Magnetosphere-Ionosphere Coupling (Physics and Chemistry in Space)

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Would you like to tell us about a lower price? If you are a seller for this product, would you like to suggest updates through seller support? In the past two decades a succession of direct observations by satellites, and of extensive computer simulations, has led to the realization that the polar ionosphere plays a principal role in large-scale magnetospheric processes - a manifestation of the physics linkage involved in solar-terrestrial interactions.

Now the challenge is to comprehend the vast amount of complicated measurements made in this magnetosphere-ionosphere sysstem of the Earth. This book addresses the electrical coupling between the hot, but dilute, magnetospheric plasma and the cold, but dense, plasma in the ionosphere. In five major chapters, this book presents: Read more Read less.

Here's how restrictions apply. Physics and Chemistry in Space Book 23 Paperback: Springer; edition June 12, Language: Be the first to review this item Amazon Best Sellers Rank: Start reading Magnetosphere-Ionosphere Coupling on your Kindle in under a minute. Don't have a Kindle? Current and future programs and interagency activities provide context.

NSF also supports the AMPERE project, which utilizes the engineering magnetometers aboard the Iridium communications network to resolve field-aligned magnetospheric currents in the auroral zone. The range of intellectually stimulating science questions that arise within the purview of atmosphere-ionosphere-magnetosphere interactions is enormous.

However, there are a subset whose connections to the needs of a 21st-century society make them compelling; it is on this basis that the panel defined the science challenges articulated in this section. Moreover, they also form an integral part of the key science goals see Chapter 1 that this solar and space physics decadal survey has set forth as its prime agenda. Before proceeding, it is useful to consider the ionosphere-thermosphere from a systems perspective and to describe what aspects of the system behavior need to be understood in order to advance toward a predictive capability.

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First, it must be understood how energy and momentum inputs from the magnetosphere are spatially and temporally distributed in the polar and auroral regions, and how the global IT system responds to these inputs. Equally important, it must be understood how energy and momentum are transferred from the lower atmosphere into the IT system, and what this means in terms of IT spatial and temporal variability.

Key to the above, it must further be understood how internal processes transform and transfer energy and momentum within the system, regulate responses to external forcing, and control the formation of regional and local structures in both neutral and ionized constituents. The consequences of two-way interactions between the IT system and the magnetosphere must also be considered. In this context, it must be understood how the high-latitude IT system moderates the transfer of energy from the solar wind and magnetosphere and how the inner magnetosphere and plasmasphere interact with the mid-latitude ionosphere and drive its variability.

Achieving the above level of understanding is a multidecade task. The AIMI panel has, however, narrowed the scope of aspirations to five AIMI science goals that have the potential to be comprehensively addressed with current technologies or those under development, and within the decade. These are enumerated in Figure 8. In addition, Figure 8.

Finally, the following section sets forth a prioritized set of strategies to address these challenges. Global Behavior of the Ionosphere-Thermosphere. How does the IT system respond to, and regulate, magnetospheric forcing over global, regional, and local scales? At high latitudes, the AIM system directly impacts magnetospheric dynamics through conductivity changes, current closure, and ion outflow.

Spatially confined energy input from the magnetosphere can quickly be redistributed to the ionized and neutral gases over much larger scales. A response of the system can occur at locations well removed from the input. Determination of changes in the system that are imposed externally and changes resulting from the internal system response is required to understand the geo-effectiveness of the interaction of the planet with the solar wind. In other words, the ionosphere-thermosphere system both adjusts to the varying input from above, and also feeds back and regulates this exchange.

Inter-hemispheric differences address the asymmetric closure of currents, as well as local ionospheric structuring and electric fields. Indeed, the dissimilarities present in the simultaneously measured magnetic.

The compelling science questions that researchers must answer are these: Differences in ionospheric conductivity play an important role in the closure of magnetospheric currents and may have a profound influence on magnetospheric current closure, as the ionosphere and magnetosphere interact to regulate the response of geospace to solar wind input. How does such a varying, spatially structured environment feed back on and modify field-aligned current and electric potential patterns imposed from the magnetosphere?

High-latitude heating mainly below km causes N 2 -rich air to upwell, and strong winds driven by this heating transport N 2 equatorward, which then mixes with ambient O in unknown ways Figure 8. IT constituents are controlled by gravity, diffusion, chemical reactions, and bulk transport. It is essential to understand how these processes determine global responses in O and N 2 after heating occurs at high latitudes.

