, including the use of plasma line measurements, can reveal the continuum of thermospheric gravity wave activity. These techniques will be highly relevant to EISCAT_3D.
Improved measurements of both large-scale and small-scale dynamics are also critically important because many transport phenomena in the upper atmosphere are hard to explain without understanding the wave dynamics. For example, Stevens et al. (2003) found that space shuttle plumes in the lower thermosphere were transported much faster than expected from current models. More recent work by Yue and Liu (2010) has indicated that such observations can be explained by the superposition of tides and planetary waves, and EISCAT_3D would be capable of providing the data to substantiate this type of conclusion.
Solar-terrestrial effects on middle atmosphere chemistry
The ionised part of the mesosphere, known as the D region, is extremely important because of its complex chemistry, which has significant implications for structure and dynamics of the middle atmosphere. The most energetic precipitating particles, such as solar protons or energetic electrons with energies in the range from tens of kiloelectronvolts to tens of megaelectronvolts, penetrate down to D region altitudes, creating significant chemical changes, including enhancements in odd nitrogen and odd hydrogen species (Rusch et al. 1981; Solomon et al. 1981; Seppälä et al. 2006; Verronen et al. 2006). These particles, known as solar energetic particles (SEPs), are usually seen in the first minutes following a solar flare (Cane et al. 1986; Reames 1990) and can reach stratospheric altitudes (Jackman et al. 2005a, b) or even to ground level. Even less energetic particles (protons with energies of tens of megaelectronvolts or electrons with energies of hundreds of kiloelectronvolts) can reach stratospheric altitudes down to around 50 km.
Alternatively, ozone depletion can occur more slowly as thermospheric species descend into the stratosphere (e.g. Clilverd et al. 2006). While odd hydrogen species are short lived and mainly affect the chemistry of the lower mesosphere and upper stratosphere, the longer lived odd nitrogen species have been shown to descend to altitudes as low as 25 km in the southern hemisphere (Callis et al. 1996; Randall et al. 1998). This descent often occurs during the late winter and early spring, though the effect does not occur every year, for reasons which are unclear, but probably related to the variability of middle atmospheric dynamics (Callis and Lambeth 1998).
In addition to energetic particle precipitation, ablation of meteors changes the chemistry of the mesosphere by adding metallic ions and aerosols in the form of meteor smoke. The Sodankylä ion and neutral chemical model, which represents the state-of-the-art in describing D region chemistry (Verronen et al. 2002; Enell et al. 2005), includes some 400 chemical reactions between 65 ions and 15 neutral species. Many of these reactions have not been extensively observed in practice, and the complexity of D region chemistry can make the interpretation of observations very difficult.
Changes in dynamical coupling are likely to be an important factor in explaining how the atmosphere responds to those changes in atmospheric chemistry which modulate ozone densities. The heat balance of the middle atmosphere, largely determined by ozone, is likely to be a key factor in regulating which waves are able to propagate from the troposphere and stratosphere into the mesosphere and thermosphere, and which are reflected or dissipated (Graf et al. 1998; Gabriel et al. 2007). This affects not only the upper atmosphere but also the structure and dynamics of the lower atmosphere, because there is evidence that reflection of wave energy in the stratosphere may be a precursor of certain types of unusual weather event (Baldwin and Dunkerton 2001).
It is increasingly accepted that, in order to produce models which fully include all of those stratospheric processes which can influence weather and climate, the upper altitude ceiling of these models needs to be raised to upper atmospheric heights, so that the geospace processes capable of creating odd hydrogen and odd nitrogen species can be fully included (e.g. Roble 2000, Schmidt et al. 2006). EISCAT_3D will provide the underpinning observations, especially concerning the frequency and extent of energetic particle events, which will make such model improvements possible, and EISCAT_3D data will allow the results of the modelling to be validated.
When strong scattering layers such as PMSE or PMWE are absent, the D region is often very difficult to observe with radars because of the low density of free electrons in this region. In this respect, the high power, large aperture, and low frequency of EISCAT_3D will give it an advantage over any other type of modern incoherent scatter radar (ISR), providing a facility with considerable synergy to the already existing European assets for mesospheric research, such as rockets, optical instruments, and other types of radar. Since most current ISRs are not capable of observing much below 80 km, a key challenge for EISCAT_3D will be to probe the extent to which these energetic particles can reach significantly lower altitudes, especially during very disturbed conditions (Jackman et al. 2005a, b). This is particularly true for energetic electron precipitation, which is hard to measure accurately in any other way, and is an important factor for global atmospheric models. While EISCAT_3D might not be able to make the full range of required measurements by itself, its data, in conjunction with measurements from lidars and other types of radar, will provide unprecedented altitude coverage of electron density profiles in this important region. Another important part of EISCAT_3D’s mission will be to provide a continuous monitor of the high-latitude D region, describing its response to forcing by solar radiation, particle precipitation, solar proton events, gravity waves, meteoric input, and cosmic rays. The latitude and longitude coverage of EISCAT_3D will also allow the spatial effects of energetic particle precipitation on the atmosphere to be investigated.
As well as passively observing the changing chemistry of the mesosphere, the EISCAT facilities have the ability to test our models of the system by perturbing the middle atmosphere in a known way through active heating experiments (Rietveld et al. 1986; Kero et al. 2000). Increasing the temperature of the D region plasma reduces its recombination rate and increases the formation of negative ions, allowing chemical models to be tested (Ennel et al. 2005). The availability of an EISCAT heating facility close to EISCAT_3D, capable of modifying the ionospheric D region, would be a very important complement to the new radar, providing an unparalleled capability for conducting controlled experiments in the middle atmosphere.
Beam focusing of the radar itself could be used to cause ionisation and even breakdown in the stratosphere, mesosphere, and lower ionosphere. Such experiments have the potential to give information on a range of atmospheric properties and constituents that are not accessible by natural excitations. A somewhat related topic in the literature is microwave discharge in the stratosphere, which has been suggested for the mitigation of ozone depletion (Akmedzhanov et al. 1995). The transmit antenna of EISCAT_3D needs to be designed appropriately to enable sufficient focusing for experiments on ionisation and breakdown in the upper atmosphere. The capability to focus the radar beam for Joule heating studies would also be useful to the development of solar power satellites, which would beam the energy back to Earth by microwaves (Leyser and Wong 2009). These powerful beams should suffer as small an energy loss in the atmosphere as possible. Focusing experiments would give information on the atmospheric response to very high frequency beams.
Dynamical and chemical coupling in the mesosphere
The mesosphere (at altitudes from about 50 to 90 km) is a very important area of the atmosphere, critical to the understanding of energy coupling, but often very difficult to observe with radars. The mesosphere has a very complicated chemistry, characterised by neutral and charged molecular species and cluster ions consisting of ice and meteoric dust. This chemistry is controlled partly by energetic particle precipitation and also by dynamical processes in which waves, tides, winds, and turbulence generated in the lower atmosphere interact with those generated above (Vincent 1984). Adiabatic cooling of the upwelling air mass produces a temperature minimum of −140 °C at the polar summer mesopause (about 85 km), making it the coldest region of the Earth’s environment (McIntyre 1989). This interplay of chemistry and dynamics is particularly manifested in the phenomenon of mesospheric thin layers, which show how both processes can affect this region of the upper atmosphere (e.g. Ecklund and Balsley 1981).
Although PMSE layers often appear almost laminar, the shape of PMSE spectra suggests that the layers may contain smaller scale coherent structures which have not yet been imaged but may be due to sudden changes in refractive index (Cho and Röttger 1997). These small-scale structures may be part of the explanation for the fact that PMSE layers appear to be strongly aspect sensitive, especially at the lowest altitudes (Smirnova et al. 2012). The reason for this aspect sensitivity is not well known; it might be due to the shape of the scattering structures themselves or result from polarisation electric fields, which arise from the charging of heavy ions of different sizes (Blix 1999). Alternatively, the aspect sensitivity could be due to the presence of waves or to horizontal structure in the turbulence, which could be investigated by volumetric imaging (Hill et al. 1999). The ability of EISCAT_3D to rapidly image the mesospheric wave field will make it one of the key tools for studying the anisotropy and horizontal structure of PMSE layers. The multi-static nature of the new radar will allow the layers to be imaged simultaneously from a variety of aspect angles. In principle, this would make it possible to observe coherent scatter from PMSE layers with one EISCAT_3D site, while another site probes the same volume via the incoherent scatter spectrum of the background plasma, at an angle where coherent scatter is weak or absent.
The shape of the backscatter spectrum at the VHF frequencies selected for EISCAT_3D is sensitive to key small-scale parameters of PMSE layers, such as the grain size of the charged aerosol particles, which is of order 5–70 nm (Hervig et al. 2009). The wide 3D coverage afforded by the new radar will make it possible to measure how the grain size varies laterally, as well as according to height. Measurements so far suggest that the grain size is likely to be gravitationally ordered, with larger particles predominating at lower altitudes (Rapp et al. 2003a). It is also known that PMSE and noctilucent cloud layers are associated with turbulence, and one of the proposed applications of EISCAT_3D is to use the new radar in conjunction with other radars at different frequencies to explore the spectrum of this turbulence and compare it with theoretical predictions which link the Schmidt number of the turbulence to the grain size of the layer particles (Rapp and Lübken 2003; Rapp et al. 2008).
Although strong scattering layers tend to be absent outside the summer months, another thin layer phenomenon known as polar mesospheric winter echoes (or PMWE) can be seen at other times of year (Czechowsky et al. 1989; Lübken et al. 2006, 2007; Kirkwood et al. 2002, 2006a, b, Zeller et al. 2006). PMWE layers generally occur at lower altitudes than PMSE (50–80 km) and are less intense, only being seen by radars when the background electron density of the mesosphere is high, for example when the solar X-ray flux is enhanced or energetic particle precipitation is present (Kirkwood et al. 2002). PMWE occur at higher temperatures than PMSE. They are also more aspect sensitive and sometimes seem to have a high horizontal propagation speed. They are clearly not the same as PMSE, and their nature is still somewhat uncertain—there are some suggestions that they may involve charged aerosols (e.g. Stebel et al. 2004; Belova et al. 2008; La Hoz and Havnes 2008), while others have suggested that PMWE layers might be purely signatures of atmospheric turbulence (Lübken et al. 2006, Brattli et al. 2006) or that they arise from highly damped viscosity waves generated by the reflection of infrasound (Kirkwood et al. 2006b).
PMSE and PMWE layers are not the only types of anomalous radar echoes which can be measured in the middle atmosphere. Rocket measurements (e.g. Thrane 1986; Blix et al. 1990; Strelnikov et al. 2009) have shown that other types of fine structure can also exist in the D region. These are believed to be associated with plasma instabilities, but the process responsible for their formation is disputed, and it is possible that more than one type of instability may be contributing to these structures. The high-quality continuous data arising from EISCAT_3D will make it possible to study these rare varieties of mesospheric plasma structure and identify their causes.
Atmospheric turbulence in the stratosphere and troposphere
The stratosphere (between about 12 and 50 km in altitude) contains the ozone layer, which is vital for life on Earth, since it absorbs the energetic part of the solar UV radiation, preventing it from penetrating to the ground. The stratosphere is a region of increasing temperature with height, since absorption of UV by ozone progressively limits the amount of radiation available to heat the lower altitudes. This temperature gradient in the stratosphere means that there is relatively little convective turbulence and that horizontal mixing is much more effective than vertical transport (Chen et al. 1994; Shepherd et al. 2000). Turbulence can still occur, however, due to variations in the jet stream and wave activity from thunderstorms or local relief (e.g. Kirkwood et al. 2010b), propagating upwards from the troposphere. The stratosphere is notable for the strong interaction it exhibits between radiative, chemical, and dynamical effects. For example, variations in the solar UV output (one of the most variable parts of the solar spectrum) can modulate the stratospheric temperature via ozone absorption, changing the heat balance and thereby modifying the spectrum of winds, waves, and tides which is able to propagate between the upper and lower atmosphere (e.g. Hartmann 1981).
The stratosphere can exchange energy with both the troposphere below and the mesosphere above. A striking example of this type of interaction is shown in sudden stratospheric warming events, which occur when the circulation of the polar vortex is disrupted, slowing down or even reversing the direction of the vortex winds during a period of a few days (Labitzke 1972, 1981; Simmons 1974). These events occur when Rossby waves, propagating upward from the troposphere, grow to large amplitudes as a result of unusual weather patterns. The growing waves interact with the circulation of the stratosphere and, if their upward propagation becomes blocked, they deposit their energy as heat at stratospheric altitudes, causing major changes in stratospheric temperature and circulation (McIntyre 1982; Limpasuvan et al. 2004). Recent work, using incoherent scatter radars as well as other types of radar, has demonstrated that these sudden stratospheric warmings affect not only the stratosphere but also the dynamics of the mesosphere and thermosphere (Kurihara et al. 2010), and that the effects are not only restricted to the polar regions but can be global in scale (Goncharenko and Zhang 2008).
The troposphere, at heights up to about 12 km altitude, is the region of the atmosphere in which weather phenomena take place. Because this region contains some 75 % of the Earth’s atmosphere, it is by far the most important region in terms of its effects on human activity. In the troposphere, the air temperature falls steadily with decreasing height until the tropopause is reached, and the temperature begins to increase with height mainly due to the increased trapping of solar radiation, by stratospheric ozone. The troposphere exchanges energy with the stratosphere by dynamical processes such as wind and wave activity and by the re-radiation of solar energy back to the layers above. A well-known phenomenon is the trapping of solar radiation by greenhouse gases in the lower atmosphere, which can feed back to the upper atmosphere by reducing re-radiation, producing cooling effects and changing the dynamics (Lindzen 2007; Archer and Pierrehumbert 2011). Chemical effects can produce similar changes in dynamics, as described above, but which of these mechanisms is most important, the circumstances under which the different processes dominate, and whether any of them is really significant in terms of its effects on the lower atmosphere are still matters of intense debate.
The advanced capabilities of EISCAT_3D for digital beam forming (including post-beam steering within a wide transmitter beam), radar imaging, and coherent integration will make it a superb instrument for stratosphere and troposphere studies, by exploiting coherent scatter from atmospheric turbulence and temperature gradients. VHF radars are very suitable for this type of work, since the radar cross-section of naturally occurring structures is high at these frequencies, the spatial and temporal coherence of the backscatter is large, and the spectrum is narrow, making it easily detectable (Rüster et al. 1998).
Above the lower stratosphere, however, the strength of radar echoes decay rapidly. The viscous sub-range limit for EISCAT_3D wavelengths is reached between 30 and 40 km (e.g. Kato 2005), although, in some conditions (e.g. solar proton events), echoes should be detectable even in this gap. Above this altitude, there may be little for EISCAT_3D to scatter from, until the ionisation of the D region begins to be noticeable between 70 and 80 km. The altitude region between 30 and 70 km is known as the “radar gap”, and observations here may still have to rely on other techniques, such as lidars or satellite limb sounders.
