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A review on the numerical simulation of equatorial plasma bubbles toward scintillation evaluation and forecasting
Progress in Earth and Planetary Sciencevolume 4, Article number: 37 (2017)
Abstract
Equatorial plasma bubbles (EPBs) have been a longstanding and increasingly important subject because they cause severe scintillations in radio waves from Global Navigation Satellite System satellites. The phenomenon was found in the 1930s as irregular ionosonde observations and was termed equatorial spread F (ESF). ESF is interpreted as plasma density irregularities associated with EPBs that have nonlinearly evolved into the topside ionosphere. Numerical simulations have been powerful tools to study the fully nonlinear evolution of EPBs, which cannot be wholly understood from theoretical predictions. In this paper, historical achievements in the numerical simulation of EPBs are reviewed, and future directions toward scintillation evaluation and forecast are discussed.
Introduction
Satellite communication and navigation are often disrupted by irregularities in the ionospheric plasma density. Fresnel scale irregularities cause rapid fluctuations in the signal phase and amplitude, a phenomenon known as ionospheric scintillation (e.g., Yeh and Liu 1982; Kintner et al. 2007 and references therein). Under the phase screen approximation, the Fresnel scale is given by \(\sqrt {2\lambda z}\), where λ is the radio wavelength and z is the height of the irregularity layer (Kintner et al. 2007). Under the assumption that plasma density irregularities exist in the ionospheric F region, the Fresnel scale for the Lband frequencies used in the Global Navigation Satellite System (GNSS) is 300–400 m. The evaluation and forecast of such plasma density irregularities are now regarded as a critical issue for stable communication and precise navigation.
Severe ionospheric scintillations in the equatorial ionosphere are caused by a phenomenon called equatorial spread F (ESF) or equatorial plasma bubbles (EPBs) (e.g., Hysell 2000; Woodman 2009). Although the Rayleigh–Taylor instability has been considered as a likely candidate for ESF generation, it cannot explain the irregularities in the topside F region, where linear theory predicts plasma irregularities should be stabilized (e.g., Dungey 1956; Farley et al. 1970). Woodman and LaHoz (1976) proposed the concept of ionospheric “bubbles,” which nonlinearly evolve from the bottomside and penetrate above the F peak altitude. EPBs contain a broad spectrum of plasma density irregularities, as measured by sounding rockets and satellites. Plasma density undulations with wavelengths of hundreds of kilometers have often been observed before the onset of EPB formation and have recently been termed largescale wave structures (Tsunoda and White 1981; Tsunoda 2015). Intermediate and shortscale irregularities (tens of kilometers to the submeter scale) have been found to be dominant in fully developed EPBs with multiple spectral indices (e.g., Rino et al. 1981; Singh and Szuszczewicz 1984; Carrano and Rino 2016). Such spectral characteristics are analogous but not identical to neutral turbulence (Kelley and Hysell 1991). To evaluate scintillation effects, intermediatescale irregularities must be resolved in numerical models.
The first numerical simulation to study EPBs was conducted by Scannapieco and Ossakow (1976), who successfully reproduced a lowdensity region penetrating nonlinearly through the topside F region. Since then, a number of numerical simulations of the nonlinear evolution of EPBs have been conducted, as reviewed in the following sections. The most recent models developed by the author and colleagues could reproduce very turbulent structures inside EPBs (Yokoyama et al. 2014, 2015; Yokoyama and Stolle 2017; Rino et al. 2017). The purpose of this article is to review the development of numerical simulations of EPBs over the past 40 years and discuss a possible future research direction involving the use of stateoftheart numerical models toward the evaluation and forecast of ionospheric scintillations.
Theory
Although each numerical model solves each set of equations with different parameters and numerical schemes, they are governed by the fundamental laws of ionospheric electrodynamics: the continuity and steadystate momentum equations for ions and electrons and the divergencefree current condition (see also Kelley 2009; Yokoyama and Stolle 2017). Under the simplifying assumption of a single ion species, these equations are written as
where N _{ i,e } is the ion/electron density (N _{ i }=N _{ e }=N under the quasineutrality condition), V _{ i,e } is the ion/electron velocity, S _{ i } represents the chemical terms, e is the elementary charge, E=E _{0}−∇ϕ is the electric field, E _{0} is the background electric field, ϕ is the electrostatic polarization potential, B is the geomagnetic field, M _{ i,e } is the ion/electron mass, g is the acceleration due to gravity, k _{ B } is the Boltzmann constant, T _{ i,e } is the ion/electron temperature, ν _{ in,en } is the ion/electron collision frequency with neutrals, U is the neutral wind velocity, and J is the total current density.