Since these disturbances are superimposed on a solar EUV-driven circulation system that is mainly ordered in a geographic coordinate frame that varies with local time and season, the interactions can be complex, and IT responses are very different depending on prevailing conditions. The relative abundances of O and N 2 are fundamental to understanding local plasma densities and total mass densities, both of which are key parameters underlying space weather forecast needs.

The question then remains, How do winds, temperature, and chemical constituents interact to produce the observed global neutral and plasma density responses of the IT system? Since the B field plays a major role in controlling the distribution of ionospheric plasma, and since ion-neutral collisions can serve to decelerate or accelerate the neutral gas, the ionospheric plasma can in many ways regulate the IT response to magnetospheric forcing.

This occurs mainly through the redistribu-. This picture varies considerably from day to day, but is available only at a single local time on any given day. Without coincident global measurements of neutral winds, temperature, and total mass density and some measure of localized heating, the causes and consequences of this composition variability cannot be ascertained. The Geospace Dynamics Constellation mission, described below in this chapter, will enable researchers to understand the relationships between these variables and, moreover, will provide this information simultaneously as a function of local time in a single day.

For instance, in connection with a sudden storm commencement, eastward penetrating electric fields can lift the equatorial ionosphere and accelerate the neutral gas through removal of the drag effect of the ions. A similar effect can occur at middle latitudes when equatorward winds push the plasma up magnetic field lines, lessening the drag on the zonal winds.

Large redistributions of plasma occur as the result of subauroral electric fields that couple the inner magnetosphere and plasmasphere to the mid-latitude ionosphere Figure 8. Disturbance winds below km generate electric fields through the dynamo mechanism, which then redistribute plasma that affects the wind system at higher altitudes. As discussed below, there are also tidal-driven electric fields that redistribute plasma as a function of local time, longitude, and season and that modify the interaction between the plasma and neutral components of the IT system.

Magnetosphere-Ionosphere Coupling in the Solar System

The key question is, How do plasma and neutrals interact to produce the observed response of the IT system, including hemispheric and longitudinal asymmetries? At high latitudes the IT system and the magnetosphere are engaged in a two-way interaction with each other. Energetic particles from the magnetosphere ionize the upper atmosphere, creating complex conductive pathways that regulate the flow of current from the magnetosphere. Electric fields guide the flow of. These signatures are believed to be connected to plasmasphere erosion and driven by subauroral electric fields from the inner magnetosphere.

Strong plasma density gradients are observed over North America, the details of which could be observed by a network of ground-based observatories. Spatial and temporal evolution of the global structure would be well observed by a constellation of satellites making in situ measurements. Foster, Space weather impacts of the subauroral polarization stream, Radio Science Bulletin The peak altitude of Joule heating in turn determines the response time of the global thermosphere to this energy input.

Energetic particles also initiate a chemical pathway to create nitric oxide, which regulates the response and recovery of the neutral atmosphere through radiative cooling. Local heating of the IT system and ionospheric flows from lower latitudes see Figure 8. The interactions and feedbacks that occur between energy deposition, dynamics, radiative cooling, energetic particles, electric fields, and plasma and neutral constituents and temperatures are how the global IT system regulates its response to magnetospheric forcing, and how it also regulates the response of the magnetosphere to solar wind forcing.

The AIMI panel concluded that a major goal of the coming decade, therefore, is to understand how regulation of the IT system occurs, and how connectivity between multiple scales arises within this regulation process.

Making the required coincident multi-parameter measurements of the system over local, regional, and global scales poses major challenges in terms of observational strategies. Strategies that employ an optimal combination of ground-based, suborbital and space-based platforms involving innovative in situ and remote-sensing instrumentation will be required. Meteorological Driving of the IT System. Numerous observational and modeling studies conducted since the decadal survey have unequivocally revealed that the IT system owes much of its longitudinal, local-time, seasonal-latitudinal, and day-to-day variability to meteorological processes in the troposphere and stratosphere.

The primary mechanism through which energy and momentum are transferred from the lower atmosphere to the upper atmosphere and ionosphere is through the generation and propagation of waves Figure 8. Owing to rotation of the planet, periodic absorption of solar radiation in local time LT and longitude e.

Surface topography and unstable shear flows arising due to solar forcing excite planetary waves PWs and gravity waves GWs extending from planetary to very small approximately tens to hundreds of kilometers spatial scales and periods ranging from 2 to 20 days down to minutes. The absorption of solar radiation at the surface and the subsequent release of latent heat of evaporation in convective clouds radiate additional thermal tides, GWs, and other classes of waves.