Although EISCAT_3D will probably not be able to observe the radar gap, the new radar will make important inputs to understanding the coupling processes which occur there, by observing winds and waves in the mesosphere (above) and in the lower stratosphere and troposphere (below), as well as the energetic particles reaching the mesosphere, and looking for evidence of fine-scale structure which would indicate the presence of turbulent mixing. Measuring the dynamics of the atmosphere above and below the stratosphere provides information on which waves are being dissipated at stratospheric heights, while observing energetic particles constrains the modelling of chemical processes which can modulate ozone. Combining EISCAT_3D data with other inputs such as satellite observations of stratospheric dynamics and photometric measurements of ozone content will lead to an improved understanding of the energy balance in the polar middle atmosphere.
While it is clear that the troposphere can strongly influence the stratosphere, via the strong flux of upward-propagating waves generated at low altitudes, the idea that the stratosphere might be able to impose some form of downward control on the troposphere has been much less accepted, until recently (Kuroda and Kodera 1999; Baldwin and Dunkerton 1999; Song and Robinson 2004). If stratospheric effects on the troposphere were shown to exist, this would provide an extremely interesting link in a chain of processes connecting the upper atmosphere to effects on weather and climate, however indirect that connection might be.
Since the beginning of the present century, it has become clearer that there are mechanisms which can allow downward control of the troposphere. A pair of well-known papers by Baldwin and Dunkerton (1999, 2001) showed strong evidence for stratospheric precursors of anomalous tropospheric weather patterns, leading to a vigorous debate on how such a sequence could arise. Three possible mechanisms have been suggested. Firstly, the mean flow of the lower stratosphere can impose a “refractive” effect on the flux of upward-propagating Rossby waves (e.g. Hartmann et al. 2000; Limpasuvan and Hartmann 2000) while Rossby waves can even be completely reflected from higher stratospheric altitudes (e.g. Perlwitz and Harnik 2003, 2004). In this way, changes in the stratosphere may be able to modulate how much of the lower atmospheric wave flux the stratosphere can accept. Secondly, changes in the potential vorticity of the stratosphere, resulting from wave-induced forcing, may be able to change the winds and temperatures of the troposphere, allowing information to propagate downwards across the tropopause (e.g. Haynes et al. 1991; Holton et al. 1995). Thirdly, there is evidence that when stratospheric wave amplitudes are large, the interaction between waves and mean flow in the stratosphere can generate perturbations sufficiently large that they can propagate downwards to tropospheric heights. In addition to these dynamical coupling mechanisms, there may be chemical coupling between the stratosphere and troposphere which is, as yet, not well understood.
A clearly established link between upper atmosphere chemistry and dynamics with variability in the troposphere might have significant implications, including providing an explanation for apparent solar cycle signatures seen in tropospheric circulation and suggesting possible links between long-term variations in stratospheric ozone or greenhouse gases and changes in the lower atmosphere. However, the extent of downward control is still a matter of vigorous debate, and great care will be needed in interpreting the data.
There has been considerable recent debate about the idea that geospace processes can influence the troposphere directly, without being mediated by the mesosphere and stratosphere. One controversial proposal is that cosmic rays can promote cloud formation, by modulating the electrical conductivity of the lower atmosphere. In this scenario, the ionisation of air by cosmic rays has been proposed to impart an electric charge to aerosols, encouraging them to clump together in groups large enough to form cloud condensation nuclei (CCN). Since the cosmic ray flux varies in antiphase with the solar cycle, and is probably also modulated by longer term trends in solar activity, the possibility of CCN creation by cosmic rays has been proposed as a direct link between solar variability and tropospheric climate (e.g. Svensmark and Friis-Christensen 1997; Svensmark 1998; Marsh and Svensmark 2000a, b). The most recent evidence suggests, however, that the observed cosmic ray variability is not capable of modulating the number of CCNs anything like strongly enough to produce a major effect on global tropospheric cloud cover (Pierce and Adams 2009; Kulmala et al. 2009). More recent versions of the theory have proposed modifications, such as limiting the connection to a linkage between cosmic rays and stratospheric (as opposed to tropospheric) clouds (Erlykin et al. 2010). It is believed that stratospheric clouds might be more effective than tropospheric clouds, in terms of their effects on climate, since stratospheric clouds re-radiate at a much lower temperature than clouds in the lower atmosphere.
Although EISCAT_3D is primarily intended as an upper atmosphere radar, its considerable sensitivity will also make it useful for observations up to an altitude of around 30 km, crossing the boundary between the troposphere and the stratosphere. EISCAT_3D has a different frequency than most other lower atmosphere radars, and its troposphere/stratosphere observations would therefore be complementary to data obtained by other radars in northern Scandinavia, as well as by satellites and balloon-borne sounders. The volumetric capabilities of EISCAT_3D can also be used at these altitudes, for example to make measurements of wind vorticity on scales of about 10 km. This could be an important parameter for meteorological studies, since it has been suggested that vorticity on this scale may trigger storms (Schumann and Roebber 2010). The physics of the low-altitude scattering mechanism at these frequencies is also an interesting issue which should be studied, including issues such as the radar cross-section and the spectral index of atmospheric turbulence and its scattering properties, such as aspect sensitivity.
If a high-frequency (HF) heater is available, as is planned to be the case for the EISCAT_3D system, it should be possible to create artificial periodic irregularities (APIs) by forming a standing wave between the ground and the lower ionosphere. Variations of refractive index occur at the nodes of the standing wave, and these can be used as targets for atmospheric scattering. This technique has been demonstrated with the existing EISCAT systems (Rietveld and Goncharov 1998) but has not been fully exploited with the existing EISCAT radars because of their limited suitability for lower atmosphere work. However, the API technique provides the ability to partially close the radar gap because observations are possible from as low as 55 km (Belikovich et al. 2002).
Short- and long-term changes in the upper atmosphere
The middle and upper atmosphere exhibit a huge amount of natural variability, on timescales from sub-seconds to decades. Reasons for this variability include changes on the Sun, solar wind forcing, plasma instabilities, turbulence, wave-wave interaction, and wave-particle coupling. Because the atmosphere is highly non-linear and coupled, the causes of such variability are not easily understood, and even the best physics-based models cannot reliably predict the evolution of the high-latitude upper atmosphere, for even the largest scales, on timescales of more than a few days (Scherliess et al. 2009; Schunk et al. 2011).
Superimposed on the small-scale variability of the middle and upper atmosphere are some long-term trends, whose causes and extents are subjects of vigorous debate. Roble and Dickinson (1989) and Rishbeth and Roble (1992) were among the first authors to draw attention to the fact that, as the lower atmosphere warms due to increased heat trapping by greenhouse gases, the reduction in heat re-radiated to the upper atmosphere should cause the mesosphere and thermosphere to cool and contract. Using the best thermosphere/ionosphere models available at the time, they predicted that a doubling of greenhouse gas concentrations in the lower atmosphere would reduce the air density at 300 km by up to 40 %, lowering the peak height of the ionosphere by 15–20 km and reducing the thermospheric temperature by 40 K. This would have some significant effects, for example in increasing the operational lifetime of satellites because of a reduction in ion drag.
Long-term cooling of the mesosphere might lead to increase of the incidence of mesospheric thin layers (e.g. Gadsden 1990, 1998). Analysis carried out by Bremer et al. (2006) suggests that although there may be some signs of a trend towards brighter noctilucent clouds and a longer PMSE season, the statistical evidence is presently too weak to confirm this as being a significant trend. Also, Kirkwood et al. (2008) and Pertsev et al. (2014) find no statistically confident long-term trend in moderate or bright NLC occurrence.
The recent protracted solar activity minimum also seems to have resulted in an unprecedented contraction of the Earth’s upper atmosphere (Qian et al. 2008; Tulasi Ram et al. 2010, Solomon et al. 2010). Combining volumetric observations of ionospheric velocity made using EISCAT_3D with simultaneous observations of thermospheric neutral wind, using e.g. a scanning Doppler imager, will provide a unique possibility to measure the density of the thermosphere in the E and F regions (e.g. Kosch et al. 2011a and references therein). Changes in neutral density, affecting the orbits of space debris objects, can be very dangerous because it makes it more difficult to predict their position, making it very important to secure better predictions by improving the current models (Klinkrad 2010; Lewis et al. 2011). EISCAT_3D will be very valuable in this respect, since it can not only measure the underlying atmospheric processes but also observe the debris objects themselves (see “Space debris”).
It should be noted that, regardless of the sensitivity of EISCAT_3D, a combination of measurements and modelling will always be needed to recover the parameters of the thermosphere. In general, the parameters needing to be modelled are the neutral density, composition and collision frequencies for energy, and momentum transfer between ionised and neutral species. Reliable estimation of these can be complicated at high latitudes, especially during active geomagnetic conditions, when the composition and dynamics of the upper atmosphere are perturbed by processes such as Joule heating and auroral precipitation. Because of this, a close relation between EISCAT_3D and modelling will be needed, allowing model and radar results to interact to fully utilise the synergy between them. “Ionospheric modelling” contains some further thoughts in this direction.
Space and plasma physics
The stream of charged particles, the solar wind, blows continuously from the Sun. When it hits the Earth’s magnetosphere, it is compressed to a radius of about 70,000 km on the dayside by the pressure of the solar wind and stretched into a long tail extending at least 3.5 million km into space on the nightside of the Earth. Some of the energy carried by the solar wind penetrates inside the magnetosphere, and a significant part of it dissipates eventually in the Earth’s atmosphere. The activity of the Sun varies on short (minutes) to long (millions of years) timescales. Perhaps the most well known is the 11-year sunspot cycle; as the number of sunspots increases, so does solar activity. During high solar activity, events called coronal mass ejections (CMEs) often take place, which suddenly and violently release bubbles of gas (plasma) and magnetic fields from the solar atmosphere. Large and fast CMEs can approach masses of 1013 kg and velocities of 2000 km/s. Earth-impacting CMEs can result in significant geomagnetic storms. During the declining phase of the solar cycle, the high-speed solar wind emanating from the coronal holes runs into the slower solar wind, and the interaction leads to a compression of the plasma and magnetic fields, forming corotating interaction regions (CIRs). Those have been found to cause also geomagnetic storms and sub-storms. CMEs and CIRs affect the ionosphere mainly by the process of magnetosphere-ionosphere interaction, whereas some other effects from the Sun like solar energetic particles (SEPs) and radiation bursts at different wavelengths can affect directly the ionosphere.
Observations by the EISCAT_3D radar can hence monitor the direct effects from the Sun on the ionosphere-atmosphere system as well as those caused by solar wind-magnetosphere-ionosphere interaction. In addition, EISCAT_3D can be used to remotely sense the magnetosphere. Because the magnetosphere occupies such a huge volume of space around the Earth, it is very difficult to observe its large-scale behaviour with in situ spacecraft. However, because of the Earth’s converging magnetic field geometry, the high-latitude ionosphere acts as an excellent screen for the magnetosphere; processes occurring over hundreds of thousands of kilometres in magnetospheric space are projected down into a few hundred kilometres of the ionosphere—a volume which is feasible for mapping by an imaging radar.
As discussed above, the high-latitude ionosphere is strongly influenced by processes in near-Earth space. In addition, the ionospheric plasma can be pumped by powerful radio waves at frequencies close to the ionospheric plasma frequency. Experiments utilising the heating facility can be used to study plasma physics in a natural laboratory, the ionosphere.
Plasma convection and multi-scale coupling
In the high-latitude ionosphere, plasma flows and 3D currents are created by the interaction between the solar wind and the terrestrial magnetosphere. The large-scale plasma convection in the ionosphere is relatively well understood and modelled. At high latitudes, the strength and size of the convection pattern, quantified by the so-called cross polar cap potential, are mainly controlled by the interplanetary magnetic field (IMF) carried by the solar wind. Both EISCAT and the Millstone Hill incoherent scatter radar have made important contributions to our understanding of this global convection at both high and middle latitudes, and one of the available models is based on the data from the latter facility (Foster et al. 1986). A great advantage of the Millstone Hill radar is its ability to cover a large area by azimuthally scanning with the dish antenna at very low elevation. The large array of SuperDARN HF radars also look at low elevation, probing a medium size area with a spatial resolution of about 45 km in range and time resolution of 1–2 min. The radars have proven to be very useful for studying the medium-scale dynamic convection patterns, in specific on the dayside. However, on the nightside, SuperDARN often cannot measure any drifts, probably because its signal gets absorbed during conditions of aurora. The difficulties with the HF radar technique for nightside auroral studies may also be related to the complex dynamics of the nightside aurora and its structuring down to much smaller scales. The incoherent scatter technique at VHF or UHF frequencies combined with volumetric imaging will not only allow the resolution of medium-scale plasma convection under all conditions but also measure electron densities and electron and ion temperatures.
In the magnetotail, satellite measurements have shown that Earthward plasma flow in the plasma sheet is dominated by transient fast flows in ambient plasma convection (e.g. Baumjohann et al. 1990). The fast flows have been observed to appear as bursty bulk flow (BBF) events on a timescale of 10 min, with peak velocities about one order of magnitude above the average convection velocities (Angelopoulos et al. 1994).
The BBFs have been observed to be associated with north-south-extending auroral structures, also known as auroral streamers in the ionosphere (e.g. Henderson et al. 1998; Kauristie et al. 2003). However, the details of the flow pattern are beyond the resolutions of present observing facilities. It has been suggested that the major part of Earthward transport of plasma and magnetic flux in the magnetotail actually takes place in the form of BBFs. There is clear evidence that BBFs are initially formed by magnetic reconnection (Øieroset et al. 2000), but this does not explain how they can penetrate so deep into the inner magnetosphere. A theoretical model associating BBFs with underpopulated flux tubes or “plasma bubbles” was developed by Chen and Wolf (1993), and it is supported by many in situ measurements, e.g. by the Cluster satellites (Nakamura et al. 2005; Walsh et al. 2009). An essential part of the bubble model is the polarisation electric field inside the bubble and associated shear flows and field-aligned currents.