For simplicity, the neutral wind velocity U was set to zero, and the appropriate approximation for the equatorial F region was applied. The ion and electron velocities and the current density J are then given by
where σ _{ P }≈NM _{ i } ν _{ in }/B ^{2} is the Pedersen conductivity. The linear growth rate of the Rayleigh–Taylor instability is obtained by substituting Eqs. (5) and (7) into Eqs. (1) and (4) for the linear analysis. The pressuregradientdriven current (the third term of Eq. (7)), which produces a diamagnetic current and enhances the main magnetic field intensity inside the EPBs (Stolle et al. 2006; Aveiro et al. 2011; Yokoyama and Stolle 2017) vanishes in Eq. (4), and thus, the Pedersen and gravitydriven currents are the major drivers of the instability. In the presence of a zerothorder vertical (zdirectional) density gradient, the linear growth rate is derived as
The growth rate is positive when the density gradient is antiparallel to g. Therefore, the linear theory predicts unstable conditions only below the F peak altitude, but density irregularities appear throughout the F region. The nonlinear terms in Eqs. (1) and (4) should be taken into account to understand the fundamental mechanisms behind the development of EPBs, for which numerical simulations have been developed since the late 1970s.
Numerical schemes
Global atmosphere and ionosphere models may use spectral methods based on spherical harmonic functions. However, regional ionospheric models for EPB studies should use finite difference or finite volume methods to enable the application of boundary conditions. A critical problem for finite difference and volume methods is the assurance of numerical stability and the suppression of numerical diffusion when solving Eq. (1). While EPBs develop in the models, sharp plasma density gradients tend to appear on the EPB walls, and these gradients should be captured by choosing appropriate numerical schemes. There are many classical schemes that have been used in the field of computational fluid dynamics, such as the upwind, leapfrog, and Lax–Wendroff schemes. These can be applied under relatively uniform and stable flows but are inappropriate for the simulation of plasma instabilities. Lower order schemes suffer from excessive numerical diffusion, whereas higher order schemes suffer from dispersive ripples in the wake region of the flow. The fluxcorrected transport (FCT) method (Zalesak 1979) has been a popular scheme in the ionospheric modeling field (e.g., Zalesak and Ossakow 1980; Retterer 2010a). The FCT scheme implements a flux limiter by combining higher and lower order schemes so as not to produce overshoot or undershoot at the subsequent time step. A similar technique called the partial donor cell method (Hain 1987) has been applied to recent models (e.g., Huba and Joyce 2007; Huba et al. 2008). The total variation diminishing (TVD) method (Harten 1983) is another popular technique that can capture shocklike structures without oscillation (e.g., Aveiro and Hysell 2010; Hysell et al. 2014b). Among these advanced algorithms, in the authors’ experience (e.g., Yokoyama et al. 2014), the constrained interpolation profile (CIP) method (Yabe et al. 2001, 2004) is the best method to deal with ionospheric irregularities. The CIP method treats the firstorder spatial derivatives of the plasma density as dependent variables so that plasma density gradients are transported over time. With the thirdorder accuracy maintained in time and space, shocklike EPB walls and turbulent internal structures can be captured by the CIP method.
Equation (4) can be rewritten as
which is a boundary value problem for the electrostatic potential ϕ with the source function S and yields a sparse linear system of equations. Classical direct methods, such as Gaussian elimination, can be used to solve this problem within a finite number of operations; however, such methods destroy the sparsity of the matrix and necessitate the allocation of a huge amount of additional memory. An efficient direct solver called the stabilized error vector propagation (SEVP) method (Madala 1978) has been applied in recent models (e.g., Retterer 2010a; Duly et al. 2014). Generally, iterative methods are preferred for sparse linear system solvers because the sparse matrix–vector product is the main operation during each iteration. However, classical iterative solvers, such as the Jacobi, Gauss–Seidel, and successive overrelaxation (SOR) methods, do not converge effectively in largescale threedimensional (3D) problems. As an alternative, Krylov subspace methods have been developed as effective sparse linear system solvers. Examples of the variants of the Krylov subspace methods include the conjugate gradient (CG), biconjugate gradient stabilized (BiCGSTAB), and generalized minimum residual (GMRES) methods. In combination with appropriate preconditioning techniques such as incomplete LU factorization on parallel computers, Krylov subspace methods can achieve excellent convergence efficiency. A different approach called the multigrid method exploits discretizations with a hierarchy of grid coarseness levels to obtain optimal convergence using relaxation techniques. Saad (2003) has provided a detailed explanation of iterative methods, including a theoretical background and different types of algorithms used in such methods. A new algorithm of the Krylov subspace method is currently under development (e.g., Fujino and Murakami 2013) and has been implemented in new simulation models (e.g., Yokoyama et al. 2014). Some software packages of sparse linear system solvers are available online, including SPARSKIT (http://wwwusers.cs.umn.edu/~saad/software/SPARSKIT) (Saad 1990) and MUDPACK (https://www2.cisl.ucar.edu/resources/legacy/mudpack) (Adams 1991).
