Response of the low- to mid-latitude ionosphere to the geomagnetic storm of September 2017
- 1Theoretical Physics Division, PINSTECH, Nilore, Islamabad, Pakistan
- 2Department of Physics, Quaid-i-Azam University, Islamabad, Pakistan
Correspondence: Nadia Imtiaz (email@example.com)
We study the impact of the geomagnetic storm of 7–9 September 2017 on the low- to mid-latitude ionosphere. The prominent feature of this solar event is the sequential occurrence of two SYM-H minima with values of −146 and −115 nT on 8 September at 01:08 and 13:56 UT, respectively. The study is based on the analysis of data from the Global Positioning System (GPS) stations and magnetic observatories located at different longitudinal sectors corresponding to the Pacific, Asia, Africa and the Americas during the period 4–14 September 2017. The GPS data are used to derive the global, regional and vertical total electron content (vTEC) in the four selected regions. It is observed that the storm-time response of the vTEC over the Asian and Pacific sectors is earlier than over the African and American sectors. Magnetic observatory data are used to illustrate the variation in the magnetic field particularly, in its horizontal component. The global thermospheric neutral density ratio; i.e., O∕N2 maps obtained from the Global UltraViolet Spectrographic Imager (GUVI) on board the Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) satellite are used to characterize the storm-time response of the thermosphere. These maps exhibit a significant storm-time depletion of the O∕N2 density ratio in the northern middle and lower latitudes over the western Pacific and American sectors as compared to the eastern Pacific, Asian and African sectors. However, the positive storm effects in the O∕N2 ratio can be observed in the low latitudes and equatorial regions. It can be deduced that the storm-time thermospheric and ionospheric responses are correlated. Overall, the positive ionospheric storm effects appear over the dayside sectors which are associated with the ionospheric electric fields and the traveling atmospheric disturbances. It is inferred that a variety of space weather phenomena such as the coronal mass ejection, the high-speed solar wind stream and the solar radio flux are the cause of multiple day enhancements of the vTEC in the low- to mid-latitude ionosphere during the period 4–14 September 2017.
It is well known fact that the geomagnetic storm is a temporary variation of the Earth's magnetic field induced by the coronal mass ejection (CME) or the high-speed solar wind stream (HSSWS). The most widely used indices and parameters to study the physical processes occurring during the geomagnetic storms are the disturbance storm-time (Dst) index, the SYM-H index, the Kp index, the Ap index and the Bz component of the interplanetary magnetic field (IMF) (Rostoker, 1972; Gonzalez et al., 1994; Fares Saba et al., 1997). On the basis of different values of the Dst index and the Bz component of the IMF, the geomagnetic storms can be categorized as follows: weak or minor storms ( nT, nT for 1 h), moderate storms ( nT, nT for 2 h), intense storms ( nT, nT for 3 h) and severe storms ( nT) (Gonzalez et al., 1994; Loewe and Prolss, 1997). Some scientists prefer to use the SYM-H geomagnetic index in place of the Dst index due to its 1 min time resolution compared to the 1 h time resolution of the Dst index (Wanliss and Showalter, 2006). Also the 3 h value of the Kp index can be used for the classification of the geomagnetic storms as follows: weak or minor storms (), moderate storms (Kp≥6), intense storms () and severe storms (Kp≥8) (Gosling et al., 1991).