Sub-storms, storms, and satellite coordination
The steady plasma convection in the high-latitude ionospheres is frequently disturbed, especially on the nightside of the globe. The reason is a phenomenon known as a magnetospheric sub-storm (Akasofu 1964). Magnetospheric sub-storms begin with a growth phase, when a part of the energy derived from the solar wind is stored in the magnetotail. The energy is a consequence of effective coupling between the IMF carried by the solar wind and the Earth’s magnetic field; this process is most efficient when the IMF has a southward component. The expansion phase of the magnetospheric sub-storm explosively releases the stored energy causing large-scale changes in the magnetosphere as well as in the ionosphere: particle acceleration and precipitation, fast plasma flows, enhanced field-aligned currents, enhanced ionospheric electrojets, and spectacular auroral displays. During the expansion phase, intense and time-varying electric fields and currents exist in the ionosphere and those can cause power grid blackouts and damage to transformers. The whole duration of a sub-storm, including growth, expansion, and recovery phases, is typically a couple of hours.
The question of which processes control these very dynamic releases of stored energy in the magnetotail continues to be controversial. It has been unclear whether a sub-storm starts with the formation of the near-Earth neutral line (NENL) in the magnetotail at 20–30 Re or by a disruption of cross-tail current in the near-Earth magnetotail at 10 Re (e.g. Angelopoulos et al. 2008) and whether the triggering mechanism is internal to the magnetosphere or externally controlled, e.g. by variations in the solar wind properties. It is not known what effect the state of the magnetosphere has in producing a particular response mode (e.g. sub-storm, pseudobreakup, or steady magnetospheric convection). Mass loading of the plasma sheet by ionospheric oxygen may have a dramatic effect in the tail, and eventually on the dayside, when convection transports plasma to the dayside reconnection region (McPherron et al. 2008). It has also been suggested that ionospheric conductivities could play an important role in allowing the currents to close via the ionosphere. In addition, the whole nature of reconnection of magnetic field lines in space plasmas is a subject of intense theoretical and observational research (e.g. Eastwood et al. 2010).
Magnetospheric sub-storms require a period of enhanced energy input (southward interplanetary field) from 30 min to 1 h. If the energy input continues significantly longer (>3 h), a magnetic storm develops. Such storms often follow from the interaction of a fast solar wind stream or an interplanetary magnetic cloud. Magnetic storms typically last from about 12 h to a few days. Storms are characterised by the formation of an intense ring current encircling the Earth with current peak at about 4 RE, i.e. well inside the geostationary orbit. The ring current is populated both by efficient convection and injection of plasma sheet particles into the inner region and by strongly enhanced ion outflow from the ionosphere. While sub-storms can occur without magnetic storms, almost all storms also include sub-storm activity (e.g. Pulkkinen 2007). Space weather phenomena (see “Space weather and service applications”) often accompany (strong) magnetic storms.
Since such a large portion of the near-Earth space and upper atmosphere is involved in the disturbance produced by a magnetospheric sub-storm or magnetic storm, simultaneous multi-scale observations would be needed both in space and in the ionosphere. ESA’s Cluster mission was the first multi-satellite mission to address the question of resolving temporal and spatial ambiguity in the near-Earth space by using four satellites. Cluster had also an extensive ground-based coordination programme (e.g. Opgenoorth and Lockwood 1997; Amm et al. 2005). Another ongoing multi-satellite mission, the NASA Themis mission, is specifically dedicated to study sub-storms. Themis is supported by an extensive number of ground-based observatories in Canada, each including a magnetometer and an all-sky camera. In the future, new multi-satellite missions are expected. The Magnetospheric Multiscale Mission (MMS) is a NASA mission to study the Earth’s magnetosphere using four identical spacecraft flying in a tetrahedral formation, building upon the successes of the ESA Cluster mission. The MMS mission was launched successfully on March 12th 2015.
Phased array incoherent scatter radars provide us with comprehensive ionospheric data locally and over medium and small scales. EISCAT_3D is designed to create this opportunity in the Scandinavian sector complementing the existing phased array incoherent scatter radars PFISR in Alaska and RISR in Canada, but providing multi-scale and multi-static observations of plasma parameters, including ionospheric conductivities and electric fields, which can be used to calculate the 3D currents. The most important asset of IS radars is the measurement of all the important plasma parameters, not obtainable by any other single measurement techniques.
Auroral dynamics and NEIALs
During magnetospheric sub-storms and magnetic storms, the auroral oval is wide and aurora can be seen even at mid-latitudes. However, auroras are present continuously and the auroral oval in the nightside ionosphere is most of the time located within northern Scandinavia. Since this area contains a lot of different kinds of ground-based instrumentation including auroral cameras (e.g. ALIS and MIRACLE networks) and photometers, magnetometers, riometers, tomographic satellite receivers, etc., it represents a unique location on the globe. In addition, two rocket launch sites (Esrange and Andøya) are located in the area.
Evidence for multiple scales in aurora come from satellite and ground-based measurements. The outer scale is the so-called inverted-V structure, typically about 100 km wide when measured by a low-orbiting satellite. Ground-based optical and radar measurements often see auroral arcs with widths of some tens of kilometres (e.g. Knudsen et al. 2001). Structures at 1 km and 100 m scales are also seen (Partamies et al. 2010), and ground-based optical measurements have revealed arc widths down to tens of metres (Maggs and Davis 1968). Large- and medium-scale arcs are often associated with a potential difference between the ionosphere and the magnetosphere, accelerating the electrons into the ionosphere (Mozer et al. 1980; Carlson et al. 1998). How the potential drop develops and to which magnetospheric processes it is related continues to be unclear (e.g. Borovsky 1993). The origin of narrow auroral arcs is even less understood, even though it has been suggested that Alfvén waves could account for some of the structures (e.g. Keiling 2009).
The past studies utilising optical, radar, and satellite observations have helped to establish the typical electrodynamic structure of medium-scale (width of some tens of kilometres) auroral arcs (e.g. Marklund 1984; Aikio et al. 1993, 2004). However, small-scale structures are more challenging to measure. Satellite and rocket flights over these structures give snapshots with a timescale of less than a minute, and the measurement is 1D. The conventional one-beam radar measurement suffers from space-time ambiguity: it sees only a part of the auroral structure at a time. Since the beam width of the current EISCAT UHF radar is about 2 km in the E region and 6 km at 300 km, the auroral structures often fill only partially the radar beam and hence the spectrum of auroral plasma cannot be correctly estimated.
Structures and boundaries in the ionosphere
In addition to aurora (associated with increased electron densities inside arcs), many other kinds of plasma structures exist in the ionosphere. As mentioned in the previous section, one such large-scale structure is the auroral oval itself. Both the poleward and equatorward boundaries of the oval are important boundaries in space as well as in the upper atmosphere. Several statistical models exist to predict their locations, but instantaneous positions may still vary a lot. Experimentally, the oval can be imaged by high-altitude polar-orbiting satellites. However, at the moment, no such satellite is in operation. Several other local methods, e.g. utilising satellite particle or radar measurements, exist; specifically, the low-elevation EISCAT VHF radar measurement of electron temperature has been used for detecting the poleward boundary of the oval, which demarcates the polar cap (see e.g. the short summary in Aikio et al. 2006; Woodfield et al. 2010). Depending on the geographic location of EISCAT_3D and magnetic activity conditions, the radar could contribute to the detection of either of the boundaries. Ground-based networks of optical instruments are an important complement for these studies. Support for such measurements ideally requires low elevations to the north and south to maximise spatial coverage. Note that it was a requirement of the EISCAT_3D antenna and array design that the gain reduction should be as small as possible for elevations up to 60° off zenith. The report by Johansson et al. (2014) shows the gain performance that can be achieved for the designs under consideration.
The structure of increased F region electron density compared to the surrounding plasma is known as the tongue-of-ionisation (TOI), in which ionisation from sub-auroral latitudes on the dayside is drawn antisunward by the high-latitude plasma convection pattern towards the polar cap (Valladares et al. 1994; Pryse et al. 2009). At high F region altitudes, the lifetime of the plasma is sufficiently long for the ionisation to be drawn through the polar region and into the nightside sector, where it can sometimes be segmented into the polar cap patches which affect communications and position finding at high latitudes (see “Space weather and service applications”). In some cases, it has been observed that the tongue-of-ionisation forms the poleward wall of the main ionisation trough (Middleton et al. 2008). Foster et al. (2005a) utilised several IS radars and the SuperDARN HF radar network to draw a conclusion that the entire low-latitude, auroral, and polar-latitude regions were fundamentally coupled during the main phase of geomagnetic storms, creating a polar tongue of continuously streaming cold, dense plasma, along with oxygen ion outflows through the global convection pattern.
To study the generation mechanisms, evolution, and coupling between different latitude regions of these large-scale electron density structures, data from a global network of instruments are needed. Radio receivers using tomographic methods can provide electron density maps, usually in 2D, in the future more often also in 3D. Convection can be studied by HF and IS radar networks. Volumetric EISCAT_3D radar can provide very valuable contribution to these studies by measuring the 3D distribution of all plasma parameters and helping to solve problems related to in situ plasma production and loss. All the measurements should be combined with modelling efforts. At the moment, several numerical models of the upper atmosphere such as the Coupled Thermosphere-Ionosphere-Plasmasphere (CTIP) model (Fuller-Rowell et al. 1987) and the Utah State University time-dependent ionospheric model (Sojka et al. 1981) are available to model these persistent, large-scale features of the high-latitude ionosphere.
At high latitudes, the E region electron densities are often enhanced by auroral precipitation. Very large changes are caused by narrow layers known as sporadic E. Sporadic E (Es) layers are thin horizontal layers with a vertical extent of 0.5–5 km and densities at least two-three times higher than the background plasma. Their sources are metallic ions, formed by ablating meteors. Much of the progress in understanding high-latitude sporadic E comes from studies made with the EISCAT radars (see the review by Kirkwood and Nilsson 2000). An important generation mechanism for Es layers at mid-latitudes is the wind shear mechanism, but at high latitudes, the electric field mechanism, vertical convergence of ionospheric plasma by the magnetospheric electric field (Nygrén et al. 1984), becomes important.
Even though Es layers have been known a long time (initially they were identified from ionosonde recordings), their horizontal distribution is not well known. EISCAT_3D will play an important role in studying the horizontal distribution and evolution of these layers as well as the role of winds vs. electric fields in layer generation by utilising the multi-static multi-beam plasma velocity measurements.
Currents and energy input into the ionosphere
Large-scale eastward and westward electrojets flow within the auroral oval. Their intensity and extent is controlled by conditions in the near-Earth space, which are characterised by magnetic activity indices. In most of the modelling studies, it is assumed that all the horizontal currents in the ionosphere flow within an infinitely thin sheet at some fixed altitude (usually 110 km) above the ground. The thin sheet approximation simplifies the analysis, but it is not always a sufficiently accurate description of the ionosphere. In reality, the Pedersen and Hall conductivities maximise at different E region altitudes and hence also the respective Pedersen and Hall currents have different altitude profiles. To calculate the 3D currents in the ionosphere, we need to have a volumetric measurement of electron density and ion velocity vector. Real altitude-resolved ionospheric measurements provide the possibility to describe the vertical closure of current within the ionosphere and to investigate the inductive coupling between the currents. Indeed, model calculations have shown that the internal induction in the ionosphere may produce significant rotational electric fields (Vanhamäki et al. 2007). The induced electric field is important at local “hot spots”, reaching values 20–50 % of the potential electric field present at the same locations. Also, the induced FAC make a large contribution to the total field-aligned currents flowing between the ionosphere and magnetosphere. The effect of induction phenomena on magnetosphere-ionosphere coupling cannot be studied without volumetric vector measurements from the ionosphere, to be provided by EISCAT_3D.
The 3D structure of ionospheric currents is directly related to 3D Joule heating in the ionosphere. Recent estimates indicate that the polar ionospheres represent a major sink for the energy arriving inside the magnetosphere by the solar wind-magnetosphere coupling. The role of Joule heating has been estimated even as 50–60 % (Tanskanen et al. 2002; Ostgaard et al. 2002). The global particle heating has been estimated as 29 % by Ostgaard et al. (2002). Finally, the energy goes to the thermosphere and may affect thermospheric dynamics and vertical energy coupling in the atmosphere.
To evaluate the energy deposited in the 3D volume of the ionosphere, we need to have a volumetric measurement of electron density and ion velocity vector. Ion velocity vector measurement together with model ion-neutral collision frequency altitude profile can be used to calculate the 3D neutral winds in the E region (Heinselman and Nicolls 2008; Nygrén et al. 2011), which are needed in estimating Joule heating. With EISCAT_3D, it would possible for the first time to quantify the energy input in the form of Joule heating and particle precipitation on the spatial scales of auroral arcs. Joule heating may vary by >100 % on mesospatial (~60 km) scales (Kosch et al. 2011a). If small-scale structures (e.g. intense localised electric fields in the vicinity of auroral arcs) are totally absent from the models, this leads to potentially significant underestimation of Joule heating rates (e.g. Deng and Ridley 2007; Aikio and Selkälä 2009).
An important phenomenon of magnetosphere-ionosphere coupling is the formation of upwelling ion populations in the topside polar ionosphere. These upflows can represent a significant loss of atmospheric gases into interplanetary space and a significant source of magnetospheric plasma, which may also affect the dynamics of the magnetosphere (e.g. Yau and André 1997; Yau et al. 2007). Key processes for upward ion flows in the topside ionosphere are suggested to be frictional heating, ambipolar diffusion driven by a heated electron gas, and transverse ion acceleration produced by plasma waves. Artificially induced ion upwelling using the EISCAT heater demonstrates that ambipolar diffusion driven by the heated electron gas is a viable mechanism (Kosch et al. 2010). It is critical to determine the relative importance of the different mechanisms in operation and to understand the 3D distribution and composition of the upflowing ions and neutrals. Detailed knowledge of these processes is important for model predictions of what will happen to the composition and density of our atmosphere in the long-term future; for example, it could tell us whether the entire atmosphere will eventually evaporate and be lost into space.
There are several transition regions for upflowing ions, for example, from chemical to diffusion dominance at 500–800 km altitude, from subsonic to supersonic flow at 1000–2000 km altitude, and from collisional to collisionless at 1500–2500 km altitude. EISCAT_3D is one of the most suitable instruments to investigate such transitions because of its wider height coverage (up to about 2000 km) along the field line. EISCAT_3D will give information on the accurate thermal ion velocity and upward flux, whereas thermal ion detectors on satellites suffer from the effect of positive spacecraft charging.