Twodimensional models
As mentioned above, the linear theory of the Rayleigh–Taylor instability does not predict the appearance of ESF above the F peak altitude, where the plasma density gradient has the same orientation as the gravitational force. It is essential to understand the nonlinear behavior of equatorial ionospheric plasma instabilities, which can be realized only through numerical simulation. Fortunately, the geometry of the equatorial ionosphere can be simplified easily on a twodimensional (2D) plane. When the zonal and vertical directions are defined as the two axes of the simulation domain at the dip equator, the geomagnetic field is perpendicular to the plane, allowing the electrodynamics parallel to the geomagnetic field to be ignored. Figure 1 shows the results obtained by Scannapieco and Ossakow (1976). Although the simulated EPB structure was oversimplified and took a very long time to evolve to the topside, it was an important achievement to simulate the penetration of the density irregularities generated in the bottomside F region into the topside F region, where the linear theory predicts no irregularities to exist.
Since the nonlinear evolution of EPBs was first successfully modeled by Scannapieco and Ossakow (1976), their group has improved the original numerical model. Zalesak and Ossakow (1980) successfully reproduced large horizontalscale EPBs from equally largescale initial perturbations by implementing a new FCT algorithm (Zalesak 1979). The FCT algorithm suppressed numerical diffusion at the sharp density gradients at the walls of the simulated EPBs and enabled the rapid growth of the EPBs into the topside. Zalesak et al. (1982) have developed a threelayer model that consists of the magnetic equatorial plane and the conjugate E regions connected by the magnetic field lines. A remarkable result they achieved using this model is the reproduction of the bifurcation from the flattened tops of EPBs, as shown in Fig. 2. From previous plasma cloud experiments (e.g., McDonald et al. 1981), they concluded that a background Eregion Pedersen conductivity played a role in the bifurcation of EPBs. They also found that a uniform eastward neutral wind contributed to the westward tilt of the EPBs, as shown in Fig. 3. Even though the neutral wind was uniform in altitude, the zonal drift velocity driven by the Fregion dynamo tended to have a vertical shear as a function of \(\Sigma _{P}^{F}/\left (\Sigma _{P}^{F} + \Sigma _{P}^{E}\right)\), where \(\Sigma _{P}^{F}\) and \(\Sigma _{P}^{E}\) are the fluxtubeintegrated Pedersen conductivities in the F and E regions, respectively. An important implication of this result is that the variations of physical parameters along geomagnetic field lines should be taken into account, which has led to the progress of theoretical work (e.g., Sultan 1996) and 3D numerical models, as presented in the next section.
Once the instability is triggered and irregularities have formed inside EPBs, they may cause severe scintillations. The degree to which satellite signals are affected by the irregularities depends on the spectral characteristics of the irregularities. Although the important features of largescale EPBs observed at that time were clearly reproduced by Zalesak et al. (1982), intermediatescale structures close to the Fresnel scale of VHF and Lband signals were also studied through simulations and compared with in situ observations (e.g., Keskinen et al. 1981; Zargham and Seyler 1987, 1989; Kelley et al. 1987). Because it was not easy to capture a wide range of irregularity spectra using simulation models at that time, these models have limited spatial domains and focused on only intermediatescale irregularities. A recent highresolution model may be able to consider unified spectral characteristics along with largescale nonlinear EPB formation (Rino et al. 2017).