Those waves that propagate vertically grow exponentially with height into the more rarified atmosphere, ultimately achieving large amplitudes. Some parts of the wave spectrum achieve convective instability, spawning additional waves or turbulence. Other parts of the wave spectrum are ultimately dissipated by molecular diffusion in the to km-height region, and some fraction of those waves penetrate all the way to the base of the exosphere ca. Along the way, nonlinear interactions between different wave types occur, modifying the interacting waves and giving rise to secondary waves.

Finally, the IT wind perturbations. See text for details. Courtesy of Jeffrey M. Although the presence and importance of waves are without dispute, the relevant coupling processes operating within the neutral atmosphere, and between the neutral atmosphere and ionosphere, involve a host of multiscale dynamics that are not understood at present.

The connection between tropical convection and modification of the ionosphere described above is just one example of emergent behavior that typifies the coupling between the lower atmosphere and the IT system. Below, the panel presents its analysis of what are the most pressing science questions that must be addressed on this topic in the coming decade, particularly with respect to developing a capability to predict the space weather of the IT system.

A first and fundamental question is, How does the global wave spectrum evolve temporally and spatially in the thermosphere? The maxima in longitude are believed to result from electric fields generated by longitude-dependent atmospheric tides in the dynamo region, with possible contributions from associated composition variations and possibly in situ north-south winds.

However, no electric field, wind, or composition measurements were available to understand the interplay between these quantities that results in the displayed structure. Satellite-based measurements are urgently needed to resolve this and many other similar issues in IT science. Oberheide, Intra-annual variability of the low-latitude ionosphere due to nonmigrating tides, Geophysical Research Letters Copyright American Geophysical Union. Reproduced by permission of American Geophysical Union.

What are needed are observations between about and km that include the critical dynamo region where electric fields are generated, and that would, moreover, make it possible to answer the question, How does the mean thermosphere state respond to wave forcing? Observations of both the mean state and of the waves are required to elucidate how the waves dissipate, how they relate to the background flow and thermal structure, and how their effects can be parametrized in general circulation models. It is important to measure the tidal PWs, and GWs together, to be able to understand the interactions between them.

For instance, PWs do not penetrate much above km, but instead are thought to impose their periodicities on the IT system by modulating the tidal and GW parts of the spectrum that do penetrate to higher altitudes. This raises the following questions: How are GWs modulated by PWs and tides, and do they effectively map these structures to higher altitudes? As one example, recent measurements reveal the fascinating result that stratospheric warmings significantly alter the state of the IT system: The electric field subsequently redistributes ionospheric plasma, dramatically changing TEC gradients that are known to degrade communications and navigation systems.

This emergent behavior in the system, once completely understood, has the potential to dramatically improve ionospheric predictions. Top Exosphere temperatures, ranging from 97 K maroon to K red. The diurnal tidal spectrum evolves with height, with the larger-scale waves penetrating to km, while the shorter-scale waves are absorbed at intervening altitudes, giving up their energy and momentum to the mean atmosphere. Researchers know very little about how the tidal, planetary wave, and gravity wave spectra evolve with height and modify the mean thermal and dynamical structure of the thermosphere.

Oberheide, Surface-exosphere coupling due to thermal tides, Geophysical Research Letters In addition, first-principles modeling predicts a thermospheric warming in response to the stratospheric warmings, and resulting changes in thermospheric winds and density that impact satellite drag. The above wave-plasma interactions focus on electric fields generated by the dynamo mechanism, but one must ask: Recent studies, in fact, show that winds associated with tides that.

Variations in composition also accompany tidal dynamics, thereby introducing chemical influences on ionospheric production and loss with large effects in scale and magnitude. Finally, breaking gravity waves are thought to provide the turbulent mixing at the base of the thermosphere ca. How does the turbopause vary in space and time, and what are the causes and consequences? Gravity waves have often been cited as the source for small-scale plasma variability, but the absence of coordinated observations of neutral waves and ionospheric perturbations in the right altitude regions has greatly impeded progress.

One hypothesis suggests that the interaction between in situ gravity waves and the steep bottom-side plasma gradient of the post-sunset equatorial ionosphere generates alternating east and west electric fields that can excite this instability. Another theory requires gravity-wave winds only in the E region, which generate electric fields that couple to the F layer.