Many existing models describe successfully only average conditions of the non-auroral, non-perturbed ionosphere, like the empirical global International Reference Ionosphere (IRI) model (Bilitza 2001). A number of physics-based models exist, too. The Global Ionosphere-Thermosphere Model (GITM) is a 3D physics-based model of the Earth’s thermosphere and ionosphere system (Ridley et al. 2006). GITM is coupled to a large number of models of the high-latitude ionospheric electrodynamics, for example, the assimilative mapping of ionospheric electrodynamics (AMIE) technique, and Weimer, Foster, Heppner, and Maynard or Ridley et al. electrodynamic potential patterns. Input parameters include the F10.7 index and solar wind parameters (e.g. Weimer 2005). The latitude resolution is 2.5°, and longitude resolution is 5° and output parameters include neutral, ion, and electron temperatures; neutral winds; neutral densities; and plasma velocities. Another model relevant to high-latitude electrodynamics is GUMICS, a global solar wind-magnetosphere-ionosphere coupling model. Its solar wind and magnetospheric part is based on solving the ideal MHD equations, and its ionosphere part is based on solving the electrostatic current continuity equation (Janhunen 1996). Model input are solar wind parameters and model output in the magnetosphere contain plasma density, pressure, velocity, and magnetic field vector in space and time, and in the ionosphere Pedersen and Hall conductances, ionospheric potential, ionospheric electric field, precipitation power, Joule heating rate, and field-aligned currents in space and time. The above-mentioned global models can be accessed by the aid of the Community Coordinated Modeling Center (CCMC) (http://ccmc.gsfc.nasa.gov/).
Global models have usually poor temporal and spatial resolution. To study the small-scale (tens of kilometres to sub-kilometres) structures that EISCAT_3D will be able to measure, more detailed models are needed. We review below some such models (TRANSCAR, IMM, and KIMIE), which have been developed in the ionospheric group at IRAP (Toulouse, France) in order to better understand the high-latitude ionosphere and its coupling with the magnetosphere and to compare with EISCAT radar data and numerical simulations. In the future, the models may be coupled together.
Two other important components of the model are the magnetospheric transport unit that makes the flux tubes convect (electric field and potential maps needed) and a neutral ionosphere unit (based on the MSIS-90 model) for the neutral-ion interactions mainly. Although TRANSCAR is not a self-consistent model, it is able to account for electrodynamic coupling between the magnetosphere and the ionosphere. Besides the knowledge of the neutral atmosphere, which can be adjusted from the MSIS-90 empirical model by calibrating the model during a quiet period (Blelly et al. 1996), it requires input parameters concerning the precipitating particles and the convection electric field. The precipitation can be given by serendipitous low-altitude satellite passes, while information about the convection can be inferred from HF radar observations (SuperDARN) or a combination of HF radars, magnetometers, and satellites (AMIE procedure). In the latter case, AMIE actually gives also the precipitation and the field-aligned currents. Lately, TRANSCAR was coupled with the IMM (Ionosphere-Magnetosphere Model described thereafter) which can also provide these necessary input parameters.
The plasma escapes from the flux tubes and precipitates in the ionosphere. This precipitation, mainly due to electrons, increases the conductivity of the ionosphere and generates the first coupling between the magnetosphere and the ionosphere.
Pressure gradients are created in the magnetosphere which induce electric currents flowing orthogonally to the magnetic field. These pressure gradients are mainly due to the ions, because their pressure is larger than the one of the electrons. The divergence of these orthogonal electric currents generates electric currents flowing along the magnetic field lines, the so-called field-aligned currents. They close in the ionosphere and induce electric currents flowing horizontally in the ionosphere. They correspond to a second coupling between the magnetosphere and the ionosphere.
From Ohm’s law, one can then compute the electric field in the ionosphere, which maps to the magnetosphere along the magnetic field lines which are assumed to be equipotential. This mapping modifies the initial electric field induced by the solar wind and requires that the modelling of magnetospheric plasma convection has to take account of the coupling between the magnetosphere and the ionosphere induced by the precipitation, the field-aligned currents, and the equipotentiality of the magnetic field lines.
As mentioned above, the coupling between IMM and TRANSCAR has provided several benefits: the IMM providing TRANSCAR with some necessary inputs like the convection electric field and the field-aligned current densities and TRANSCAR providing IMM with the ionospheric conductances. In turn, the coupling with IMM facilitates a better interaction between EISCAT_3D and models such as TRANSCAR.
KIMIE (KInetic Model of Ionospheric Electrons) is a 1D kinetic model developed by Garcia and Forme (2009). It describes the transport of electrons in a collisional and partly ionised plasma, including electron-electron, electron-ion, and electron-neutral collisions. Collisions between charged particles and between charges and neutral particles are treated differently. Electron-neutral collisions are binary and are described by the Monte Carlo method, while collisions between charged particles are long-range interactions, modelled by Fokker-Planck equations. This code was initially developed to study the kinetic effects due to strong current density in the Earth’s ionosphere. Its first results showed that very strong current densities result in non-Maxwellian distribution functions and that such currents are carried mainly by suprathermal electrons. These suprathermal electrons significantly modify the local conductivities and may carry very strong currents with parallel electric fields much lower than those predicted by the fluid theory.
EISCAT_3D model joint studies
A particular EISCAT_3D data set can be modelled and a close comparison can be made at any required temporal and spatial resolution.
Various physical processes can be tested on a synthetic or real event, by tuning the input parameters of the model.
Nowcasting and even forecasting of the physical parameters in a given ionospheric volume could in principle be performed, provided that sufficiently realistic inputs (solar extreme UV (EUV) flux, particle precipitation, and electric field essentially) can be supplied by real-time data or empirical models.
The resolution of the modelling far surpasses what can be observationally achieved by the present EISCAT system. EISCAT_3D’s spatial and temporal resolutions will make it possible to compare data and simulations at smaller scales, enabling a better understanding of the microphysical phenomena.
Although it is possible in principle to infer ion composition from incoherent scatter data, this is not done routinely for the present EISCAT systems. One problem is that ion composition effects on the incoherent scatter spectrum are to a large extent ambiguous with effects due to ion temperature. Multi-parameter fitting to recover both temperature and composition is possible but requires very low measurement errors in the amplitude comparison function ACF (autocorrelation function). For the present EISCAT radars, these ACF errors are basically determined by signal to noise ratio. The accuracy of EISCAT_3D measurements, however, will be limited only by the self-noise of the transmitter codes (Lehtinen et al. 2014). This, and the possibility to contain estimates from all of the EISCAT_3D sites, should facilitate much better composition measurements from EISCAT_3D.
With the tristatic EISCAT UHF system, it is possible to determine the three components of the electric field, but only at a single point. Having several simultaneous beams will be a huge improvement for, among other things, the determination of electric field vectors at several points in an ionospheric volume. EISCAT_3D will be able to measure electric field distributions in altitude and horizontally in latitude/longitude, which will be a great improvement for the study and modelling of electrodynamical phenomena, such as the ionospheric response to ULF waves.
Attempts to compare the present EISCAT data with predictions from TRANSCAR, IMM, and KIMIE are limited by a number of factors. These issues, which can all be resolved by EISCAT_3D, are the following:
The volumetric imaging capability of EISCAT_3D will also be extremely useful for coordinated observations with optical networks like ALIS (Auroral Large Imaging System, owned by the Swedish Institute of Space Research, Kiruna). ALIS is capable of providing 3D volume emission rates (VER) for several emission lines from a set of simultaneous optical images obtained from several stations located in northern Scandinavia. The typical time resolution is about 5–10 s. By inverting vertical profiles of the blue VER at 427.8 nm (N2+ 1NG) with tomography-like techniques, fluxes of precipitating electrons can be inferred in 2D from ALIS data, for example across and along an auroral arc. The current configuration of EISCAT only allows precipitating electron fluxes to be retrieved in one dimension, along the magnetic field line. EISCAT_3D will be able to produce 2D maps of electron fluxes and with a higher time resolution than currently provided by ALIS. These electron fluxes can be used as inputs for TRANSCAR/TRANS4 in order to reproduce either electron densities and temperature profiles obtained from EISCAT_3D measurements, or emission line profiles obtained with ALIS. Such flux measurements would also be very useful to test magnetosphere-ionosphere coupling models and could be compared to in situ data from a spacecraft crossing the same magnetic field line at higher altitude.
FMI electrodynamical models
In order to get an accurate picture of ionospheric electrodynamics, several different physical quantities need to be observed with good spatial and temporal resolution. This is most readily realised with large instrument networks, such as MIRACLE, which consists of magnetometers, all-sky cameras (ASC), and radars situated in northern Europe and operated and owned by the Finnish Meteorological Institute (FMI). Several other instruments that are not part of the MIRACLE network also operate in the same area (e.g. the EISCAT incoherent scatter radars and SuperDARN radars). The FMI group has developed a set of different analysis methods for solving the ionospheric electrodynamical parameters based on MIRACLE and supporting observations (e.g. Amm et al. 2003).
EISCAT_3D should cover an analysis volume of at least 300 km × 300 km × 50 km (altitude) and hence will cover the typical extent of mesoscale auroral forms for integration with magnetometer-based studies in connection with MIRACLE. The radar observations will need to cover the E region, in order to be able to estimate conductances. Spatial resolutions of at least 20 km × 20 km × 2 km (altitude), and temporal resolutions between 10 s and 1 min, are needed for integration with MIRACLE, but these will not be a problem for EISCAT_3D. The parameters that EISCAT_3D could provide as input into modelling, or which could be compared with model results, include electric fields and Hall and Pedersen conductivities. From those, horizontal currents could be calculated and vertical currents could be inferred from the divergence of the horizontal currents.
The Sodankylä Ion-Neutral Chemistry (SIC) model is a comprehensive 1D (in altitude) coupled model of the chemistry of the middle atmosphere, covering the mesosphere and lower thermosphere as well as the ionospheric D region. SIC has been developed by the SGO Aeronomy Group in close collaboration with the Finnish Meteorological Institute (Turunen et al. 1996).
The SIC model includes more than 400 reactions of positive and ions and neutral constituents. Sources of ionisation accounted for are solar EUV, X rays, protons, and electrons, as well as galactic cosmic rays. The altitude range is from 20 to 150 km and the typical time resolution is 5 min. Output parameters are ionisation and dissociation rates, electron density, ion composition, and odd oxygen, hydrogen, and nitrogen concentrations. SIC can be run either in a steady-state mode, which calculates the equilibrium concentrations of the modelled components, or in a time-dependent mode where the concentrations are advanced in time using the modified Euler method for stiff equations. The steady-state mode is suitable for estimating the effects of constant forcing during daytime, whereas the time-dependent mode allows us to study effects of diurnal variations or transient events, such as precipitation of energetic particles.
Continuous observations (long-term characterisation of EPP forcing)
Latitude-longitude imaging capability (spatial extent of EPP)
D region coverage (HOx/ozone region)
Plasma physics and active experiments
The geospace environment forms a superb natural laboratory for the study of plasma physics, affording a better vacuum than the best obtainable on Earth as well as a measuring volume uncontaminated by vessel geometries or edge effects. Since more than 99 % of the observable universe consists of plasma, passive observations and active experiments using the solar-terrestrial plasma provide a unique window on processes that are fundamental throughout the universe. Since the density and composition of the rarefied neutral atmosphere varies strongly as a function of height, the kind of plasma found in the upper atmosphere is also a strong function of altitude, ranging from charged dust/ice complexes in the mesosphere (see “Dynamical and chemical coupling in the mesosphere”), through plasmas dominated by molecular species and atomic oxygen in the upper ionosphere, to hydrogen-dominated plasmas at magnetospheric altitudes.
EISCAT_3D resolution and range extent requirements for the different science topics. A phased array system with fast pointing, multiple beams and calibrated signal is assumed
Parameter for which resolution is given
Temporal resolution (s)
Horizontal resolution (km)
Vertical resolution (km)
Height range (km)
Mesoscale electrodynamics and flows (including BBFs)
N e, T e, T i, V i
20 in the F region
Small-scale (auroral) dynamics
T e, T i, V i
Fine-scale auroral structures
N e, T e, T i
Ion outflow (natural and heater-induced)
N e, T e, T i, V i, ion comp.
NEIALs (aperture synthesis imaging)
0.05 at 300 km
N e, T e, T i, V i
Topside composition (O+, He+, H+)
mi (and N e, T e, T i, V i)
Transition region composition (NO+/O2 + vs. O+)
mi (and N e, T e, T i, V i)
High-energy particle events (SEPs, etc.)
T e, T i, V i
Atmosphere-ionosphere coupling (AGW, winds)
N e, T e, T i, V i, V n
0.1 or better
As low as possible—120 km
Mesosphere-stratosphere-troposphere (MST) small-scale dynamics
Vector neutral wind, N e
0.1 or better
As low as possible—110 km
D region phenomena
N e, T e (=T i) V i (=V n)
Raw data, Doppler velocity, spectral width
0.1 or better
Meteoroids and their effects on the background (Es, PMSE etc.), high-power mode
Raw data, polarisation matrix, and N e, T e, T i, V i
(30) 70–200 (1000)
Planets and asteroids
Raw data, power, polarisation matrix
N e, T e, T i, V i
Heating experiments, aperture synthesis imaging
Spectra (raw data)
IPP (~2 ms)
Space debris monitoring and satellite tracking
Raw data, power, Doppler velocity
Meteoroid monitoring (piggyback and low-power mode)
Raw data, polarisation matrix, and N e, T e, T i, V i
IPP ~100 ms for low-power mode
Down to 10 m
(30) 70–200 (1000)
EISCAT_3D radar coverage and location requirements for different science topics, together with suggestions for complementary instruments
Optimal location of radar
Number of beams; other requirements
Complementary ground-based instruments
Mesoscale electrodynamics and flows (including BBFs)
As wide as possible (30° elevation with all azimuths)
Within auroral oval
20 × 20; multi-static meas.
Magnetometers, optical equipment, tomography radio receivers, SuperDARN
Small-scale (auroral) dynamics
100 km in the F region, 33 km in the E region
Within the auroral oval
30 in N-S, 10 in E-W; Multi-static meas.
Optical equipment, rockets
Fine-scale auroral structures
5 km in the E region, within 10–20 km from magnetic zenith in the F region
Within the auroral oval
5–7 N-S, 1–7 E-W; multi-static meas., interferometric studies
Optical equipment, rockets
Ion outflow (natural and heater-induced)
~100 km curvature of field line
Within the auroral oval
N-S fan of 5–10 beams
Optical equipment, rockets
NEIALs (aperture synthesis imaging)
40 km × 40 km at 700 km
Within the auroral oval
Spreading the beam in the F-A direction; plasma lines ±6 MHz
Optical equipment, rockets
As wide as possible
Within the auroral oval
20 × 20
GPS scintillation measurements, rockets
Topside composition (O+, He+, H+)
N/A (field line tracing)
Fan, enough to cover field line curving
Optical equipment, rockets
Transition region composition (NO+/O2 + vs. O+)
One; heater ion-cyclotron freq. gives additional information
Optical equipment, rockets
High-energy particle events (SEPs, etc.)