During the geomagnetic storms, the ionosphere features also vary along the latitudes and longitudes due to different current systems flowing in the magnetosphere. The physical processes such as the mass transport, prompt penetration of the magnetospheric electric field (PPEF) and an ionospheric disturbance dynamo electric field (DDEF) are the common features of the magnetic storms. A number of models have been utilized to investigate the role of these physical processes in the observations of the global magnetic perturbations (Blanc and Richmond, 1980; Fejer et al., 1983; Vasyliunas, 1970). Some theoretical studies are devoted to understanding the thermal expansion of the thermosphere due to the transport of energy and momentum from the auroral region to the midlatitudes to low latitudes during a magnetic storm. These studies highlighted the importance of the season and the local time at the beginning of the storm (Fuller-Rowell et al., 1994, 1996). Sharma et al. (2011) investigated the low-latitude ionosphere total electron content (TEC) response to the geomagnetic storm of 25 August 2005. On the day of the storm, a doubly humped peak in the TEC with an amplitude that is almost twice that of a quiet day value is observed. The first peak is attributed to the PPEF; however, the second peak is due to the plasma fountain effect. It is also found that the effect of the PPEF is almost uniform along the longitudinal direction. Thomas et al. (2013) studied the storm-time TEC variations in the mid-latitude northern American sector. It is observed that the storm-time ionosphere response is season dependent; i.e., the storms occurring in the summer have a large negative effects while the winter events have a strong initial positive phase with the minimum negative storm effects. Moreover, the events occurring in the fall and spring have almost the same effects. Many studies have analyzed the St. Patrick's day storm (the largest geomagnetic storm of the solar cycle 24) by using the TEC data analysis techniques derived from the Global Positioning System (GPS) to understand the positive and negative ionospheric-storm effects due to the energy transfer between the solar wind and the magnetosphere (Fagundes et al., 2016; Nayak et al., 2016). In this context, Nava et al. (2016) investigated the low and mid-latitude ionospheric response to the St. Patrick day storm of 2015. The storm effects are characterized by using the global electron content (GEC) and regional electron content (REC) in different longitudinal sectors such as the Pacific, Asia, Africa and the Americas. The authors observed a strong enhancement of the vertical total electron content (vTEC) in the American sector. It is also found that the Asian sector shows a comparatively large decrease in the vTEC. They also used the spectral analysis of the magnetometer data to separate the effects of the convection electric field and of the disturbance dynamo. Zhang et al. (2018) analyzed this event by using the GPS data of the Crustal Movement Observation Network of China. It is found that during the sudden storm commencement (SSC) phase, a rapid enhancement in the ionospheric electron density distorts the structure of the northern equatorial ionization anomaly (EIA) region. It is also observed that during the main phase a significant decrease in the vTEC occurs at the high-latitude region as compared to the low-latitude region. Moreover, the height of the peak electron density in the F2 layer also increases during the geomagnetic storm. Watson et al. (2016) presented a study based on the data of about 17 geomagnetic storms of the solar cycle 24 with nT to identify the solar sources of these geomagnetic storms. It is found that the low geomagnetic activity is associated with the weak dawn-to-dusk solar wind electric field. The authors have shown that the slow CME plays a main role in the commencement of the geomagnetic storms of the solar cycle 24. Kashcheyev et al. (2018) have made a comprehensive analysis on the basis of the two great geomagnetic storms ( nT) which occurred on 17 March and 22 June 2015. It is found that the absence or presence of a scintillation in the African sector is associated with the local time at the beginning of the storm. Another finding is that the summer storm results in the formation of the plasma bubbles which propagate up to the midlatitudes and cause strong scintillation in the Global Navigation Satellite System (GNSS) signals. Based upon this comprehensive analysis, the authors suggested that a number of factors such as the local time at the commencement of the storm and the season play an important role in the modeling of the ionosphere response to the solar activity. Blagoveshchensky and Sergeeva (2019) presented a study based on multi-instrument analysis to reveal the variation in the ionospheric parameters during the geomagnetic storm of 6–10 September 2017. The present work aims at investigating the response of low-latitude to midlatitude ionosphere to the large geomagnetic storm of 6–9 September 2017. The storm effects are analyzed by using the data from the individual GNSS receivers and ground magnetic observatories located in different longitudinal sectors. The approach used in the present study is similar to that used by Nava et al. (2016) and Kashcheyev et al. (2018). In addition, the storm-time response of the neutral atmosphere in the thermosphere is analyzed by using the global O∕N2 density ratio maps derived from the Global UltraViolet Imager (GUVI) on board the Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) satellite. The remainder of this article is organized in the following manner: Sect. 2 presents a description of data sets used in our analysis. Section 3 briefly describes the case study that is the solar event under investigation and its characterization on the basis of the global plasma parameters. In Sect. 4, we present results and a general discussion of our findings. Finally, the summary and conclusion of this study is presented.