A longstanding and still unresolved problem in the equatorial ionosphere is what triggers ESF/EPBs. Daytoday variability in the occurrence of ESF is largely unpredictable (e.g., Hysell and Burcham 2002; Woodman 2009; Retterer and Roddy 2014). Because the linear growth rate of the Rayleigh–Taylor instability on its own cannot be large enough to account for the rapid growth of EPBs from thermal fluctuations (e.g., Farley et al. 1970), an initial “seeding” is required in EPB simulations. In most previous simulations, plasma density perturbations have been used as the initial seeding, but the source of such initial density perturbations has not been discussed. Meanwhile, the interaction between atmospheric gravity waves (AGWs) and ionospheric plasma has long been considered as a plausible mechanism to modulate the ionosphere (Hines 1960). From Jicamarca radar observations, Kelley et al. (1981) have proposed that the modulation of the bottomside density gradient induced by AGWs is amplified by the Rayleigh–Taylor instability. The seeding effect by AGWs has been numerically analyzed in a series of studies (Huang and Kelley 1996a, b, c, and d). It was concluded from these studies that AGWs over a wide range of amplitudes and wavelengths work effectively as a seeding mechanism.
The growth rate of the original Rayleigh–Taylor instability described in Eq. (8) can be extended to that of a generalized Rayleigh–Taylor instability by including electric field and neutral wind effects (e.g., Kelley 2009). Sekar et al. (1994) included vertical winds in their model and showed that downward wind enhanced the growth of EPBs. The variability of the vertical wind, which may be related to AGWs, could be responsible for the daytoday variability of the generation of EPBs. They also investigated EPB growth under various background conditions, such as seeding amplitudes and wavelengths, topside F region profiles, zonal plasma drift shear effects, and molecular ions (Sekar 2003and references therein).
Although the idea of the seeding of ESF and EPBs by AGWs has been widespread, it is quite difficult to find direct evidence of the interaction between AGWs and the generation of ESF and EPBs. It is true that some initial perturbation in the bottomside F region must occur for it to be amplified by the Rayleigh–Taylor instability, but AGWs may not be the only source of such perturbations. Hysell and Kudeki (2004) have proposed that the vertical shear of zonal plasma drift in the bottomside F region around sunset triggers ESF via a collisional shear instability. The growth rate of this instability could be comparable to that of the Rayleigh–Taylor instability, and their simulation results were consistent with radar observations prior to the onset of ESF. They concluded that in addition to AGWs, shear instabilities must be considered as another likely seeding source.
Higher spatial resolution and improved numerical schemes have enabled the simulation of the internal structures of EPBs, which could not be reproduced using previous models. Huba and Joyce (2007) have developed a new code that uses an eighthorder spatial interpolation scheme and the partial donor cell method (Hain 1987). Figure 4 shows a number of secondary bifurcations from the walls of primary depletions. Although turbulent structures were reproduced in this model, Vshaped primary depletions are somewhat unnatural and may have arisen because of the 2D treatment. Around this time, a rapid transition from 2D to 3D modeling studies was underway.
Threedimensional models
The 2D models presented in the previous section assume that all parameters are uniformly distributed along latitude and the magnetic field lines extend to infinity in the horizontal direction. These assumptions are far from the real configuration, in which equatorial ionization anomalies and magnetic field curvature are present. The rapid advancement of highperformance computing technology has made it possible to conduct ionospheric simulations in a fully 3D domain. In preliminary 3D simulations of EPBs presented by Keskinen et al. (2003) and Kherani et al. (2005), it was concluded that finite parallel conductivity effects slow the evolution of EPBs. 3D modeling studies of EPBs have been widely recognized since a new model was developed by Huba et al. (2008) based on the global ionosphere model SAMI3. As shown in Fig. 5, as EPBs grow into higher altitudes, magnetic flux tubes become fully depleted, and steep plasma density gradients form around the equatorial ionization anomaly regions. Although such structures were expected from ground and satellite observations, the SAMI3/ESF model clearly reproduced the 3D structure for the first time. Intensive studies using the model have been conducted, including studies on the effects of neutral wind on EPB evolution (Huba et al. 2009; Krall et al. 2009; Huba and Krall 2013), the decay phase of EPBs (Krall et al. 2010a, b), and the electrostatic reconnection process of merging EPBs (Huba et al. 2015).
