Comparative Study of the Geomagnetic Activity Effect on foF2 Variation as Defined by the Two Classification Methods at Dakar Station over Solar Cycle Phases

This paper aims to establish a comparison between both geomagnetic activity classification methods on foF2 diurnal variation over solar cycle phases. It concerns first a comparison of geomagnetic activity occurrences according to both classification methods; and second the geomagnetic effect on foF2 diurnal variation profiles as defined for the equatorial latitudes. The occurrences of the different disturbed geomagnetic activities (recurrent activity (RA), shock activity (SA) and fluctuant activity (FA)) according to both classifications (ancient classification (AC) and new classification (NC)) have been studied at Dakar ionosonde station (Lat: 14.8 ̊N; Long: 342.6 ̊E). Regarding both classifications, the RA occurs more during the decreasing phase. And it’s observed that the RA occurs the most during the increasing phase for the AC and during the minimum phase for the NC. The maximum gap of occurrence ( occ ∆ ) between both classifications is −11.1% (for the negative value which is observed during the increasing phase) and +16.74% (for the positive one which is observed during the decreasing phase). The occurrence of the SA in relation with both classifications is the lowest during the minimum phase and the maximum occurrence is observed during the maximum and decreasing phases, for the AC, with a value close to 37% and for the NC at the maximum phase with a percentage of 54.47%. The maximum gap of occurrence ( occ ∆ ) between both classifications is −17.85% (for the negative value which is observed at maximum phase) and +13.53% (for the positive one which is observed during the decreasing phase). For both classifications, the FA occurs the least during the minimum phase and the most during the maximum phase for the AC and at maximum and decreasing phases with percentage How to cite this paper: Sandwidi, S.A., Gnabahou, D.A. and Ouattara, F. (2020) Comparative Study of the Geomagnetic Activity Effect on foF2 Variation as Defined by the Two Classification Methods at Dakar Station over Solar Cycle Phases. International Journal of Geosciences, 11, 501-517. https://doi.org/10.4236/ijg.2020.118026 Received: July 3, 2020 Accepted: August 14, 2020 Published: August 17, 2020 Copyright © 2020 by author(s) and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY 4.0). http://creativecommons.org/licenses/by/4.0/


Introduction
The irradiation of the Earth space environment by the magnetized plasma propagating from the Sun induced a continuous global magnetic disturbance, namely geomagnetic storms [1]. In fact, the Sun magnetic field interacts with the Interplanetary Magnetic Field (IMF) by means of its two components: 1) the poloidal magnetic field which is closed and responsible of the Coronal Mass Ejections (CMEs), the magnetic clouds and high stream solar wind, 2) the toroidal magnetic field named sunspot activities which is the source of slow solar wind [1] [2] [3] [4] [5].
This Sun-Earth interaction is characterized by four geomagnetic events identified by [1] by using: 1) the geomagnetic aa index carried out by [6] [7] [8] [9], 2) the date of Sudden Storm Commencement (SSC) and 3) the correlation existing between the geomagnetic aa index and the solar wind speed established by Svalgaard [10]. The same number of geomagnetic activity has been found by Richardson et al. [2] [3] [4], but they named the fluctuating activity as the unclear activity which characterized the cases where the solar mechanisms cannot be clearly identified. This classification gives only 60% of the geomagnetic activities solar sources clarification.
Zerbo et al. [11] established a new classification criterion which clarifies about 80% of the geomagnetic activities solar sources by lowering the limit of the aa index for the shock and recurrent events and adding other causes from solar activity. Then the two schemes are different only for the disturbed geomagnetic activities. This paper deals with the comparison of the both classifications critical frequency of the ionosphere F2 layer (foF2) diurnal profiles as measured at Dakar ionosonde station (Lat: 14.8˚N; Long: 342.6˚E; dip: +5.53).
Several papers (e.g. [12]- [23]) have been carried out in African Equatorial Ionization Anomaly (EIA) sector about the morphological studies of the foF2 profiles by using Legrand  International Journal of Geosciences layer critical frequency (foF2) time variation at Dakar station. The novelty of this study appears as it is a first paper where such comparison is made for the two classification methods. This paper aims, in short term, to highlight how the signature of the storm effect is shown by the geomagnetic events of the both classification methods and in mean and long term to contribute to improve the understanding of the sources of geomagnetic activities.
The outline of the paper is as follows: Section 2 concerns materials and methods, Section 3 is devoted to results and discussions, and the conclusion and research perspectives end the paper as its fourth section.