Here we present the characteristics of the solar event along with the data sets that have been used in this study.
For solar event characterization, the relevant information is provided by the National Oceanic and Atmospheric Administration (NOAA) Space Weather Prediction Center (SWPC). According to NOAA SWPC, a number of space weather events were observed between 4 and 14 September 2017. The detailed description of these events is also given by Redmon et al. (2018). Here we give an overview of these solar events. Several X-class and M-class solar flares along with the CMEs occurred during this period. On 6 September, the sun emitted X2.2 and X9.3 solar flares at 08:57 and 11:53 UT, respectively. On 7 September, the two solar flares M7.3 and X1.3 are emitted at 10:11 and 14:20 UT, respectively. On 8 September 2017, the M8.1 solar flare is fired off at 15:35 UT. On 12 September, the X8.3 solar flare is emitted at 15:35 UT. The associated earthward CMEs have induced the geomagnetic storms of different intensities in early September 2017.
The solar wind parameters and IMF have been obtained from the OMNI database (https://omniweb.gsfc.nasa.gov/form/dx1.html, last access: 20 April 2019). The information about the Bz component of the IMF and the solar wind speed (Vsw) is provided by the NASA Advanced Composition Explorer (ACE) satellite.
The world data center for Geomagnetism (Kyoto) provides information about different geomagnetic indices, among them are AE, Ap, Kp and SYM-H indices. The AE index is a proxy of the auroral electrojet enhancement which estimates the energy transfer from the solar wind to the auroral ionospheric regions. Both the Ap and Kp indices quantify the disturbance in the horizontal component of the Earth's magnetic field, and the SYM-H index measures the intensity of the storm-time ring current (Rostoker, 1972; Wanliss and Showalter, 2006).
For ionospheric electron density variation, the data sets of the nine GPS stations are analyzed here. These stations are selected on the basis of data availability and their geographic and geomagnetic locations. The geographic and geomagnetic locations of these stations are given in Table 1. Our analysis is based on the four different longitudinal regions: the Pacific (180–120∘ W; 150∘–180∘ E), Asia (60∘–150∘ E), Africa (30 W–60∘ E) and the Americas (120∘ W–30∘ E). In order to analyze the diurnal variation of the vTEC in different longitudinal sectors, the relevant data with 2 h time resolution have been extracted from the IGS Global Ionosphere Map (GIM) data, available in the IONEX format (ftp://cddis.gsfc.nasa.gov/gps/products/ionex/, last access: 20 April 2019). The tomographic kriging GIMs computed by the Technical University of Catalonia (UPC) have been used to study the global electron content (GEC) variations during the storm period under consideration. The GEC is the total number of electrons present in the near-Earth space environment. The GEC is obtained from the UPC GIM data by the summation of the vTEC values in a cell Il,m multiplied by a cell's area Sl,m over all GIM cells and it is given by Afraimovich et al. (2006),
In Eq. (1), the symbols l and m represent the latitude and longitude of a certain GIM cell, respectively. The latitudinal and longitudinal extent of the elementary GIM cell is 2.5∘ and 5∘, respectively. The unit of GEC is 1 GECU=1032 electrons. The regional electron content (REC) is the total number of electrons in the specified region of the ionosphere. The REC is calculated similarly to the GEC, with the summation being restricted to the GIM cells of that particular region. For both GEC and REC, the UPC GIM data at the time resolution of 15 min have been used.
The storm-time magnetic field variations are analyzed by using the data obtained from the magnetic observatories located along the geomagnetic equator in the three longitudinal sectors: Asia (Kourou, KOU), Africa (M'Bour, MBO) and the Americas (Guam, GUA). The quasi-definitive data of these observatories available at http://intermagnet.org (last access: 10 September 2019) have been used for the analysis. Table 2 shows the geographic and geomagnetic locations of these observatories. In order to calculate the magnetic field variations, we have adopted the approach of Nava et al. (2016) and Kashcheyev et al. (2018). A brief description of this approach is given here. During the geomagnetic storm, the horizontal component H of the Earth's magnetic field can be expressed as follows (Le Huy and Mazaudier, 2005):
where Ho represents the magnetic field produced in the Earth's core and crust, SR is the quiet daily variation of the Earth's magnetic field given as , DM is the disturbance which comes from the magnetospheric currents due to the Chapman–Ferraro current, the ring current and the tail current (Cole, 1966), and Diono represents the magnetic field variations due to the disturbed ionospheric currents.