The seeding of EPBs by collisional shear instabilities has been studied by Hysell et al. (2006) using a model that includes finite parallel conductivity effects. The model was extended by Aveiro and Hysell (2010) to reproduce the nonlinear evolution of EPBs seeded by collisional shear instabilities. Because the nonequipotential solution provides the 3D current system in the model, including diamagnetic and fieldaligned currents, the magnetic signatures inside EPBs can also be reproduced (Aveiro et al. 2011; Yokoyama and Stolle 2017). Aveiro and Hysell (2012) and Aveiro and Huba (2013) further examined the difference between the equipotential and nonequipotential solutions and concluded that the nonequipotential solution contributed to the formation of complex EPB structures. The model was also applied to the evaluation of actual observations by adopting presunset observation data to define the initial conditions (Aveiro et al. 2012; Hysell et al. 2014b, c, 2015). This data assimilation approach may greatly strengthen the probability of forecasting the occurrence of EPBs.
The seeding mechanism of EPBs remains one of the most important subjects investigated using numerical models, and the effects of AGWs have been intensively studied in this context. Most studies on this topic have yielded results that indicate AGWs with large vertical wavelengths (> 100 km) are possible seeding sources of EPBs (Keskinen and Vadas 2009; Keskinen 2010; Krall et al. 2013a, b; Retterer and Roddy 2014). On the other hand, Hysell et al. (2014a) concluded that AGWs with small vertical wavelengths (< 100 km) did not trigger topside ESF, though they did deform the bottomside density structures to some extent. The difference between the results of these studies has been attributed to the background neutral wind conditions and the interaction time between AGWs and ionospheric plasma. Offequatorial phenomena, that is, sporadicE (E _{s}) layers and mediumscale traveling ionospheric disturbances (MSTIDs), have also been proposed as seeding sources of ESF and EPBs via electric field mapping along geomagnetic field lines (Tsunoda 2007; Miller et al. 2009). A preliminary modeling study has been conducted by using the SAMI3/ESF model with artificially imposed MSTID structures in offequatorial regions (Krall et al. 2011). These effects could be quantitatively investigated by coupling the 3D ESF models with highresolution midlatitude models (e.g., Yokoyama and Hysell 2010) that can numerically reproduce the E _{s}layer instability and MSTIDs.
An interesting approach is to resolve EPBs in a global ionospheric model. Huba and Joyce (2010) modified the dusk sector of the global SAMI3 model to have a higher spatial resolution (approximately 7 km). Owing to the selfconsistent treatment of global electrodynamics and the formation of EPBs in this method, largescale EPBs are generated successively at the dusk sector as shown in Fig. 6. This method coupled with a global thermosphere model would be a strong tool to assess the possibility of EPB occurrence.
The most recent 3D model is the HighResolution Bubble (HIRB) model developed by Yokoyama et al. (2014). Adopting a spatial resolution as fine as 1 km and the CIP scheme for plasma transport, the HIRB model is capable of reproducing EPBs that grow nonlinearly from the crest of a largescale upwelling, bifurcate at the top of EPBs, then become turbulent at the topside of the F region. Figure 7 shows the plasma density distribution of fully developed EPBs in a 3D domain. This distribution shows that depletions contain very turbulent structures that are elongated along magnetic flux tubes and reach offequatorial latitudes. Applying multiple seeding components and an eastward neutral wind, east–west asymmetry, and tilted structures can also be reproduced, as shown in Fig. 8 (Yokoyama et al. 2015). Although the outline of tilted EPBs is similar to the previous 2D model, result shown in Fig. 3, their internal structures are markedly different.
Even though computer hardware has been significantly advanced, it is still difficult to simultaneously reproduce the Fresnel scale of Lband signals (300–400 m) and largescale EPBs (approximately 100 km) in the same model. Retterer (2005) proposed a scintillation forecasting system based on numerical modeling and satellite observation as a part of the Communication and Navigation Outage Forecasting System (C/NOFS) program. Retterer and Gentile (2009) conducted an EPB simulation with the physicsbased model (PBMOD) described in Retterer (2005). The initial background conditions were derived from the global ambient ionospheric model that was used for scintillation forecasting with vertical plasma drifts (Retterer et al. 2005). The simulated EPB occurrence was well correlated with DMSP satellite observations. Retterer (2010a, b) tried to evaluate amplitude scintillation with a phase screen model by extrapolating the density irregularity spectra of EPBs simulated by the PBMOD. However, because the spatial resolution of the PBMOD was limited to 2.5 km at most, spectral breaks at the intermediate scale were not observed (e.g., Singh and Szuszczewicz 1984). To extrapolate irregularity spectra down to the Fresnel scale, it is necessary to reproduce smallerscale irregularities as accurately as possible. The spatial resolution of the HIRB model was improved for this purpose. In the model with improved resolution, the longitudinal axis is divided by 1120 grid points with a grid spacing of 333.6 m. The number of magnetic field lines on the magnetic meridian is increased more than twofold to 1821, and the altitude range of 300 to 800 km over the magnetic equator is uniformly sampled with a spacing of 700.8 m.