As wide as possible
Oval and just equatorward of the oval
20 × 20
VLF, riometers, MF radar, satellites (POES, GOES, LANL, etc.), rockets
Atmosphere-ionosphere coupling (AGW, winds)
As wide as possible
Auroral oval and at the edge of the polar vortex
20 × 20
MST radar, MF radar, meteor radar, lidar, airglow imager, FPI, sounding rockets, heater (API)
Mesosphere-stratosphere-troposphere (MST) small-scale dynamics
As wide as possible
Location inside the polar winter vortex favourable for some questions
20 × 20 (M), one (ST); additional low-power TX mode, dual frequency (200–1000-kHz separation) for interferometric distance determination
MST radar, MF radar, meteor radar, lidar, airglow imager, sounding rockets, heater
D region phenomena
As wide as possible
Oval and just equatorward of the oval
20 × 20
Riometer, VLF, MF radar, rockets, heater
As wide as possible
20 × 20
MST radar, additional ISR at higher frequency, lidar, sounding rockets, heater
Meteoroids and their effects on the background (Es, PMSE, etc.), high-power mode
Fattened beam or multiple beams
Tracking mode (20 × 20 piggyback), fan for receiver beams, multi-static measurements for trajectory
Meteor radar, MST radar, optical networks
Planets and asteroids
Low elevation look direction to the south, at least 25°
As far south as possible
One; arbitrary polarisation TX and RX, hydrogen maser clocks
Other IS radars, optical instruments
Low elevation with all azimuths, particularly to the south
One; BW > 20 MHz, minimal RFI and ability to clip out individual narrow-frequency bands prior to integration over the bandwidth
Other radio receiver networks, including LOFAR and e-MERLIN
20° zenith angle
10 × 10
MST radar, airglow imager, FPI, sounding rockets
Heating experiments, aperture synthesis imaging
20° zenith angle
Fatten the beam or multiple beams (10 × 10)
MST radar, airglow imager, FPI, sounding rockets
Space debris monitoring and satellite tracking
25° elevation with all azimuths
North for satellite tracking
N/A; multi-static meas. for trajectory, multiple overlapping receiver beams for interferometric angle determination, dual freq. (200–1000-kHz separation) for interferometric distance determination
Meteoroid monitoring (piggyback and low-power mode)
Meteor radar, MST radar, optical networks
In the ionosphere, powerful radio waves can excite Langmuir turbulence and upper-hybrid resonance, raise the electron temperature greatly (up to 4000 K), and trigger ion upflow in the topside ionosphere (Kosch et al. 2010; Rietveld et al. 2003, and references therein). Critical for the efficiency of the heating is the angle that the HF pump wave vector makes with the geomagnetic field, but the reasons for this are not clear. Kosch et al. (2011b) found that adjusting the pointing direction of the radar by 1° resulted in a different observation, in which the ionospheric radio window in the bottomside ionosphere was observed at 7°–8° south of zenith, along with HF radio wave penetration to the topside ionosphere. The wavelength of the VHF radar is ideally suited to study Langmuir turbulence. Exceptionally bright optical emissions attributed to Langmuir turbulence were observed in self-focusing of the transmitted pump wave (Kosch et al. 2004). Artificial optical emissions are normally observed when upper-hybrid resonance is stimulated. It has been discovered, using the EISCAT heating facility, that the emissions depend strongly on the relationship between the pump frequency and the electron gyro-harmonics (Gustavsson et al. 2006; Kosch et al. 2002). The gyro-harmonics, in turn, depend on the magnetic field strength and the altitude in the ionosphere. The question arises of what electron acceleration mechanisms are at play in (what appears to be) a new non-linear regime.
One very interesting aspect of EISCAT_3D’s ability to support plasma turbulence experiments arises due to its capability for sub-beam width imaging, which will allow the small-scale density irregularities produced by the heating facility to be imaged for the first time. The size and distribution of these filaments and the way in which their properties evolve during pumping are not well known because existing radars do not have sufficient resolution to measure them; however, they are important to study, for example, because they affect satellite communications and navigation and because of the possibility that the density cavitations might play a role in electron acceleration. The temporal focusing of artificially induced optical emissions provides indirect evidence for this (Kosch et al. 2007). Last but not least, the evolution and self-organisation of the wide spectrum of spatial scales of the density filaments teach us about how plasmas dissipate energy flow in general. To date, only one experiment has detected a glimpse of the spatial organisation of the density filaments, obtained by in situ measurements with a rocket at the mid-latitude Arecibo facility (Kelley et al. 1995). This experiment indicated a most interesting organisation of the density structure, with a wide range of coupled spatial scales. The observed spatial scale down to below 10 m gives the resolution transverse to the geomagnetic field that should be aimed for with EISCAT_3D. However, the physics of the response of the ionospheric plasma as it is pumped by the powerful radio wave is likely to be significantly different at high auroral latitudes than at the mid-latitude Arecibo facility, because of the different geomagnetic field geometry; much more pump energy is dissipated through the formation of density filaments at high latitudes.
In addition to its use as a radar, EISCAT_3D has the possibility to act as a D region heater by focusing its power into a narrow beam. Although the frequency will be too high to stimulate ionospheric plasma resonances, the huge effective radiated power (100 s of GW) will make for an extremely effective ohmic heater of the ionospheric plasma, especially in the D region. Such capability would be invaluable in the study of dusty plasma, which occurs due to meteoric ablation in the mesosphere. The radar signature of dusty plasma (polar mesospheric summer/winter echoes) is modified by heating the surrounding plasma (e.g. Havnes et al. 2003; Kavanagh et al. 2006), allowing the dust properties such as grain size and charge to be inferred. Ionospheric studies of dusty plasma relate directly to astrophysical plasmas, which are also dusty, but also to climate change because the mere existence of radar echoes from dusty plasma is due to increasing mesospheric water content and cooling, both brought on by climate change (Olivero and Thomas 2001). Beam focusing can be used to cause ionisation and even breakdown in the atmosphere (stratosphere and mesosphere) and lower ionosphere. Such experiments have the potential to give information on a range of atmospheric properties and constituents that are not accessible by natural excitations. This would also allow ULF and VLF electrojet modulation experiments. Such low-frequency ULF and VLF transmissions open the possibility to study the ionospheric Alfvén resonator (Robinson et al. 2000) as well as cyclotron resonance interactions with radiation belt particles (Inan et al. 2004).
EISCAT_3D may also allow the flexibility to transmit different frequencies from different sections of the antenna array, allowing “beat frequency” experiments, where the heater frequency is provided by the beat frequency between the two transmissions. This would be an excellent technique to generate some of the very low frequencies presently inaccessible to the Tromsø heating facility. Another interesting property of EISCAT_3D is the possible use of phase and polarisation flexibility to create “twisted beams” carrying orbital angular momentum (Leyser et al. 2009), which can interact with angular momentum phenomena in the ionosphere. There are theoretical predictions of twisted beams of plasma waves, specifically of Langmuir waves (plasmons) and ion acoustic waves (phonons) (Mendonca et al. 2009a, b), and it has been suggested that such twisted wave groups can be excited in aurora. Twisted beams can also be used to detect small-scale plasma flows transverse to the beam that fit within the radar beam cross-section, such as vortices and sheared flows. To detect angular momentum effects of strong plasma flows in the ionosphere requires high degrees of beam twisting together with narrow beams (orbital angular momentum mode number of 10 or higher with a beam width of 1°).
At the bottom of the cascade linking large-scale and small-scale structures lies the whole area of plasma turbulence, whose understanding and description remain one of the most important unsolved problems in classical physics. Turbulent plasma comprises an array of structures covering a wide range of scale sizes and lifetimes, all of which are non-linearly created, coupled, and destroyed. In its turbulent state, plasma reaches a quasi-stationary point, which is, however, very far from thermodynamic equilibrium. The effects of plasma turbulence are extremely important; for example, turbulent diffusion and transport represent a fundamental limitation on the ability to confine energy within plasma.
An important but unexplored and difficult type of experiments are those that attempt interaction of the transmitted pump wave with natural (free) energy sources (Leyser and Wong 2009), including pump-induced Langmuir turbulence interacting with auroral electron precipitation or naturally enhanced ion acoustic waves. By seeding the ionosphere with Langmuir or ion acoustic waves during appropriate conditions of auroral electron precipitation, energy might be channeled into the plasma waves, which might open up for studying new non-linear regimes of plasma turbulence. Further, in such experiments, possible feedback of the ionospheric plasma turbulence on the larger scale system supplying the precipitation might be studied. Interferometric measurements are important to study the self-organisation of the turbulence in the pump-plasma interaction region, including the possibility of filamentation, which has been predicted theoretically for a long time.
Solar system research
Even though EISCAT_3D is designed to study the ionosphere and atmosphere of the Earth, it can also be used to study the properties of our solar system. Due to the high power and great accuracy, mapping of objects like the Moon and asteroids can be done. Material in the form of dust and meteors from our own solar system, and also from interstellar space, impacts the Earth’s atmosphere continuously. Because of their high power and large antenna aperture, incoherent scatter radars can be extraordinarily good monitors of extraterrestrial dust and its interaction with the atmosphere. It is very important to make good measurements of the flux of meteoric material entering the upper atmosphere, because meteoric dust plays an important role in the chemistry and heat balance of the middle atmosphere and thus forms a very important input into middle atmosphere models. In addition, the observations can contribute to work on solar system dust models (e.g. Mann 1995). Last, if wideband receiving capability is retained, the work utilising interplanetary scintillation can be continued to give information of the structures in the solar wind.
Meteoroids roam through the solar system with orbits of all inclinations. Meteoroids (interplanetary or interstellar debris) range in size from small asteroids with radii of ~10 km down to micrometeoroids with radii of ~0.1 mm and dust, radii of ~1 m. When a meteoroid enters the atmosphere, it is heated up and it loses mass due to ablation. The time duration of visible meteors is less than 1 s, and the main ablation takes place from 140 to 70 km. The radar target is provided by the coherent reflection from ionised plasma, and there are two types of echoes: meteor head and trail echoes. The head echoes are from a point-like source, moving with the meteoroids and relatively independent of aspect angle. Trail echoes come from the ionised trail, and the conventional low-power meteor radars (15–60 MHz) are able to detect only meteor trails through specular reflection. In the early 1990s, the EISCAT UHF became the first ISR system to be deliberately applied to the study of meteor head echoes (Pellinen-Wannberg and Wannberg 1994, Wannberg et al. 1996). Soon thereafter, all the world’s leading ISR facilities joined in.
EISCAT_3D has good potential to be a powerful instrument for studies of the effects of the meteor influx as well as the off-ecliptic component of the interstellar dust. At the VHF operating frequency of 233 MHz, event rates will be much higher than at 930 MHz, probably by more than an order of magnitude. The multi-beaming capability makes it possible to perform three or more tristatic observations at different heights simultaneously, which will increase the event rate further by a factor of 3 or more. Another beneficial effect of the lower operating frequency is that head echoes will become observable at up to 115-km altitude. This enables observing interstellar particles, which disintegrate at higher altitudes than particles on closed orbits due to their higher velocities.
The Canadian Meteor Orbit Radar (CMOR) survey (Brown et al. 2008), conducted between 2002 and 2008, measured the orbital parameters of 2.5 million meteors. This survey resulted in the detection and orbital characterisation of 109 major and minor meteor showers, 12 of which were previously unreported sources. The EISCAT_3D radar will have the potential to measure much more accurate orbital parameters for micrometeors, because its sensitivity will be of a different magnitude compared with the CMOR radar, making EISCAT_3D capable of measuring the orbits of smaller micrometeors at higher accuracy and providing new insight into a population that has not previously been measured continuously with good statistics. It is thus probable that the multi-static meteor head echo observations that will be conducted by EISCAT_3D will result in the detection of numerous new sources of meteors and thus provide valuable new insight into the formation, distribution, and evolution of dust within our solar system.
A recent study by Chau and Galindo (2008) showed that it is possible to distinguish parent sources for meteor head echoes measured with high-power large-aperture radar. This shows that it is feasible to utilise such radars for mapping the distribution of micrometeoroids within our solar system. Furthermore, a recent extensive study by Kero et al. (2011) using the MU radar has shown that it is possible to measure meteor head echo trajectories in an automated fashion and hence to construct a large catalogue of meteor orbits.
The total mass flux of meteors reaching the upper atmosphere is believed to deposit somewhere between 2 and 200 tonnes of material in Earth’s upper atmosphere daily (Murad and Williams 2002). The chemical composition and net mass of disintegrating meteors are important, since they are related to many physical and chemical phenomena such as polar mesospheric summer echoes and noctilucent clouds in the mesosphere as well as polar stratospheric clouds in the stratosphere. By applying simultaneous radar and optical imaging (multi-static video and spectral imagers), small-scale fragmentation and sudden breakup, in which locked populations of volatile chemicals are assumed to be released from the meteoroid body, could be studied in great detail. Narrowband optical instrumentation using emission filters could help to identify chemical compounds such as water (cf. the “water-Leonid” observations reported by Pellinen-Wannberg et al. 2004). Such observations would improve the mass flux estimates and also contribute to a better understanding of the physics governing the head echo process. Meteor head echo observations could be run in parallel with standard ionospheric mode, which would produce a semi-continuous meteor data set.
Planets and asteroids
Planetary radar is a field of research which involves using radars to study objects in our solar system. These include the Sun, planets and their moons, comets, and asteroids (Gordon 1958; Ostro 1993). The advantage of using a radar is the ability to control the signal that is used to illuminate the target. This allows measurements of various properties of targets through the use of time delay, polarisation and Doppler shift.
Planetary radar measurements can be used, among other things, to determine and refine orbital elements and spin vectors, to study surface and sub-surface composition, and to study the shape and topography of planetary objects (Kaasalainen and Lamberg 2006; Ostro 1993). Most planetary radar work has been conducted with Earth-based radar systems, such as Arecibo, Goldstone, and the VLA, but recently, space probes have also been used to conduct radar measurements of various targets, such as the Moon (Bussey and Mini-RF 2010), Venus (Pettengill et al. 1980; Saunders et al. 1990); and Mars (Picardi et al. 2005). Ground-based planetary radar measurements typically involve measuring the same and opposite circular returns of the backscatter to determine the surface reflectivity and roughness (Ostro 1993; Thompson 1978; Campbell et al. 2007). Because the targets are typically far away, the spatial resolution is obtained by combining rotational Doppler shift and time of delay. The resulting range-Doppler or delay-Doppler images of the targets are not completely unambiguous, as several different parts of a rotating object can result in identical Doppler shift and round-trip delay.