In order to estimate Sq, the average value of ΔHi is computed from 1 min time resolution values of the five quietest days in September 2017 by using the following expression:
where j is a day number, n is the total number of quiet days and with i=1 to 1440 min. The baseline value Ho is an average of hourly values at midnight (LT) and it is computed as follows:
The corrected hourly solar quiet variation in H that is Sq(H) can be given as follows:
here i=1 to 1440 min.
The DM can be estimated by using the dayside SYM-H index in the following expression:
where ϕ is the geomagnetic latitude.
here ΔH is the variation of the H component of the magnetic field.
The global thermospheric column density O∕N2 ratio can also serve as a sensitive indicator in the upper atmosphere for the disturbances induced by geomagnetic storms (Yuan et al., 2015; Wang et al., 2018). These maps are obtained from the GUVI and TIMED covering the days 5, 8 and 11 September 2017.
In early September 2017, the three CMEs with earthward trajectories are emitted on 4, 6 and 10 September. A CME originating from the massive X9.3 solar flare of 6 September reached the Earth at 23:00 UT on 7 September. The arrival of this CME caused a significant disturbance in the magnetosphere which leads to a severe geomagnetic storm with a maximum value of the geomagnetic index of . However, the arrival of the other two CMEs on 6 and 12 September leads to minor geomagnetic storms of G1 category (Kp<3). Figure 1 illustrates the global morphology of these solar events. In Fig. 1, the storm-time variations of the various interplanetary plasma and magnetic field parameters are depicted in the following order (from top to bottom): the Bz component of the IMF, the solar wind speed (Vsw), the Ey component of the interplanetary electric field (IEF), the solar radio flux F10.7, the SYM-H index, the AE index and the Kp index. The three vertical lines represent the arrival of the CMEs on Earth which lead to the SSC at 23:43, 23:00 and 20:02 UT on 6, 7 and 12 September, respectively, as reported by http://www.obsebre.es/php/geomagnetisme/vrapides/ssc_2017_d.txt (last access: 20 April 2019). However, the present study is focused on the effects of the G4 category storm which occurred on 8 September 2017. On the arrival of the interplanetary shock on 7 September at about 23:00 UT, the initial phase of the storm begins with rapid variations in the abovementioned parameters. During the main phase, the Bz component of the IMF is more southward, reaching the maximum lowest value of about −32 nT at 00:00 UT, and then it rapidly increases to the value of approximately +16 nT. The Bz becomes southward again by performing a negative excursion of −17.6 nT at 11:55 UT and remains southward until 13:56 UT. Afterward, the Bz component decreases gradually and stays around 0 nT from 9 to 12 September. It can be seen that on 8 September, the Vsw also exhibits an abrupt change by attaining the maximum value of about 820 km s−1 around 02:00, and after 12:00 UT it gradually decreases. The Ey component of the IEF calculated as also exhibits noticeable variations during the storm period. It depends on the Bz component of the IMF and the X component of the Vsw. It means that the positive northward IMF leads to the westward IEF on the dayside and the eastward field on the nightside. It can be seen that the Ey fluctuations occur between −15 and +20 mV m−1 during the storm. The next plot illustrates the behavior of the solar radio flux F10.7. The solar flux fluctuates significantly during the period 4–14 September 2017. In order to analyze the geomagnetic activity behavior, the SYM-H index is also presented in Fig. 1. During the main phase of the storm, the SYM-H index decreases and reaches the negative value of nT, thus producing the first minima of the SYM-H index at 01:08 UT. During the partial recovery phase from 01:08 to 11:00 UT, the SYM-H also increases from −146 nT to the value of −38 nT. Thereafter, the SYM-H index decreases again and it reaches the second minimum value of nT. This is the end of the main phase of the storm which lasted for ∼15 h. The main phase can be characterized by the occurrence of the two pronounced minima of the SYM-H with values −146 and −115 nT at 01:08 and 13:56 UT, respectively, on 8 September 2017. The recovery phase started after 13:56 UT on 8 September, the SYM-H increases slowly and returned to its normal value at 14:00 UT on 11 September. It can be seen that the recovery phase lasted for about 3 d.