In addition, the tidal and mean wind fields modulate the accessibility of gravity waves to these ionosphere regions, and moreover contribute to instability onset and suppression criteria, and to instability growth rates. Thus, the interactions between small, local, and regional-scale plasma-neutral coupling phenomena are all involved in this complex but highly relevant emergent behavior in the system. Resolving this problem requires high-resolution measurements of neutral and plasma parameters with high spatial and temporal resolution over the to km height region, and further development of the relevant theories and models.

Finally, lightning is known to generate low-frequency electromagnetic waves called whistlers, which can induce precipitation of radiation belt particles into the opposite hemisphere and enhance lower ionosphere densities there. Lightning events also accelerate electrons to very high energies and create strong electric fields in the mesosphere. Gamma-ray flashes observed from space e. Luminous optical manifestations of these events are referred to variously as sprites, elves, or blue jets Figure 8.

All of these processes raise questions about chemical modification of the mesosphere and electrodynamic coupling between the troposphere, the ionosphere, and all of geospace through these energetic lightning events. The AIMI panel concluded that a major goal of the coming decade is to understand how tropospheric weather drives space weather.

How do high-latitude electromagnetic energy and particle flows impact the geospace system? What are the origins of plasma and neutral populations within geospace? The IT-magnetosphere interaction at high latitudes is catalyzed by convective flows, which transport and mix plasma and neutral gases across subauroral, auroral, and polar regions, and by magnetic field-aligned flows of plasma and electromagnetic energy, which couple the collisionless magnetosphere to the collisional ionosphere-thermosphere boundary layer. Researchers now recognize that the active response.

Effects on the upper atmosphere and ionosphere of transient electric fields, electromagnetic waves, and high-energy electrons produced by these events remain unknown. Reprinted by permission from Macmillan Publishers Ltd: Electric jets, Nature Determining the processes that control this coupling is critical in understanding geospace dynamics and for development of accurate predictive capabilities. Knowledge of auroral acceleration processes and of auroral electrodynamics derived from satellite missions such as FAST, POLAR, and IMAGE is now fairly mature, but placing these processes in the context of IT-magnetosphere system dynamics is forcing the need to confront larger-scope questions: How is electromagnetic energy converted to particle energy?

What controls the conversion rates and the spatial-temporal distributions of Joule heating, particle precipitation, and ionospheric outflows at high latitudes? How do these distributions and their spatial gradients, combined with neutral-wind feedback, regulate ionosphere-thermosphere-magnetosphere dynamics? Answering these questions over the next decade will require combining model results with new multipoint in situ and remote-sensing measurements.

The relationships are shown schematically in Figure 8. Measurements at two or more points along magnetic flux tubes in the collisionless region above the topside ionosphere will be required to determine the mechanisms through which electromagnetic energy is converted to particle energy, and their rates; conjugate measurements at lower altitudes are essential for determining the impacts of precipitating and outflowing particles on the ionosphere and thermosphere and, in turn, the influence of the resulting IT activity on the source populations of outflowing ions and on the development of gradients for example, in conductivity that moderate electrical current flow and electro-.

Researchers lack firm empirical knowledge of the relative importance of the inferred processes, all of which occur in the ionosphere. The observed correlations from FAST satellite data suggest causal relationships, but determining causality among these processes requires, at a minimum, two-point measurements along magnetic flux tubes.

Elphic, Factors controlling ionospheric outflows as observed at intermediate altitudes, Journal of Geophysical Research Modified by permission of American Geophysical Union. Combining optical measurements with in situ measurements is needed to provide contextual information, in particular, how locally inferred acceleration processes influence, and are influenced by, larger-scale structure and dynamics. The synthesis required to connect these measurements with solar wind and magnetospheric drivers will require development and application of increasingly realistic models for global and regional dynamics.

Without the photo-ionization present in the dayside ionosphere, the nightside ionosphere is susceptible to structuring and modulation by variable fluxes of charged particles precipitating from the magnetosphere. Gradients in the resulting ionization cause ionospheric currents to be diverted into field-aligned currents. Recent studies have revealed the unexpected possibility that the accompanying ionospheric flow structures are mirrored in the plasma sheet by the formation of fast flow channels and by steep plasma pressure gradients in the outer ring current. These ionospheric flow structures form at steep gradients in ionospheric conductivity, which remains one of the most poorly diagnosed and vitally important ionospheric variables.