Planetary radar measurements conducted with high-power large-aperture radars have resulted in a wealth of new information about solar system bodies (Campbell 2002). Measurements mainly conducted with the Arecibo Observatory radar (Ostro 1993) have provided new information about several planets and a large number of asteroidal bodies. A high-power large-aperture radar is also a valuable tool in accurately measuring the orbital parameters of potentially hazardous near-Earth objects. Radar measurements can also provide information about the shape and composition of these objects.
The main advantage of the EISCAT_3D system will be its complementary location compared with the US radars. This will allow opportunistic measurements of near-Earth objects that happen to pass Earth on our side of the planet, i.e. if the US planetary radars cannot measure a near-Earth object passing Earth at closest approach, the EISCAT_3D system will be able to do this with a large probability. Radar measurements provide complementary information about the range and non-convex shape of these objects, which can be compared with optical measurements (Kaasalainen and Lamberg 2006). An example of such a situation was the close approach of 2012 DA14, which passed Earth with a distance of only 26,000 km in January 2013. It was not possible to measure this asteroid with the US planetary radars at closest approach, but the existing set of EISCAT radars, located in northern Fennoscandia, secured some good observations.
The EISCAT_3D radar will also use a complementary frequency compared with the US planetary radars. The Arecibo Observatory radar, which can use either 450 MHz or 3 GHz, is at much higher frequency than the 233-MHz frequency planned for the EISCAT_3D radar. While the lower frequency results in a smaller sensitivity for measuring near-Earth asteroids, it provides larger ground penetration and thus allows better sub-surface probing capabilities, allowing an improved measurement of the composition of planetary targets.
The downside of the high-latitude location of EISCAT is that many of the planetary sources are at low elevation (20°–30°), significantly restricting the available sources that can be measured. This also poses a conflicting requirement for antenna sensitivity compared with ionospheric plasma incoherent scatter radar measurements. As mentioned in “Structures and boundaries in the ionosphere”, the EISCAT_3D design is a compromise, recognising that most EISCAT_3D measurements will be made at higher elevations, but choosing an antenna and array design which preserves a reasonable antenna gain down to elevations below 30° (Johansson et al. 2014).
Interplanetary scintillation from the solar wind
The amplitude of a radio signal from a compact astronomical radio source, passing through the inner heliosphere, is modulated by the motion of solar wind plasma irregularities across the line of sight. This modulation, which may be observed with a suitable radio telescope, is termed interplanetary scintillation (IPS). It is produced by variations in solar wind density (and thus the refractive index) and subsequent interference. The turbulent-scale density irregularities in solar wind can be used as flow tracers—assuming that their velocity is closely related to that of the background solar wind (e.g. Hewish 1989). Simultaneous measurements by two antennas show similar patterns of scintillation, and the time lag for maximum cross-correlation gives an estimate for the solar wind outflow speed. Increasing the baseline between the antennas helps to resolve the presence of multiple solar wind streams which can be located in the same line of sight. As the baseline rotates relative to the solar wind outflow, estimates of the direction of flow can be made. The existing Kiruna and Sodankylä UHF receivers have been used to carry out a series of world-leading observations of scintillating structures in the solar wind showing, among other things, how rapidly the solar wind is accelerated within a short distance after leaving the Sun, and how streams of different speeds can interact to produce complex solar wind structures (e.g. Bisi et al. 2010; Dorrian et al. 2010).
Since the solar wind structures (CMEs, CIRs) carry the enhanced fluxes of momentum and energy that drive geomagnetic activity, IPS measurements are potentially an important space weather activity that can help to predict the onset of geomagnetic activity (Hapgood and Harrison 1994). The advantage of IPS measurements over in situ measurements by satellites is their very good spatial coverage, since the solar wind can be observed at any latitude and observations can also cover a wide range of distances from the Sun. The temporal resolution is, however, often worse than in satellite measurements. Use of several arrays and frequencies would give improved coverage of the inner heliosphere, reducing seasonal variations in that coverage and offering a better possibility for cross-comparison to identify sources of interference and improve statistics. During the operating lifetime of EISCAT_3D, a number of other systems such as LOFAR and SKA will be available, with the potential to make complementary solar wind observations, allowing EISCAT_3D the possibility to play a role in a wide international coordination.
The data product needed for IPS is total power, integrated over a wide frequency band and sampled at >50 Hz. The required receiver bandwidth must be equal to or larger than 20 MHz and contain minimal radio frequency interference (RFI). In order to facilitate this science, EISCAT_3D should also have the ability to clip out individual narrow-frequency bands prior to integration over the bandwidth. The required elevation angles are low (down to 5°), at all azimuths.
Space weather and service applications
Over the last decade, a vibrant international community has grown up around the study of space weather, focusing on the study of how varying conditions in geospace affect human activity (e.g. Baker 1998, 2002; Echer et al. 2005; Bothmer and Daglis 2007). Space weather has a wide variety of impacts. For example, solar-terrestrial disturbances can produce significant changes in the density of the ionosphere, particularly in the high-latitude regions, while electric fields can cause structuring of the ionospheric density into irregularities on a wide range of spatial and temporal scales. These density structures have serious impacts on radio propagation, both for trans-ionospheric signals from global positioning satellites (e.g. Mitchell et al. 2005) and for ground-to-ground or ground-to-air communications reflected from the ionosphere (e.g. Wilink et al. 1999). Processes that heat the thermosphere-ionosphere system lead to the expansion of the neutral upper atmosphere, enhancing the thermospheric density at high altitudes and increasing satellite drag. Events such as coronal mass ejections (CMEs) and magnetospheric sub-storms increase the flux of high-energy particles, which can damage spacecraft electronics and increase the radiation exposure of astronauts, airline passengers, and air crew. These phenomena hence have profound consequences for the multi-billion dollar aerospace and space technology sector (e.g. Feynman and Gabriel 2000; Pirjola et al. 2005). In addition, auroral ionospheric currents can affect infrastructure on the ground, by inducing current flow in systems such as power grids and pipelines. There is thus strong interest from a variety of industrial sectors in understanding and predicting space weather, so that its effects can be mitigated. The ability to predict space weather events requires highly capable models, able to assimilate data from a diverse global network of continuously observing instruments (e.g. Vassiliades 2000; Wehrenpfenning et al. 2001). Although incoherent scatter radars, such as EISCAT_3D, are few in number, the power and versatility of their measurement technique means that they can measure parameters which cannot be obtained in any other way. EISCAT_3D will thus be one of the key cornerstones in the international endeavour to measure and predict space weather effects.
Space weather effects on high-latitude ionospheric irregularities
A major effect of space weather on the ionosphere is the ability of solar-terrestrial processes to modulate and structure electron density. The term “ionospheric irregularities” indicates structures which are different from the ambient ionosphere in electron density, either much higher or much lower. Their scale size can range from centimetres to hundreds of kilometres. Irregularities can appear in a specific region or can be created over wide areas by global-scale processes such as magnetic storms. They can occur on all timescales from seconds up to a few days. While shorter timescale processes are always present to some extent, they can be greatly enhanced under specific space weather conditions. Space weather particularly affects the high-latitude regions, but can also act to produce density changes, waves, winds, and electric fields on a global scale. In order to understand the formation of irregularities, it is necessary to measure all of the processes responsible for their formation, including density gradients, particle precipitation, ExB drifts, and thermospheric winds (Belehaki et al. 2009).
Irregularities in the high-latitude region may result from patches of plasma density, large-scale plasma blobs, and density troughs, whose steep edges are unstable, so that smaller scale density structures develop along these edges. These smaller scale irregularities cause intense scintillation effects. Individual patches of irregularities have lifetimes of 2–3 h; however, irregularities are seen to persist for periods of up to 8 h. These irregularities are not specifically related to space weather disturbances but do increase with the solar activity cycle.
At high latitudes within the auroral oval and cusp, precipitating energetic particles produce enhanced electron densities. The fluxes of precipitating particles are very structured in space and time and create irregular structures in the ionosphere. These types of irregularities are very variable in space and time during space weather disturbances.
When intense scintillation occurs, the integrity of Global Navigation Satellite Systems (GNSS) such as GPS, Glonass, and Galileo can be jeopardised. Under extreme conditions, this corruption leads to the loss of satellite lock and the total failure of global positioning, as occasionally happened during the last solar cycle (e.g. Basu et al. 2001; Webb and Allen 2004; Mitchell et al. 2005; Foster et al. 2005b). Since so many aspects of the global economy now depend on GNSS, the understanding of their vulnerabilities and the development of risk-mitigating countermeasures constitute key challenges (Fisher and Kunches 2011).
Current studies of irregularities frequently utilise the ground-based reception of GNSS signals to derive scintillation climatologies (e.g. Spogli et al. 2009; Alfonsi et al. 2011; Prikryl et al. 2011). In polar regions, however, the density of GNSS receivers is sparse and supplementary observations from other instruments are needed, not only to improve the climatology but also to investigate the physical processes behind irregularity formation.
Scintillation effects occur at all latitudes, but particularly at the equator as well as at high and polar latitudes (Aarons 1982; Mitchell et al. 2005), making northern Scandinavia an ideal location for studying the formation and evolution of the scintillation-producing irregularities and the effects that they can have. In order to improve the characterisation of ionospheric irregularities, two types of EISCAT_3D observations will be needed. Campaign-based observations will specify the real-time distribution and short-term variations of irregularities in the high-latitude region, while long-term monitoring is essential to build climatologies of recurrent features in their dynamics and temporal evolution (Alfonsi et al. 2011). A complete understanding of irregularities can only be achieved on the basis of continuous and systematic ionospheric monitoring, able to describe the temporal changes of the plasma on long timescales (months, years, decades) as well as on short timescales (minutes, hours, days) with a wide spatial coverage (hundreds of kilometres). Such observations would be a superb complement to the monitoring data already available from other instruments (Altadil et al. 2009). Because of its ability to measure continuously over long periods and to image the ionosphere over wide spatial scales, EISCAT_3D will play a critical role in providing these measurements in the European high-latitude sector, thus providing new insight into processes that lead to irregularity formation.
Although we have focused so far on the creation of ionospheric irregularities and their effect on satellite signals, it should be noted that the same space weather processes which produce strong density structures in the high-latitude ionosphere also severely affect the propagation of radio signals at all frequencies from ELF to VHF, including commercial radio broadcasts and ground-to-ground and ground-to-air communications. Reflections from sharp density gradients, such as auroral boundaries or trough walls, can introduce large multi-path delays to received signals, while fast plasma drifts in the ionosphere can give rise to spectral spreading and Doppler shifts in radio signals. The most severe of all are the impacts caused by geomagnetic storms and sub-storms, which can radically affect the density distribution of the ionosphere and can completely inhibit radio propagation, since signals can be completely absorbed in the lower ionosphere or can propagate straight out into space without being reflected (e.g. Blagoveschensky and Borisova, 2000; Hunsucker and Hargreaves 2002). As a result, there is a wide community of potential users needing reliable forecasts of the radio propagation environment in the high-latitude region, where models are notoriously unreliable. The wide coverage area and continuous operation of EISCAT_3D will make it an invaluable resource for users of the radio spectrum who need to constrain model predictions with real data (see “Space weather impacts on technology”).
Space weather effects on the high-latitude ionosphere-thermosphere
Space weather can also have very significant effects on the neutral atmosphere, especially at high latitudes. As noted above, some of the most significant processes are associated with geomagnetic storms, because such events can last several days and have global effects. During storms and sub-storms, large amounts of energy are injected into the polar upper atmosphere in the form of electric currents, accelerated particles, and Poynting flux. The sudden heating of the upper atmosphere can change its composition and chemistry, which in turn feed back into changes in the density and structure of the ionosphere. Some of the energy entering the polar atmosphere can also affect the neutral winds, changing the circulation of the upper atmosphere. In addition, storm and sub-storm effects generate a whole spectrum of atmospheric gravity waves, which in turn produce travelling ionospheric disturbances (TIDs).
TIDs correspond to perturbations of the ionised gas associated with the passage of internal atmospheric gravity waves. They can give rise to horizontal gradients in electron density, and, in this respect, their effects are similar to those of ionospheric irregularities. A rich variety of publications has addressed the subject of TIDs (see review by Hocke and Schlegel 1996). The neutral wind and the Earth’s magnetic field seem to be the main geophysical factors governing the structure and dynamics of TID disturbances, although the physical mechanisms underpinning their relationship are still not entirely understood (Afraimovich et al. 1999).
As well as the effect of thermospheric chemistry and heat balance on the ionosphere, and the ability of thermospheric waves to produce ionospheric structure through TIDs, there are two other major space weather effects involving the thermosphere, both of which rely on the ability of space weather process to modulate the electric currents which flow naturally in the ionosphere, especially in the high-latitude region.
The ability of the ionosphere to carry electric currents depends on the fact that the ionosphere is embedded in the neutral thermosphere. The differential motion of ions and electrons under the action of magnetospheric electric field gives rise to electric currents flowing horizontally in the E region of the upper atmosphere. The collisional interaction between ions and neutrals acts to heat both species, a process which is conventionally referred to as Joule heating. Joule heating dissipates magnetospheric electromagnetic energy in the upper atmosphere. The effect of the heating is that the neutral upper atmosphere expands outward, so that the density of the high-altitude thermosphere increases during periods of strong Joule heating.
A significant effect of E region currents is that their rapid variations are able to cause induced currents in conductive systems on the Earth’s surface, such as electricity distribution grids and oil pipelines. Currents induced by space weather effects can be a significant problem for certain technological sectors, and these are discussed in “Space weather impacts on technology”.
The role of EISCAT_3D in investigating these phenomena will be to provide underpinning data to help constrain and validate the models which are used in this area. We briefly discuss more of these models in “Modelling and forecasting of space weather”. EISCAT_3D will also play an important role in supporting current and future spacecraft missions designed to investigate the space weather effects arising from ionospheric currents. One such mission is ESA’s 3-satellite SWARM mission, launched in November 2013 and with a nominal lifetime of 4 years, initially at altitudes of 460 and 530 km. The main objective of the SWARM mission is to provide the best ever survey of the geomagnetic field and its temporal evolution. The geomagnetic field is made up of both internal and external components. The internal field arises from the magnetism of the Earth’s core, the crust, and the oceans. The external component arises from space weather processes, in particular from ionospheric currents. In order to separate the internal and external contributions, the three SWARM satellites carry instruments to obtain unique new data of unprecedented resolution and accuracy for the global ionospheric science community.
The SWARM instrumentation allows the estimation of electric currents and fields, ion and electron densities, and temperatures. From these, further parameters like the electromagnetic power (Poynting flux), electron cooling rates, etc. can be derived. The satellites’ acceleration indicates neutral density as well as cross-track winds. Predecessors of the SWARM satellites, particularly CHAMP, Dynamics Explorer, and the DMSP series, have, in the past few years, already established the existence of relatively small-scale but strong density variations in the thermosphere (Lühr et al. 2004) and enhancements of the Poynting flux at high latitudes (Knipp et al. 2011).