Figure 9 shows a 2D snapshot of the higher resolution result under the same conditions as for Fig. 8, demonstrating that more turbulent internal EPB structures can be observed at a higher resolution. The power spectra of the irregularities inside the EPBs were calculated along the zonal and vertical coordinates using a simple FFT technique, and they were averaged over altitudes ranging from 400 to 700 km. Figure 10 shows the average power spectra along the zonal and vertical coordinates. Spectral breaks appeared near 2 and 8 km for zonal and vertical density irregularities, respectively. The break scales are nearly the same as those seen in the previous in situ measurements (Singh and Szuszczewicz 1984). Waveletbased analysis may provide a better description of the spectral characteristics (Rino et al. 2014, 2016). Analysis of the simulated spectral characteristics based on wavelet analysis techniques is underway (Rino et al. 2017).
Conclusions
Numerical modeling efforts to understand ESF and EPBs in the past 40 years were reviewed in this article. Since the nonlinear evolution of EPBs was first successfully modeled, various models have been intensively developed and improved because of the rapid advancement of highperformance computing technology and numerical algorithms. However, present methods remain far from forecasting the occurrence of EPBs on a daytoday basis. Some models set up initial background conditions from global ionospheric models, but there are significant deviations among the existing global models, especially under nighttime conditions (Anderson et al. 1998; Fang et al. 2013). This means that the causes of the daytoday variability of the background ionosphere are not fully reflected in existing global models. It may be necessary to include assimilative techniques from realtime observations to reliably model the background conditions. Furthermore, the growth of EPBs in the models strongly depends on how initial seeding perturbations are added. As the required spatial resolution for EPB formation (< 10 km) is much finer than that of the global models (> 1°), the use of some artificial inputs as seeding perturbations is unavoidable. It is necessary to employ appropriate background conditions and initial perturbations to conduct reliable forecasting using numerical models, but this is not an easy task.
The recent development of a highresolution bubble model has made it possible to resolve nearly Fresnel scale irregularities for Lband GNSS signals. Because the spectral characteristics of density irregularities inside EPBs do not obey a simple power law, extrapolation from largescale irregularities cannot be used to accurately estimate the scintillation strength. It is necessary to directly resolve Fresnel scale irregularities to quantitatively evaluate the scintillation. On the other hand, several issues must be addressed for the development of veryhighresolution models. The equipotential assumption may no longer be justified, and the ion inertial term must be included for parallel transport. These terms can be omitted for the evolution of largescale EPBs, but they do affect density irregularities smaller than approximately 100 m.
The next realistic step is to couple global simulation models, in which realtime observation data are assimilated, with regional models that can resolve smallscale irregularities. The partially highresolution global model developed by Huba and Joyce (2010) could be applied relatively easily for forecasting purposes. Regarding the model configuration, the definition of appropriate boundary conditions is important because EPBs tend to occur around the dusk terminator, where the eastern and western boundaries should correspond to the nightside and dayside ionospheres, respectively. An understanding of the electrodynamics in the dusk side is still important for EPB forecasting.
If a full highresolution global simulation model were realized, it could model all phenomena at all scales. Such a model might be realized in the distant future, but we should keep developing stateoftheart models and prepare for the future when superhighperformance computers become available.
Abbreviations
 AGW:

Atmospheric gravity wave
 CIP:

Constrained interpolation profile
 ESF:

Equatorial spread F
 EPB:

Equatorial plasma bubble
 FCT:

Fluxcorrected transport
 GNSS:

Global navigation satellite system
 HIRB:

Highresolution bubble
 PBMOD:

Physicsbased model
 SAMI3:

Sami3 is also a model of the ionosphere
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Acknowledgements
This work was carried out as a computational joint research program at the SolarTerrestrial Environment Laboratory, Nagoya University, Japan. The simulation was also performed by using Hitachi SR16000/M1 at the National Institute of Information and Communications Technology (NICT), Japan.
Funding
This work was supported by JSPS KAKENHI Grant Number 16K17814.
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Correspondence to Tatsuhiro Yokoyama.
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Keywords
 Equatorial ionosphere
 Equatorial spread F
 Equatorial plasma bubbles
 Numerical simulation
 Scintillation
 Highperformance computing
 Space weather