The next two plots represent the AE and Kp indices. The AE index shows several peaks during this period. After the arrival of the first CME, there is an increase in the auroral activity such that the AE index reaches the peak value of about 1430 nT on 7 September at 09:07 UT. However, the occurrence of the two strong peaks with AE>2000 nT indicates that the most intense auroral activity occurred after the arrival of the second CME. The Kp index shows the two episodes of the maximum value of approximately between 00:00–03:00 and 12:00–15:00 UT on 8 September.
In this section, we present the variations in the variety of parameters such as the GEC, the REC, the vTEC, the H component of the magnetic field and the thermosphere neutral composition as a result of the G4 category geomagnetic storm of 7–9 September 2017. Figure 2 shows the ΔGEC (a), the ΔREC (b) and the SYM-H index (c) during the period 4–14 September 2017. Both the ΔGEC and ΔREC are calculated by subtracting the quiet-time variation from the value itself. The quiet-time variation is computed by using the three quiet days before the storm on which the Kp index below 4. The quiet days considered are 2, 3 and 4 September 2017. It can be seen that the ΔGEC shows two positive peaks at 01:08 and 13:56 UT corresponding to the first and second minima of the SYM-H index, respectively. In order to find the region which contributed to the peaks in the ΔGEC, the ΔREC is plotted for the four longitudinal sectors: the Pacific, Asia, Africa and the Americas. It can be seen that during the period 4–14 September 2017, the ΔREC varies significantly over the four longitudinal sectors. The observed behavior of the ΔREC can be attributed to the energy inputs from the solar wind to the magnetosphere (Nava et al., 2016). The AE index, which is an indicator of the energy transfer from the solar wind to the magnetosphere, is shown in Fig. 1. It can be seen that the AE index shows several episodes of the energy inputs (having AE>1000 nT) which occurred on 4, 7, 8 and 13 September. In response to these energy inputs, the amplitude and the occurrence time of the maxima and minima of the REC also vary.
Our analysis shows that the first peak in the GEC is due to the Asian and Pacific sectors and the second peak is due to the African and American sectors. Some authors have analyzed the variations of the GEC with the 10.7 cm solar radio emission, i.e., F10.7 index (Nava et al., 2016). In order to see the effect of the F10.7 index on the GEC, the fourth plot illustrates the variation of the F10.7 index during the period 4–14 September 2017. It can be seen that the F10.7 index is higher than 100 sfu between 4 and 8 September, as shown in Fig. 1. During this period, the higher value of the ΔGEC can be seen, which decreases significantly after 9 September, as illustrated in Fig. 2. According to Afraimovich et al. (2007, 2008) and Nava et al. (2016), there is a correlation between the GEC and the F10.7 index. Therefore, it can be inferred that the variation of the GEC from 4 to 8 September can also be affected by the higher solar flux, i.e., F10.7>120 sfu.
The nine plots in Fig. 3 illustrate the variation of the vTEC for the individual station of the three longitudinal sectors, i.e., Asia, Africa and the Americas, from 4 to 14 September 2017. In Fig. 3, the plots from one to three represent the stations of the Asian sector (i.e., BJFS, BAKO and YAR2), the plots from four to six represent the African sector (i.e., NOTI, NKLG and WIND), and the plots from seven to nine represent the stations of the American sector (i.e., BOGT, AREQ and ANTC). On each plot the vTEC is displayed in red and the quiet-time daily variations in blue. The quiet-time daily variations are computed by averaging the quiet-time data of the five days before the storm. These quiet days are chosen on the basis of having minor level geomagnetic activity, with a Kp index below 4. The following pertinent features of the vTEC can be noticed:
An enhancement in the vTEC is observed for all the stations in the three longitudinal sectors on the day of the storm. The three stations in the Asian sector exhibit an increase in the vTEC at the beginning of 8 September. However, the stations in the African region show the increasing trend of the vTEC in the middle and American stations on late 8 September. The variability in the occurrence of the vTEC peaks depends on the local time of the SYM-H minima at these stations.