The causes of these variations are not yet well understood. However, it is clear that they originate with the space plasma processes which heat and force the upper atmosphere. In terms of absolute magnitude, this takes predominantly place in the lower thermosphere and E region, well below the altitudes where satellites can orbit. These height regions are, however, well covered by incoherent scatter radars. Thus, only a combination of SWARM satellites and EISCAT_3D radar can deliver the measurements that allow us to understand magnetosphere-ionosphere-thermosphere coupling more fully. Previously, it has been difficult to separate spatial from temporal variations and to assign the proper scale sizes to these. In the near future, this will be possible, thanks to the volumetric imaging capability of EISCAT_3D and the multi-satellite nature of the SWARM mission.
There is currently a growing interest worldwide in the development of fleets of nano-satellites or “cubesats” (size 10 × 10 × 10 cm). As an example, the QB50 network (led by von Karman Institute, Belgium) will comprise a set of 50 cubesats built by university teams and research institutes worldwide that will be launched together in early 2016 into a circular orbit at 320 km altitude with an inclination of 79°. The duration of the mission is expected to be between 6 weeks and 3 months depending on solar activity. The objectives of QB50 are to explore in situ the low thermosphere and to study the atmospheric re-entry process.
Half of the cubesats of the QB50 mission will have a multi-needle Langmuir probe (mNLP), developed at the University of Oslo (Bekkeng et al. 2010). The instrument is able to measure small-scale (down to tens of meters) density variations that result from the complex magnetosphere-ionosphere interaction. For a good understanding of the physical processes, supplementary data are needed. These include simultaneous measurements from other spacecraft (both in low and high Earth orbits) on roughly the same field line, the EISCAT_3D radar data, or ALIS data (ionospheric optical tomography). QB50 Langmuir probe data and EISCAT_3D data could be used for cross-validation at 320 km. EISCAT_3D will also provide the overall ionospheric context in which the mNLP data should be interpreted. The goal would be to try to identify in what situations density variations could be expected at the satellite altitude.
Space weather impacts on technology
In “Space weather effects on high-latitude ionospheric irregularities”, we already looked at the impacts of space weather on radio propagation and global positioning systems. In this section, we look at geomagnetically induced currents, already mentioned in “Space weather effects on the high-latitude ionosphere-thermosphere”, and at the effects of energetic particles.
The forecasting of GIC is increasingly recognised as an important priority for Europe, and improved forecasting techniques will be demonstrated within the FP7 EURISGIC project, during the period 2011–2014 (Viljanen 2011). The US solar shield method (Pulkkinen et al. 2010) is already in use in North America, and its output will be extended to the European region. The GUMICS-4 simulation of the Finnish Meteorological Institute (Janhunen et al. 2012) will also be enhanced to make it suitable for forecasting purposes.
The role of EISCAT_3D in GIC research would be to provide the data needed for a comprehensive analysis of ionospheric electrodynamics based on solar wind-magnetosphere-ionosphere simulations. Although the primary driver of GIC events is the solar wind, the conditions in the ionosphere play a decisive role. From the viewpoint of GIC, understanding the temporal and spatial (3D) behaviour of ionospheric currents on scales of seconds and a few tens of kilometres would be extremely valuable. The combination of ground magnetic field recordings and ionospheric electric field recordings by EISCAT_3D will provide the tools needed to reach this goal.
The Earth’s radiation environment comprises energetic particles trapped in the radiation belts and magnetosphere, those generated by solar energetic particle (SEP) events, and galactic cosmic rays (GCRs). Of these different populations, the most highly variable, and consequently the most difficult to anticipate, is the SEP population. This is also the population that can often cause the most damaging effects (Zank 2012). At cruise altitudes of commercial aviation, both SEPs and GCRs pose threats through single-event upsets in critical electronics and through exposure of crew and passengers to radiation (Dyer et al. 2003; Barnard et al. 2011). The gravity of the consequences for biological structures depends on the energy of the particles responsible (Bottollier-Depois et al. 2003). Radiation effects are especially significant for polar flights, because the cosmic radiation particle flux increases with increasing latitude and altitude, being significantly higher on board aircraft than at ground level; however, the complexity of the radiation field does not make dose measurements easy. Indeed, the particles encountered vary considerably, and a wide range of energies and types of particle are found.
Radiation standards for air crew are based on past experience, and there are no regulations concerning passenger exposure. Allowed radiation limits on the ground vary between nations. The International Commission on Radiological Protection (ICRP) recommends a 20-mSv limit for the annual exposure of occupational radiation workers and a 1-mSv annual limit for the public and prenatal exposure (Wrixon 2008; Mertens et al. 2010). Dosages during a flight depend on the path, duration, and altitude as well as on the level of solar activity. For example, Mertens et al. (2010) found that a commercial 8‐h polar flight during the 2003 “Halloween” SEP event would have given 0.7 mSv. Models such as QARM (Lei et al. 2006) show that a round trip of two such flights during the recent solar minimum gave a GCR dose of order 0.2 mSv, while an equivalent trip during the largest known SEP event, the “Carrington event” of 1859 (Shea et al. 2006; Hapgood 2011), would have given 20 mSv. Estimates vary, but from studies of smaller events, the direct and knock‐on (loss of service, etc.) costs of a Carrington‐scale event have been estimated at $1–2 trillion and full recovery would take 4–10 years (Odenwald et al. 2006).
Although EISCAT_3D is unlikely to measure directly the most energetic particles which penetrate into the lower atmosphere, EISCAT_3D data will still contribute to energetic particle studies by providing measurements to validate ionisation models for lower energy precipitation into the middle atmosphere, where EISCAT observations are possible. In addition to the validation of models, climatologies of energetic particle data, derived from EISCAT_3D measurements, will be examined to assess whether they can be extrapolated to obtain useful predictions e.g. to help facilitate the planning of safe aircraft routes.
Modelling and forecasting of space weather
“Ionospheric modelling” has already discussed some of the models used to describe the state of the magnetosphere-ionosphere/thermosphere system, and given some details of how EISCAT_3D can be used to verify and constrain such models. It should be noted here that the space weather community makes use of a specific set of models, devoted to the prediction of ionospheric and geospace conditions. In general, these models tend to be empirical or semi-empirical in nature, since purely physics-based models are of limited use in operational settings (e.g. Mikhailov et al. 2007). For example, the radio propagation community makes considerable use of empirical models such as the global IRI, or the European COST-PRIME and COST-PROF family of models, which describe the average conditions of the unperturbed, sub-auroral ionosphere (Bilitza 1992; Bradley 1995; Hanbaba 1995; Zolesi and Cander 2004).
Forecasting of ionospheric conditions, e.g. for the coming 24 h, is of considerable importance for a variety of communication, positioning, and frequency management tasks, especially during disturbed space weather conditions. However, accurate forecasting remains a challenging problem, due to the wide variety of potential forcing mechanisms and the diversity of their possible effects. One of the fundamental problems is the lack of data on the statistical variability of, and the interrelationship between, different effects such as sporadic E, spread F, blobs and patches, irregularity formation, and changes in the height profile of electron density. The construction of better forecast models remains the subject of a broad international effort, but this relies on strong underpinning science driven by more complete and better coordinated sets of long-term observational data.
While it is not impossible that pure physics-based modelling could eventually provide reliable space weather predictions, given increased understanding and development, a better approach for operational use in the short term is in the development of assimilative models (e.g. Schunk et al. 2004; McNamara et al. 2007; Angling 2008), in which real-time data are used to describe global conditions and to constrain models which seek to predict the future evolution of the system over a relatively short period. In this respect, the situation is similar to meteorology—while we cannot predict the weather from first principles, we can forecast quite successfully for a limited period by accurately measuring the current conditions and using physical models to extrapolate the short-term evolution of the weather and climate system.
For the determination of current space weather conditions and their impact on the ionosphere, real-time specification is usually preferable to modelling. The problem with specification, however, is that it relies on the assimilation of real-time observations which are often very sparse, meaning that underlying theoretical constraints are needed, for example to regularise the observation grid. Certain types of observation themselves need to be supplemented by modelling. For example, one of the most widely available observing techniques is ground-based vertical-incidence HF sounding; but this technique cannot provide any information on the shape of the topside ionospheric profile, and models based on the ionospheric-scale height are used to provide this information (e.g. Reinisch et al. 2001a; Belehaki and Kersley 2006). In addition, during very disturbed conditions, the signal is absorbed in the ionosphere. Observing techniques including incoherent scatter radars (Farley 1996) like EISCAT_3D, sounding data from satellites (Reinisch et al. 2001b), ionospheric tomography (Leitinger 1996), or radio occultation measurements (Jakowski 2005) can be used to obtain the missing information.
Both modelling and real-time specification are particularly challenging at high latitudes, where the ionosphere tends to be considerably more structured. In principle, this implies the need to assimilate a greater density of observations; however, the distribution of ground-based observing instruments is often the most sparse at the highest latitudes, putting a greater premium on the assimilation of satellite data, e.g. from Langmuir probes and radio occultation techniques, or data derived from GPS tomography.
One of the primary goals of the space weather community is to secure an improved set of real-time and historical data on which to base specification and empirical modelling. This implies not only the deployment of more observing instruments but also better international collaboration to maximise data availability and improve data exchange (Stanislawska and Belehaki 2009). A variety of organisations have responsibility for the management of data relevant to space weather, including ESA, EUMETSAT, Intermagnet, ISES, COST, DIAS, and the World Data Centres. The present EISCAT data, as well as the future EISCAT_3D data, will be highly relevant to this challenge, implying a requirement for better methods of disseminating and assimilating EISCAT data.
Many of the concepts described above are captured in a recent proposal to develop a common framework covering all the main types of observing systems for monitoring near-Earth space, together with the current generation of models. The development of such a system, known as the “Geospace Array” (Lind 2011), has recently been summarised in a white paper to NASA. It calls for a combination of globally distributed small-scale and medium-scale instruments, supported by facility-class instruments such as EISCAT_3D, all of which contribute data to a “Geospace Assimilation Grid” which in turn provides data to a range of search engines, virtual observatories, and space weather models. The users of these products would include not just the space weather and atmospheric science communities but also the education sector and the general public.
The wide-scale coverage and continuous operational capability of EISCAT_3D will make it a superb tool for specification of the high-latitude European sector and for the provision of data to initialise and constrain forecast models, with the potential ability to provide detailed real-time ionospheric maps of a region some hundreds of thousands of cubic kilometres in extent. EISCAT_3D is complementary to other instruments, since while tomographic techniques, for example, can provide a wide-scale context, EISCAT_3D can provide the detailed multi-parameter data to help explain why a particular phenomenon is happening, not just where it occurs. Collaborations have already been established with the leading ionospheric tomography project in the Scandinavian sector (TOMOSCAND, Vierinen et al. 2010), and the practical details of how the interaction between the two projects will proceed are already under active consideration.
As well as providing the basic underpinning data needed to generate and validate space weather models, EISCAT_3D will have the capability to reconfigure its operations to respond to changing space weather conditions. The use of “intelligent scheduling” (see “Observing techniques and measurement philosophies”) will enable the radar to initiate special experiment modes in response to particular space weather events, such as solar flares, magnetic impulses, or sudden storm commencements. This capability will overcome a fundamental limitation of the present EISCAT radars which, because they are not operated continuously, often fail to observe the very dynamic conditions which occur at the start of such events, whose effects are of particular interest for the space weather community.
Europe has recently begun making efforts to establish a space situational awareness (SSA) programme, under the aegis of the European Space Agency. This programme is designed to provide an independent capability for monitoring spacecraft and the growing amount of “space debris”, ranging from large objects, such as dead satellites, to the millions of sub-centimetre fragments in Earth orbit (Klinkrad and Jehn 1992; Klinkrad 2006). While space debris poses no immediate danger to most humans, there is a severe risk to satellites and space missions operating in low Earth orbit, which provide many useful services to society.
Currently, there are approximately a million objects larger than 1 cm in orbit. Any of these objects would be likely to cause serious damage in the case of a collision with an operational satellite. The situation is made worse by the so-called Kessler syndrome (Kessler and Cour-Palais 1978), a modelling result that predicts that the current orbital debris will collide with other orbital objects, creating ever more small debris and further increasing the risk of orbital fragmentation events. This collisional cascade could potentially render many of the low Earth orbital regimes unusable in the next 100 years if no active measures are taken.
Space debris monitoring has three main goals: firstly, to identify and monitor the most significant objects and debris clouds and characterise their orbits; secondly, to validate the current models of how the space debris population is evolving over time, for example monitoring the dispersal rates of debris clouds and quantifying the tendency of debris populations to cascade into progressively smaller fragments (Rossi et al. 1998); and thirdly, to measure how the locations and orbital parameters of the space debris population are modified by specific space weather events, such as geomagnetic storms, which can perturb their motions or cause them to de-orbit through increases in thermospheric drag.
One of the most effective and cost-effective active measures that can be taken is the so-called orbital collision avoidance manoeuvre. In order to reduce the number of these manoeuvres and minimise the amount of fuel required to perform them, accurate orbital elements of centimetre-scale orbital debris are needed. EISCAT is currently building a capability for measuring orbital elements of space objects, with several successful campaigns conducted in the recent years in collaboration with ESA. However, the slowly moving, single-beam nature of the current EISCAT radars makes it difficult to track spacecraft or debris objects.
The design of EISCAT_3D enables it to overcome many of the limitations inherent in monitoring space debris with dish-based radars. Its wide spatial coverage and capability to generate multiple, rapidly moving beams will enable EISCAT_3D to track individual objects, including multiple objects simultaneously, for an optimal characterisation of their orbital parameters and the monitoring of orbit perturbations. The EISCAT_3D radar will therefore be able to provide the high-accuracy measurements required for orbit determination, and it is probable that such measurements can be “piggybacked” onto normal incoherent scatter measurements, with relatively sparsely spaced dedicated tracking pulses aimed at further refining the measurement of orbital elements. Satellite tracking and space debris measurements in EISCAT_3D will also benefit from some of the other new system capabilities, including the use of aperture synthesis imaging techniques to improve the resolution of sub-beam width-sized hard targets.
The sensitivity of the proposed EISCAT_3D system in both cases is comparable to the existing UHF radar. Based on these assumptions, the EISCAT_3D system will be capable of detecting objects with 1.5–2-cm diameter at a distance of 1000 km. There are currently very few space surveillance radar systems capable of routinely tracking such small-sized objects, although new capabilities are being built around the world. EISCAT_3D would thus be a very valuable asset for the global space surveillance network, providing orbital element measurements of small but potentially harmful objects, which could be used to reduce the risk of collisions between space objects and orbiting spacecraft.