While empirical models of electron precipitation have become increasingly sophisticated, knowledge of the associated conductivity dynamics on spatial scales down to 1 km is still lacking. Even less is known about conductivity enhancements due to ionospheric turbulence—effects that have been theoretically predicted to be capable of doubling the total height-integrated conductivity during disturbed geomagnetic conditions.

A compelling question is thus, What are the spatial and temporal scales of ionospheric structure and associated conductivity that determine energy deposition, plasma and neutral flows, and electrical current flow in the ionosphere-thermosphere interaction? Plasma of ionospheric origin mixes with solar wind plasma to populate the plasma sheet, ring current, and plasmasphere.

During episodic events such as storms and substorms, the presence of ionospheric plasma in these regions can be a controlling factor in geospace dynamics. For example, dense, convecting plasmaspheric plumes are thought to modulate dayside magnetic reconnection upon contacting the magnetopause. What are the processes that cause the plume structure to appear as storm-enhanced densities in the ionosphere? The relative abundance of these ions influences the plasma wave intensities that are responsible for the scattering and loss of radiation belt electrons. Recognition that ionospheric plasma is a critical agent in regulating the geospace system is accompanied by the humbling reality that researchers do not know what controls the abundance or distribution of ionospheric plasma in the magnetosphere.

How does the flow of ionospheric plasma into the magnetosphere during storms change as a result of IT plasma and neutral redistributions? The AIMI panel concluded that an additional major goal of the coming decade is to understand how the IT and magnetosphere interact to regulate their coupled response to solar wind forcing. Plasma-Neutral Coupling in a Magnetic Field. How do neutrals and plasmas interact to produce multiscale structures in the AIM system? An intriguing aspect of the IT system is the transfer of energy and momentum that occurs between the plasma and neutral components of the system, and how electric and magnetic fields serve to accentuate and sometimes moderate this interchange.

The pathways through which ions and neutrals interact are of course fundamental to space physics, as they occur all over our solar system.

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Addressing the compelling science questions described within previous sections also presents many opportunities to employ the IT system as a local laboratory to expand understanding of plasma-neutral coupling processes that have broad applicability across the solar system. In particular, these interactions occur over local, regional, and global scales, and in many cases cross-scale coupling exists. Some insight into the range of topics that can be addressed is provided in the following section, which begins with the low latitudes and then moves toward the polar regions.

The equatorial IT system represents a rich laboratory for investigation of plasma-neutral coupling in the presence of a magnetic field. The unique features are the quasi-horizontal orientation of the B field, the plasma instabilities that arise from this configuration, the ability of winds to generate electric fields through the E- and F-region dynamo mechanisms, the change in plasma-neutral collision frequency with height, the unimpeded ability of neutral winds to move plasma along field lines, and the relatively rapid change in magnetic inclination with latitude.

Combined with a variety of chemical processes, interactions between the plasma and neutral gases in the above environment produce emergent behaviors in the neutral and plasma densities, their bulk motions, and their temperatures. One example of emergent structures in neutral density is provided in Figure 8. The universal time day runs from right to left, so as to display the data on top of geographic maps. Crosses dashed lines mark the locations of the equatorial temperature anomaly ETA crests troughs. Magnetic activity was mostly quiet, except on day 83 when Kp reached values of The longitudinal alignment of the ETA trough and crests suggests a connection with a magnetic coordinate system and hence with plasma densities.

Researchers do not know how quiet-time and disturbance wind, electric field, and composition variations interacted to produce the observed changes. With just single-satellite sampleing, tmporal variations cannot be separated from longitude variations; moreover, measurements are made only at two local times. A constellation of satellites would remove the longitude-universal time ambiguity and would reveal how these structures varied in local time.

Forbes, Longitudinal and geomagnetic activity modulation of the equatorial thermosphere anomaly, Journal of Geophysical Research The longitudinal alignment is reminiscent of the plasma feature referred to as the equatorial ionization anomaly EIA , but the EIA maxima are less widely spaced in latitude and do not respond to changes in geomagnetic activity to the same degrees as do the neutral structures. Although theories exist that involve plasma and neutral transport and temperature and density responses due to adiabatic heating and cooling terms in the thermodynamic equation, the absence of coincident wind, temperature, electric field, and composition measurements over a range of spatial and temporal scales precludes a definitive interpretation.

