Space Physics and Aeronomy, Ionosphere Dynamics and Applications - Группа авторов

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wide spread in model results, the fluctuations in measured Poynting flux are not captured in any of the models (see Fig. 1.8, panels (a) and (e)). This is also apparent in the plots of the timing errors shown as DT in panels (c) and (g) in both figures.

      Ultimately the effect of energy input into the ionosphere is Joule heating of ions and consequently of neutrals. The subject has been studied for many years, both from a theoretical approach (Cole, 1962; Vasyliunas & Song, 2005) and on the basis of empirical and physics‐based modeling (e.g., Ahn et al., 1983a; Lu et al., 2016, and many others). In general, the models show significant Joule heat in the auroral zone but little heating outside these latitudes.

      As might be expected from the model assessment described in section 1.5 above, when model predictions are compared with observations for specific locations during specific events, there are significant discrepancies between models and data. Examples have been shown by Huang et al. (2016) where measured ion temperatures at DMSP show the largest increases at polar, and not auroral, latitudes. Anomalously high ion temperatures have also been reported from ISR studies at auroral and polar latitudes (Akbari et al., 2017), suggestive of non‐Maxwellian plasma distributions.

      Discrepancies also appear when comparisons of neutral density and model predictions are carried out (Shim et al., 2012). Storm‐related neutral density perturbations have been observed poleward of the auroral zone in several event and statistical studies (Lühr et al., 2004; Liu et al., 2010; Huang et al., 2014, 2016).

      1.6.1 New Data Analysis and Modeling Approaches

      Capturing the energy input to the IT system is crucial to realistic specification and forecast of the IT response to solar wind driving. An assessment of the ability to forecast the impact of space weather on Total Electron Content and neutral density shows significant gaps in current capabilities (Shim et al., 2015). While large‐scale averages over several hours or large geographic areas generally indicates approximate agreement between model and observed parameters, comparisons on finer scales show discrepancies, which can be large, as indicated in the Rastaetter et al. (2016) study. Current operational models of MIT coupling depend on empirical and climatological approaches, which have limited forecast capability. The outstanding problem, illustrated in the model assessment carried out by Rastaetter et al. (2016), is that there is little consistency in the apparent model discrepancies. The discrepancy varies from event to event and from model to model.

      There are two classes of potential errors in the models:

      1 The current trend in GCMs is to use empirical models for the high‐latitude drivers. As has been pointed out, the results of these simulations can reproduce the average state of the ionosphere, but when detailed data for specific locations under specific conditions are compared with model predictions, the models show poor agreement.

      2 In the GCMs, a number of assumptions are made in order to reduce computational demands. The assumptions are reasonable if the system is driven by large‐scale perturbations in the solar wind. But the effect of small‐scale variability can be large as we discuss below.

      There are a number of possible solutions, which might alleviate the problem. Data assimilation has been used in the AMIE model, but as noted above, there are restrictions on the application of the methodology. Other assimilative models and tools such as the Data Assimilation Research Testbed (Anderson et al., 2009), the Global Assimilation of Ionospheric Measurements (USU_GAIM), the Global Assimilative Ionospheric Model (JPL‐GAIM), the Ionospheric Data Assimilation Four‐Dimensional (IDA4D) model, and others (Schunk, 2002; Scherliess et al., 2004; Hajj et al., 2004; Pi et al, 2004; Bust et al, 2004) have been developed but not widely applied to the high‐latitude region. The complexity of assimilation at polar latitudes is twofold. When energy enters high latitudes, it is typically sporadic and dynamic; hence, fluctuations on small temporal and spatial scales can be significant. Second, data in the Northern Hemisphere are sparse due to the high percentage of ocean. Distribution of ground receivers is limited and coverage is irregular. In the Southern Hemisphere, distribution of ground instruments is limited by harsh climatic conditions.

      The highest density of ionospheric data sources is probably the Global Navigation Satellite System (GNSS), a worldwide array of GNSS receivers. Data from approximately 5,000 receivers is newly available through the CEDAR Madrigal website (http://cedar.openmadrigal.org/index.html/). The repository contains vertical TEC for the past 20 years, and slant TEC for the past 2 years at the time of writing. It is expected that this will increase with time. While coverage at polar latitudes is restricted as noted above, GNSS data complements existing radar facilities and polar‐orbit satellite data collection. GNSS data are the basis of certain assimilative models as mentioned above. Wider distribution of TEC data will contribute to more accurate specification via assimilation, but does not resolve the outstanding problem of forecasting the IT response when the solar wind is fluctuating.

      A question related to data coverage and analysis is the relevant resolution required to capture the IT system response to magnetospheric input. It has been shown that estimates of Poynting flux increase if higher resolution data are used to capture the variability in the electric field (Codrescu et al., 1995; Cosgrove & Codrescu, 2009; Matsuo & Richmond, 2008). However, there has not been an investigation into the geoeffectiveness of the variability that should be carried out in order to place limits on required resolution for data as well as models. While it seems intuitive that larger Poynting flux will result in larger Joule heating, it is not clear whether the IT response depends on other constraints, such as the time needed for collisional chemical reactions or for transfer from Poynting flux power into kinetic energy of ions or neutrals.

      1.6.2 Wave Energy Input

      The field of MIT coupling has been dominated by fluid theory for many years, but as computer power has increased, ideas based on kinetic theory have been developed. Wave power is often ignored as a source of high‐latitude energy, but observations have shown that Alfvén waves, commonly present in the interplanetary medium, can contribute to the total energy available (Tsurutani et al., 1990, 1995; Chaston et al., 2005; Streltsov & Lotko, 2003; Verkhoglyadova et al., 2018). Kinetic transport of super‐thermal electrons (Khazanov et al., 2014, and references therein) show significant energy deposition related to magnetosphere‐ionosphere coupling processes. Evidence of ULF waves reaching ground observatories at polar latitudes has been reported

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