The high-latitude location of the EISCAT_3D radar has pros and cons. The biggest disadvantage is that the radar will not be able to measure objects with low inclinations, as these will never fly over the radar. However, most of the orbital debris is in high-inclination Sun-synchronous orbits, which means that it will pass over EISCAT_3D. Due to this fact, the density of orbital debris is higher at high latitudes, meaning that EISCAT_3D will be able to observe more debris per unit volume than radars located in more southern locations. This gives EISCAT_3D the potential to conduct orbital parameter surveys of space objects at a faster rate than radars at more southerly locations.
Radar techniques and new methods for coding and analysis
Over the 30-year period for which the EISCAT facilities have been in operation, one of their key contributions to the field of upper atmospheric science has been in the development of new observing techniques to improve the quality, time resolution, and spatial resolution of the radar measurements. EISCAT has always been a test bed for new ideas in coding and data analysis, whose user community has pioneered many novel applications, including new coding strategies (e.g. Virtanen et al. 2009; Lehtinen et al. 1998, 2008), new types of data analysis (e.g. Lehtinen and Huuskonen 1996; Virtanen et al. 2008), and other applications of fundamental mathematical and statistical theory to experiment design and data taking (e.g. Vallinkoski and Lehtinen 1991). Many of these new techniques, first developed at EISCAT, are now in standard use among incoherent scatter radars worldwide.
EISCAT_3D represents a further substantial step in the design of atmospheric radars. The system will be the first of a new generation of software radars (e.g. Grydeland et al. 2005a), whose advanced capabilities will be realised not by its hardware (which is relatively inexpensive and modular) but by the flexibility and adaptability of the scheduling, beam forming, signal processing, and analysis software used to control the radar and process its data. In this respect, EISCAT_3D will be a world leader in the development of new observing techniques, which will eventually be implemented by the next generation of incoherent scatter radars around the world. The use of EISCAT_3D to test innovative radar techniques aimed at major advances in resolution, measurement speed, coverage, occupancy, consistency, and responsiveness is needed not just to increase the scientific output of the facility itself but to position the whole international radar community to move forward over the coming years.
EISCAT_3D is designed to provide a high-power, high-gain aperture, combining fully digital element technology with a wide receiver bandwidth over a large number of simultaneous, adaptive, and independent receiver beams. The system will be able to carry out large-scale volumetric imaging of the upper atmosphere, while also providing high-resolution images to probe small-scale targets beyond the reach of existing radars. In addition, EISCAT_3D will have the ability to conduct a number of different experiments simultaneously, not only for conventional incoherent scatter radar applications but also for carrying out passive radar applications over multiple regions of frequency space and undertaking generic monitoring functions for applications such as space weather and space situational awareness.
Phased arrays (such as EISCAT_3D) offer many additional degrees of freedom compared to conventional dish-based radars. Among others, these include the possibilities for modularising the radar array, for imaging applications (Grydeland et al. 2005b); post-beam forming (e.g. Hansen 2009), for example to produce multiple receiver beams within the volume of a single transmitter beam; aperture tapering to achieve finely tuned control of the beam shape; and array coding to generate twisted beams (Tamburini et al. 2012). The necessity to develop an entirely new transmitter system for EISCAT_3D makes it possible to include further additional capabilities, such as the possibility to handle amplitude modulation and higher resolution phase and polarisation control, which are not practical in the current EISCAT radars.
In order to achieve these aims, considerable amounts of computing power will need to be devoted to the signal processing and analysis of the EISCAT_3D data (Mann et al. 2013). Because the low-level EISCAT_3D data will be very large, some of this capability will need to be deployed at the radar sites and will be devoted to data decimation, data combination, short-term storage, and event detection. Many of these functions will have to be automated, since the volume of data is so large as to be beyond the ability of a human operator to interpret them in real time. Because of this, it is also desirable to store data at the lowest level possible for a limited period, so that decisions made automatically can be revised in the light of later reconsideration, for example if interesting events are found to develop from initially unpromising conditions.
The remainder of the EISCAT_3D storage and computing capabilities will be provided off-site, utilising the power of supercomputing and archiving centres in the various participating countries. These centres will provide the Web-based remote control, data visualisation, and experiment design capabilities required for the operation of EISCAT_3D, as well as the intelligent technology that will make it possible for the radar to respond adaptively to changing conditions, e.g. by changing its aperture characteristics, look directions, coding schemes, and data recording rate.
The following sub-sections discuss some specific applications which, while impossible with the current generation of EISCAT radars, will form a fundamental part of the observing capabilities of EISCAT_3D. In each of these applications, EISCAT_3D will serve as a “pathfinder” instrument, where new techniques will be developed into standard observing applications for implementation in the next generation of software radars.
Observing techniques and measurement philosophies
Because EISCAT_3D is a very different type of radar to the existing EISCAT systems, and has considerably more flexibility, it opens the possibility for a radical re-appraisal of the principles under which such radars should be operated in future. The major novel techniques opened up by the new facility are as follows:
One of the most important requirements for this application is to find an intelligent way to balance the trade-offs between coverage area, observation density, and time resolution in constructing a volumetric image. An interesting aspect of this is that the optimum imaging strategy is highly condition dependent, since the scattering cross-section is dependent on the density of the ionosphere and is likely to be significantly more variable than might be the case for weather radar. Another issue will be the existence of ionospheric structure at various different scales, depending on time, location, and magnetic activity level, which determines the density at which the volumetric image should be sampled. This means that the optimum imaging strategy will need to be varied in real time during experiments as conditions change, and strategies for doing this appropriately will need to be evolved. In certain circumstances, there will be contradictory demands, for example if the ionosphere has low density and a high degree of structure, such that potentially no volumetric imaging strategy will be able to adequately represent it. The chosen approach to volumetric imaging is a complex problem, which not only involves a trade-off between scan speed and measuring volume but also involves trade-offs between parameters such as transmitter power and beam shape (see below). The task of developing an automated approach to the handling of volumetric imaging, balancing time integration and spatial resolution in an optimal way, will be crucial for the next generation of imaging upper atmospheric radars and one in which EISCAT_3D will have a path-finding role to play (Wannberg et al. 2010).
Post-acquisition beam forming is a critical technique on the receiver side of the system, needed to ensure that the volumes illuminated by the radar transmitter are being appropriately measured. In the context of a multi-element array, the challenge is mainly in the computation and data handling capacity required to ensure that enough receiver beams are generated to map the full extent of each transmitter beam, with required range resolution. As with volumetric imaging, changes in conditions will imply changes in the required resolution, especially if the ionosphere changes from a relatively quiet state to one having a high degree of horizontal and vertical structure. This type of change is very likely at the auroral latitudes where EISCAT_3D will operate. Another circumstance requiring an adaptive approach to beam forming would be the need to study a particular region of interest as it propagates through an observing region illuminated by a known transmitter pattern. It is worth re-iterating that, in contrast to the changes in volumetric imaging philosophy discussed above, these changes in beam forming strategy can be achieved simply by data post-processing. The challenge is equivalent to an inversion problem in which the measured set of all samples from every radar antenna is inverted in an optimal way to recover the large-scale structure of the scattering ionosphere, subject to certain constraints on temporal and spatial resolution imposed by the measurement strategy. EISCAT users already have considerable experience with the application of inverse problems to radar experimentation, and the use of inversion techniques to produce optimal estimates of wide-scale ionospheric structure through beam forming is likely to represent a significant contribution to the future generation of ionospheric phased array radars, which is well matched to the community’s existing capabilities.
Aperture synthesis imaging radar
Beam and phase front shaping
The possibility to use shaped phase fronts will be of particular interest when using the large EISCAT_3D aperture in the near field, i.e. for lower atmosphere measurements. At these altitudes, the phase fronts emanating from a dish antenna of equivalent size to the EISCAT_3D array would be highly non-planar, making it complicated to interpret the instantaneous signal received from a broad, distributed, horizontally stratified target such as the atmosphere. As long as the beam shape and the physics of the scattering process are known, of course, any such scattering problem can be handled by inversion techniques, but the ability to conduct adaptive beam shaping to reduce the degree of non-planarity in the radar phase fronts can simplify the problem by reducing the need for computationally intensive inversion. The ability to control phase front shape may thus be important in the plans to use EISCAT_3D for meteorological applications. Although tropospheric and lower stratospheric studies are not the main purpose of the radar, this is expected to be a scientifically interesting application which opens the radar up to a wider user community.
Event identification and object tracking
One of the significant improvements which EISCAT_3D will bring over the existing EISCAT radars is the ability to track moving objects, which has been impossible with the current generation of large, slowly scanning dishes. Such objects can be natural, such as plasma blobs, troughs, flow channels, and aurora, which need to be followed so that their evolution can be observed, or man-made objects, such as space debris, which need to be tracked so that their orbital parameters can be calculated.
Adaptive interleaved experiments
It is implicit in many of the above sections that EISCAT_3D will radically redefine the experimental philosophy of incoherent scatter radars. In contrast to the current situation, where the radar runs a single experiment at a time, the new generation of phased array radars will be able to share their duty cycle between a number of different modes, whose operations will be interleaved. For example, although the radar might devote a substantial proportion of its duty cycle to a pre-defined mode of ionospheric observation, a fraction of its observing time could be simultaneously devoted to other applications such as space debris, while some of its receiver beams could be used for radio astronomy observations, e.g. for solar wind studies via interplanetary scintillation.
A major issue, which will drive the development of techniques for all phased array radars of this type, is the question of how these interleaved experiments should change as conditions alter. This question has many aspects: not only how the experimental modes themselves should change, in terms of beam direction, modulation scheme, or transmitted power, but also how the division of observing time should be re-assigned between competing applications, how the computing resources should be re-distributed between different kinds of data processing, and, perhaps most importantly, the identification of what circumstances would trigger such changes in the observational philosophy.
EISCAT_3D will have a capacity to serve scientists and science in a better way than the present EISCAT has by enabling a more flexible radar scheduling system. While it will still be possible to assign time in advance to pre-defined modes, there will be considerable emphasis on a condition-dependent response to changing conditions. This requires the development of a strong set of criteria specifying what conditions would trigger a change of mode, or what class of phenomenon would require an interruption of “normal” observations, or a significant re-distribution of resources, in order to make detailed observations of its development. One method of achieving this, which should be pioneered using EISCAT_3D, is to make a very strong connection between data and models, with radar (and other) data being assimilated to models in real time and used to predict the future development of the geophysical processes which, in turn, will trigger new modes of observation. This will need considerable development effort, since both the modelling and the assimilation infrastructure are not currently at the level where they can fully support such a system, and there is clear potential for wrong decisions to be made, if the predictions are not good enough to be up to the challenge.
The whole field of adaptive experiments and intelligent scheduling is a significant area of study in itself, with considerations potentially extending beyond pure science into issues such as logistics and economics. It encapsulates the challenge of how to derive the maximum benefit from a multi-faceted resource, which not only can be represented in terms of transmitter and computing power but also needs to be evaluated in terms of its scientific and technical benefit.
Many of these issues, which are fundamental to the operation of EISCAT_3D, are studied in the Handbook of Measurement Principles which is being produced as an output of Work Package 6 on Performance Specification (Lehtinen et al. 2014). The handbook makes a first-principles introduction to the fundamental underpinnings of phased array observations, and discusses the various trade-offs which apply in the case of each measurement strategy. These will form the basis for a first definition of the operating modes of the new radar, and will feature heavily in the succeeding generations of the Performance Specification Documents, which will be the other major outputs from Work Package 6.
Radar coding and data analysis methods
One of the most prominent contributions which the EISCAT community has made over the whole 30-year operation of the facilities has been the development of new methods of coding and data analysis to optimise the scientific return from the radars. These include the operational development of techniques such as the flexible re-use of radar samples in correlation (the GEN system, Turunen 1986), the use of modulations based on Walsh codes (alternating codes, e.g. Häggström et al. 1989, Wannberg 1993, Lehtinen et al. 1998), and analysis based on the principles of statistical inverse theory (GUSDAP, Huuskonen and Lehtinen 1996; Lehtinen and Huuskonen 1996). Many of these techniques are in use, not only at EISCAT but also elsewhere in the worldwide network of incoherent scatter radars.
The development of new techniques has, however, now reached the point at which some of the newly designed experiments cannot be tested operationally at EISCAT, given the limitations of the current EISCAT hardware, though they have been tested elsewhere (e.g. Virtanen et al. 2013). For example, the work on polyphase codes, exploring how additional degrees of freedom can be opened up by the control of the transmitted polarisation to levels of polarisation change less than 180°, cannot be exploited because the current EISCAT transmitters are not capable of the required phase control. In addition, the use of amplitude modulation in EISCAT coding, which has been extensively studied by the Finnish EISCAT user community, cannot be implemented in practice because the present transmitter exciters are not capable of the required amplitude control. These limitations will not exist in EISCAT_3D, for which the transmitter is being designed not only to be sufficiently flexible to transmit all of the coding strategies which have so far been devised by the EISCAT community, but also to accommodate the next round of coding developments anticipated during the coming years.
Although probing for ionospheric signatures of orbital angular momentum is not the main justification for EISCAT_3D, the technology can in principle be deployed easily on the new radar, and the novelty value of an actual demonstrated detection makes it well worthwhile to plan for this kind of experiment to be included in the repertoire of EISCAT_3D.
This paper is a revised version of Deliverable 3.6 of the EISCAT_3D Preparatory Phase Study, funded by the European Union as part of its Seventh Framework Programme. The project deliverable version can be found online at the EISCAT_3D website, at https://www.eiscat3d.se/content/deliverable-36-final-version-eiscat3d-science-case.
The intent of the science case document has been to set out a broad scope of achievable science aims, without going into great detail on any one topic in particular. In doing so, it offers a basis for users in each potential EISCAT_3D member country to accentuate particular science areas for their own national funding applications, which should be geared to their own research strengths.
The authors wish to recognise the contributions of the European Union’s Seventh Framework programme, which supported the meetings of the working groups and funded the time of the convenors to construct the science case document. We would also like to thank the staff of the EISCAT Scientific Association for their assistance and support. In particular, we express our appreciation to Stephan Buchert and his colleagues at IRF Uppsala, for hosting the annual series of EISCAT_3D User Meetings, which provided the venue for several of our working group discussions and were a rich source of ideas and discussions. In developing the science case, we have sought to reach out to researchers from both within and outside the current member countries of EISCAT. As well as participants from Norway, Sweden, Finland, Japan, and the UK, we are pleased to acknowledge the contributions of our colleagues from Belgium, France, Germany, Italy, and Poland. Their experience and expertise have helped considerably to strengthen this document.
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