On the day of the storm, the northern and southern midlatitude stations (BJFS and YAR2) in the Asian sector show an increase in the vTEC. However, in the equatorial station (BAKO) a relatively smaller increase in the vTEC is observed.
In the African region, the largest increase in the vTEC is observed for the equatorial and southern midlatitude stations (NKLG and WIND) during the storm. However, a small increase in the vTEC can be seen in the northern midlatitude station (NOTI) in this sector.
In the American sector, the largest increase in the vTEC is observed for the equatorial station BOGT during the storm period. It can also be seen that the vTEC decreases significantly for this station after the day of the storm. Both the southern midlatitude and equatorial trough stations ANTC and AREQ depict the multi-peak structures of the vTEC on the day of the storm. On the day after the storm, the ionization disappears at the southern midlatitudes and the vTEC returns to its quiet value.
Figure 4 illustrates the variation of the vTEC as a function of time and latitude over the four longitudinal sectors that are the Pacific (first plot), Asia (second plot), Africa (third plot) and the Americas (fourth plot). These vTEC plots are extracted from the IGS GIM data which are available in the IONEX files for the entire globe. For a fixed longitude, a vTEC map covering the latitudinal range of −90 to 90∘ can be plotted. The longitudes considered are given as 150∘ E for the Pacific, 110∘ E for Asia, 10∘ E for Africa and 70∘ E for the Americas. The vTEC maps shown in Fig. 4 cover the period from 4 to 14 September 2017 and the latitudinal range from −90 to +90∘. The SYM-H index over this period is also shown at in Fig. 4e. As mentioned earlier, the space weather conditions during this period are highly disturbed due to multiple events such as the CMEs and HSSWS. As a result of these space weather events, the vTEC maps of the four longitudinal sectors also show dramatic variation with the following features:
During geomagnetically quiet conditions, the vertical E×B drift at the dip equator lifts the ionospheric plasma upward. Under the influence of the gravitational and pressure gradient forces, the uplifted plasma can diffuse symmetrically with respect to the magnetic equator along the geomagnetic field lines like a plasma fountain. Therefore, the ionospheric electrodynamics generates the fountain effect which leads to the plasma density enhancement also known as the equatorial ionization anomaly (EIA) at ± 10–15∘ from the equator (Namba and Maeda, 1939; Balan and Bailey, 1995). As expected, in response to the geomagnetic storm the latitudinal extent of the EIA is increased up to about 30∘ latitude.
On 7 September, the observed vTEC enhancement in each sector can be associated with the impact of the first CME, which arrived at 23:43 UT on 6 September.
During the initial phase of the G4 storm on 8 September, the vTEC enhancement mainly occurred in the crest regions of the EIA with a clear latitudinal separation.
On the day of the storm, the vTEC was strongly enhanced in the crests of the EIA and in the magnetic equator region as compared to the days before and after the storm. The enhancements of the vTEC in the EIA region in response to the geomagnetic storms have been reported in many studies (Zhao et al., 2005; Astafyeva et al., 2015; Lei et al., 2018).
It can be clearly seen that the local dayside sectors such as Asia () and the Pacific () exhibit the largest increase in the vTEC on early 8 September, corresponding to the first SYM-H minima. However, at the time of the second minima the other two sectors, i.e., the Americas () and Africa (), are on the dayside and show the largest increase in the vTEC.
In the Asian sector, a regular pattern of the vTEC, which consists of well defined crests, can be observed on all days except the day of the storm. However, both the African and Pacific sectors show irregular patterns; i.e., sometimes one and sometimes two crests of the vTEC appear. During the recovery phase on 9 September, the vTEC returns back to its normal pattern. In the American sector, we mostly observed one crest of the vTEC and a very strong ionization on the day of the storm which returns to its normal level after the storm on 9 September.