Data
For the present paper, data involved are:

Description of the Two Geomagnetic Activity Classification Methods
Based on the strong correlation between geomagnetic index Aa (obtained from the following website: http://isgi.unistra.fr/data_download.php) and solar wind velocity established by [1] and [10] [32] whereas the scheme proposed by Zerbo et al. [11] allows to clearly classify 80% of the geomagnetic activity. The new classification is characterized by: 1) the same limit with the first classification for the quiet activity (Aa < 20 nT) and 2) the lowering of the limit (Aa ≥ 20 nT) for the shock and recurrent events for whom the causes from solar activity are more highlighted [11]. Therefore: 1) recurrent activities (RA), characterised by Aa ≥ 20 nT, are now the recurrent activity of Legrand and Simon plus the Corotative Moderate Activity (CMA) and they are due to solar high wind stream and Corotating interaction Region (CIRs); 2) shock activities (SA) are now the shock activity of Legrand and Simon plus the Cloud Shock Activity (CSA) and they are caused by Coronal Mass Ejections (CMEs) and magnetic clouds, respectively, with Aa ≥ 20 nT and 3) fluctuating activities (FA) or unclear events represent the fluctuating activity of Legrand and Simon plus the Corotating Moderate Activity (CMA); they are consequences of the fluctuation of solar heliosheet. This paper thus concerns the comparison between the profiles of foF2 daily variation during disturbed activities of both schemes of geomagnetic activity classification as described.
The pixel diagram presents the variation of the geomagnetic activity by solar rotation, also called Bartels rotation [12] [34]. It shows per year an overview of the whole solar geoeffectiveness activity (each type of the solar wind activity [slow, recurrent, CIRs and fluctuating winds activity] and that of CMEs and magnetic clouds [19]. This colour board is used to determine the geomagnetic data as a function of solar activity as described by solar rotation duration (27 days) which consists of: 1) plotting the aa daily values in Bartels diagrams, 2) exhibiting the different types of geomagnetic activities as described above according to both criteria. Figure 1 showed the pixel diagram highlighting the process to determine the different geomagnetic activities following the criteria of the two methods of classification.