What is needed to dispel speculation are simultaneous measurements of neutral and ion densities, temperatures, winds, and plasma drifts E fields so that physical connections can be explored and model simulations can be constrained. In fact, the proposed measurements will enable investigation of several low-latitude phenomena whose origins can be elucidated only through simultaneous multi-parameter measurements. These phenomena include, for instance, the equatorial temperature and wind anomaly, the midnight temperature maximum, the post-sunset atmospheric jet,.

In summary, the overarching question that captures most low-latitude IT phenomena is thus, How are gas temperatures and densities at low latitudes modified by momentum transfer between neutrals and ions in the presence of a magnetic field? Middle latitudes serve as a laboratory for different kinds of plasma-neutral interactions that also exhibit emergent behavior. The TEC data are obtained from a network of ground-based GPS receivers, and airglow measurements are obtained from ground-based all-sky imagers.

The depicted waves, which are predominantly south-westward propagating, are thought to originate as neutral density waves at high latitudes, which then interact with the mid-latitude ionosphere to create the observed structures; however, the occurrence of these waves is curiously unrelated to level of magnetic activity. It is hypothesized that the southwestward directionality of the waves, at least at nighttime, is aligned in the direction of weakest Joule damping as predicted by the Perkins instability.

This hypothesis is supported by measurements that indicate the existence of electric fields within the wave structures, which are. The TEC measurements were obtained using an array of GPS receivers, and the airglow measurements were made with five all-sky charge-coupled device cameras. The airglow emission is from excited neutral atomic oxygen atoms produced as a result of dissociative recombination of molecular ions and electrons. Note that the maxima in TEC mostly correspond with the airglow peaks, consistent with this interpretation. A North American ground-based observing network would enable investigation of these and many other regional-scale space weather phenomena involving fundamental plasma-neutral coupling processes, while a complementary satellite mission would provide insights into coupling on a global scale.

It also appears that the physics behind the ionospheric manifestation of the waves may be different during nighttime and daytime, and that their directionality varies with season. Note that explanation of this phenomenon involves coupling between instability, local, regional, and global-scale processes in ways that scientists do not understand, leading to the question, How do plasmas and neutrals interact across local, regional, and global scales to produce the operationally important density variations referred to as space weather?

Plasma-neutral interactions at high latitudes are strongly coupled to solar wind and magnetospheric dynamics. This coupling is regulated to a large extent by the ionospheric conductance, which is dependent on the ion and neutral gas densities. Despite their importance in the AIM interaction, the spatial distributions of these densities and their time variability are among the most poorly measured parameters of the IT system. Consequently, the interplay between neutral and ionized gas constituents and electromagnetic activity are not well understood.

At high latitudes, ion motions driven by the interaction of Earth with the solar wind provide the strongest forcing to the neutral atmosphere. The temporal and spatial scales of the neutral atmosphere response are quite different at different altitudes and quite different from those imposed by the driver. The driven neutral gas motions persist long after the driving fields change, and the neutral gas convects and diffuses well beyond the region of ion forcing. This complex interaction changes the energy deposited in the atmosphere, which causes changes in the global temperature, composition, and density that cannot yet be predicted.

For example, in both the cusp region and its counterpart in the night-side ionospheric convection throat, the average mass density of the neutral atmosphere near the F-region peak is observed to be significantly higher than that predicted by the empirical reference thermosphere MSIS90 Figure 8. This discrepancy has stimulated a search for the causative mechanisms. Determining cause and effect among these variables and advancing an operational capability to predict regional enhancements in neutral density will require simultaneous, multivariable measurements in the topside and bottomside ionosphere.

Thus the population of the magnetosphere by ionospheric outflows is also dependent on plasma-neutral interactions. Breakthroughs in the next decade in understanding the dynamic interaction between the magnetosphere and the IT system must therefore confront the question, How do activities in neutral and ionized gases and electromagnetic fields interact to produce observed magnetic field-aligned structure and motions of the thermosphere and ionosphere?

The AIMI panel concluded that a major goal of the decade is to understand the plasma-neutral coupling processes that give rise to local, regional, and global-scale structures in the AIM system, particularly those relevant to society. How is our planetary environment changing over multidecadal scales, and what are the underlying causes?

The preceding discussions indicate why achieving an understanding of how the whole atmosphere system is coupled to the geospace environment remains a singular challenge for AIM research. Model ionospheric convection streamlines are superposed. Burch with Remarks by C. Axford with Remarks by P. Peterson, and Takumi Abe Utilizing the Spacecraft Potential S. Hanson with Remarks by R. Johnson with Remarks by C. Liemohn and Daniel T.

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