Data Analysis Method
This paper aims to study the difference of foF2 time variation, throughout solar cycle phases for a given disturbed activity for the both geomagnetic activity classifications. The data analysis will be done through two ways: 1) The analysis of the recurrence of the different geomagnetic activities according to the both methods of classification over solar cycle phases in one case and seasons in another case; 2) The profiles obtained are analyzed in comparison with the five standard profiles established by [35] for African Equatorial Ionization Anomaly (EIA) region and 3) the quantitative analysis based on comparison between foF2 profiles from both classifications methods.
Firstly, the analysis of the occurrence of the geomagnetic activities is done by: 1) comparing the occurrence of the different geomagnetic activities in relation with the both classification by using the Equation (1)  NC is the occurrence of the concerning geomagnetic activity class in relation with the new classification And 2) putting error bars in data graphs. We can note that error bar is obtained by using the Equation (2) and N the total number of observations for a particular dataset.
Secondly, the foF2 profiles (see Figure 2), linked to the nature, the strength or the absence of electric currents in E layer of ionosphere [36] [37] [38] [39] [40], are: Noon bite out or B profile characterized by a double peak (morning and evening) parted by a trough around midday; Reversed or R profile characterized by a single peak at evening; Morning pic or M profile characterized by a single maximum at morning; Plateau or P profile characterized by an ionization plateau International Journal of Geosciences This morphological analysis of the profiles will reveal the difference between the equatorial ionosphere characteristics highlighted by the profiles obtained by the both classification methods. In fact those profiles express respectively a signature of a high electrojet, an important afternoon conter-electrojet, a moderate electrojet, a weak electrojet and an absence of electrojet. In addition [41]- [47] reviewed on mechanism responsible of equatorial trough at noon induced by electrodynamics × E B process. In a third time, the quantitative analysis based on the appreciation of the difference between foF2 values of the ancient classification and those from the new one will be made through the relative deviation of foF2 defined by: where AC foF2 and NC foF2 are the foF2 from the ancient geomagnetic activity classification and the new one respectively. foF2 ∆ is the relative deviation with the following appreciation:   throughout solar cycle phases (panels "a" and "b"). The panels "a" and "b" concern the ancient classification (AC) and the new classification (NC) respectively.     Figure 6. The same as Figure 5 but for shock activity. tion of the geomagnetic activity) will enable to make difference with the AC. Figure 5 shows the foF2 values diurnal variation for the RA according to the two classification methods and the relative deviation percentage between both classifications. The panels "a" and "d" highlight that the two classifications curves show an "R" profile during the minimum and the decreasing phase. Therefore, the RA is characterised by the presence of an important afternoon conter-electrojet in the E layer of the ionosphere during minimum and decreasing phases considering the two classifications. Otherwise for the decreasing phase (panel "d"), we observe a difference between both classifications between 2100 LT to 0400 LT with respect to error bars shown in NC graph and for the remaining daily time the two profiles were overlapped. The right column of the panel "d" highlights this observation. In fact, we observe that the foF2 σ shows value: 1) within ±10% between 0500 LT to 2000 LT, 2) a value greater than +10% between 2100 LT to 0400 LT with a maximum positive value of +20.27% observed at 0000 LT and 3) the negative values between 0700 LT to 0900 LT with a maximum negative value of −4.04% observed at 0800 LT. And during minimum phase (panel "a"), the AC curve is almost always over the curve of the NC with respect to error bars shown in NC graph; but only before 0600 LT to before 0800 LT the two curves were overlapped and we observe a difference between the graphs of both classifications between 1000 LT to 0200 LT with respect to error bars shown in NC graph. The right column of this panel highlights this observation. In fact, the foF2 σ shows value within ±10% between 0600 LT to 0900 LT and 1500 LT to 1700 LT. The maximum positive foF2 σ value is observed at 0100 LT with a value equal to +55% and the single negative value, observed at 0600 LT and equal to −5.15%.

Profiles Comparison for Both Classifications throughout Solar Phases
Panel "c" shows that during the maximum phase, both curves show a "P" profile for both classifications. Therefore, the RA is characterised by a weak electrojet in the E layer of the ionosphere during the maximum phase considering both classifications. Otherwise, we observe that the two graphs are overlapped during all the daytime; but both curves are different at 0600 LT and between 2000 LT to 2400 LT with respect to error bars shown in NC graph. Both curves showed a night time peak, with a peak of 12 MHz observed at 2100 LT (for the curve of AC) upper that of the NC (peak of 10 MHz observed at 2200 LT σ value is observed at 2100 LT with a value equal to +18.80% and the maximum negative value, observed at 0600 LT, is fairly equal to −13.27%. At the increasing phase (panel "b") we observe a high difference between the two curves. The NC curve shows an "R" profile while the AC profile shows a B profile with a trough around 1300 LT. Therefore, during increasing phase, the RA shows an important afternoon conter-electrojet for the NC while it is characterized by an intense electrojet for the AC. Otherwise, we observe that the AC graph is almost over that of the NC, except between 0500 LT to 0600 LT and at 1600 LT. We observe that the two graphs are nearly overlapped between 1300 LT to 1600 LT; but both curves are different between 1800 LT to 0300 LT, 0500 LT to 0600 LT and 0800 LT to 1100 LT with respect to error bars shown in NC graph. The right column of this panel highlights this observation. In fact, the foF2 σ graph shows values within ±10% at 0700 LT, at 0400 LT and between 1200 LT to 1700 LT. The maximum positive foF2 σ value is observed at 0100 LT with a value equal to +93.55% and the maximum negative value, observed at 0500 LT, is equal to −26.10%. Figure 6 shows the foF2 values diurnal variation for the SA according to the two classification methods and the relative deviation percentage between both classifications. Panel "a" shows a "B" profile for both classifications graphs with an afternoon peak greater than the morning one. Therefore the SA of the two classifications is characterized by a high electrojet during minimum phase. Otherwise, we observe that the AC graph is almost over that of the NC. And the graph presents a difference between both classification's curves between 2100 LT to 0500 LT with respect to error bars shown in NC graph; but for the remaining daily time the two profiles are closely in a good agreement. The right column of this panel highlights this observation. In fact, the foF2 σ curve shows positive values within [0; +10%] at around 0300 LT and between 0500 LT to 2100 LT. The maximum, observed at 0000 LT, is equal to +29.84% and the minimum one, observed at 1800 LT, is equal to +1.48% Panel "b" presents an "R" profile for both classifications graphs; but that of the AC is coupled with a trough observed at 1400 LT. Therefore, at solar increasing phase, the SA of the NC classification is characterized by an intense afternoon conter-electrojet while the one of the AC is characterized by a couple of an intense afternoon conter-electrojet and a late high electrojet, signature of a trough observed at 1400 LT. Otherwise, we observe a difference between both classification's curves between 2000 LT to 2300 LT with respect to error bars shown in NC graph; but for the remaining daily time the two profiles are closely in a good agreement. The right column of this panel highlights this observation. In fact, the foF2 σ curve shows values within ±10% between 2000 LT 2300 LT. The maximum positive foF2 σ value is observed at 2100 LT with a value equal to +26.51% and the maximum negative value, observed at 0500 LT, is equal to −9.84%. At maximum phase (panel "c"), for both classifications graphs, the SA profile is characterized by "P" profile which is a signature of a weak electrojet. We observe that the two curves are overlapped during all the daily time with respect to error bars shown in NC graph. The right column of this panel highlights this observation. In fact, the foF2 σ curve shows values within ±10% during all the daily time. Otherwise, we observe at 3.1) that the maximum negative gap between both classification occurrences for SA is observed at maximum phase with a value occ 17.85% ∆ = − . Therefore the Cloud Shock Activity CSA occurs more during solar maximum like have been found by [11] [49]. We can make the assumption that a high occurrence of CSA doesn't impact the electrodynamics of the ionosphere E layer.
Panel "d" presents an "R" profile for both classifications graphs. Therefore, at solar decreasing phase, the both classification's SA are characterized by an intense afternoon conter-electrojet. We observe that the two curves are overlapped during all the daily time. The right column of this panel highlights this observation. In fact, the foF2 σ curve shows values within ±10% during all the daily time. Otherwise, we observe at 3.1) that the maximum positive gap between both classification occurrences for SA is observed at decreasing phase with a value occ 13.53% ∆ = + . Therefore, we can make the assumption that the high occurrence of cloud shock activity (CSA) doesn't impact the electrodynamics of the ionosphere E layer.

Conclusion
This paper shows that both classifications geomagnetic classes, at Dakar station, are different in terms of occurrences throughout solar cycle phases. It emerges that, for the RA, the higher the occurrences between two classes for a given phase are different, the more the profiles show difference and also the physical interpretation of the electrodynamics in the ionosphere layer. But the SA profiles of both classifications are closely similar during maximum and decreasing phase.
In general, the AC and NC curves show different profiles during minimum and increasing phases for the RA and the SA. The FA profiles don't depend on the classification method at all.