The observed dayside positive storm phases can be explained on the basis of the two phenomena, i.e., the PPEF and the traveling atmospheric disturbances (TADs). The TADs originated from the polar regions due to a large amount of energy deposition from the magnetosphere during the storm period moving to the low latitudes and across the equatorial regions (Fuller-Rowell et al., 1994). The propagation of these TADs to the low latitudes and across the Equator can cause disturbance in the ionosphere by moving the plasma up and down along the magnetic field lines. According to Lei et al. (2018), the upward vertical E×B drifts are very strong between 01:00 and 14:00 UT on 8 September. These enhanced E×B drifts can be associated with the PPEF and the DDEFs driven by the thermospheric winds (Spiro et al., 1988; Blanc and Richmond, 1980). During the main phase of the storm, the upward drifts can shift the plasma to the higher altitudes where the chemical losses are very small and it can induce a super-fountain effect. On the other hand, the equatorward winds can inhibit the downward diffusion of plasma (Balan et al., 2010). The combined effect of the electric field and thermospheric wind can lead to the enhancement of the vTEC in the EIA. Besides these factors, the solar radio flux F10.7, which varies greatly during this period, can also affect the vTEC (Lei et al., 2018).
The three plots in Fig. 5 represent the magnetic field variations at the three equatorial magnetic observatories corresponding to the three longitudinal sectors of Asia (GUA), Africa (MBO) and the Americas (KOU). Each plot shows the variation in the H component of the magnetic field (in black), the quiet daily variation (Sq) (in blue) and the ionospheric disturbances (Diono) (in red). The three dashed lines correspond to the impact of the CMEs on 6, 7 and 12 September. The following features of the H component can be seen in all the three sectors:
Firstly, an increase in the H component occurs during the initial phase of the storm. This enhancement is due to the Chapman–Ferraro current resulting from the contraction of the magnetosphere (Chapman and Ferraro, 1931).
Secondly, a strong decrease in the H component can be observed during the main phase of the storms. It can be attributed to the diamagnetic behavior of the equatorial ring current. The enhanced ring current in the magnetosphere induced the magnetic field opposite to the Earth's northward dipole field, which strongly reduces the H component (Gonzalez et al., 1994).
Following the strongest decrease in the H component, the recovery phase started, which lasted for several hours. During the recovery phase, the ring current decays and the H component of the magnetic field returns back to the normal level.
Two pronounced dips in the H component at 01:08 and 13:56 UT on 8 September are observed in the three stations. It can be seen that the first dip (around 01:08 on 8 September) is strongly negative for both GUA (−142 nT) and KOU (−142.5 nT) as compared to MBO (−102 nT). However, the second dip (around 13:56 UT on 8 September) is strongly negative for MBO (−164 nT) as compared to GUA (−133 nT) and KOU (−112 nT). This behavior is due to the local time variation of the ring current during the storm.
Overall, the largest disturbance of the H component of the magnetic field is observed at MBO as compared to GUA and KOU.
The disturbance due to ionosphere electric current Diono is represented by the red curve in Fig. 5. It follows an anti-Sq signature during the storm period. It can be noted that during the first southward excursion of the IMF, the Diono decreases at GUA, which is in the noon sector. However, an increasing trend in the Diono is observed for MBO and KOU which are in the night sector. During the second southward excursion of the magnetic field, Diono decreases significantly for MBO and KOU, which are now in the dayside. The Diono contains signatures of the PPEF and DDEF therefore, the observed trend of the Diono can also be explained by these two electric fields (Kashcheyev et al., 2018).
Another effect that can be seen during the storm is the variation in the thermospheric neutral composition, i.e., the O∕N2 density ratio. It is well understood that the thermospheric composition plays an important role in the dayside ionospheric density variation. Under quiet conditions, the photoionization of the atomic oxygen and the chemical reaction of the molecular nitrogen N2 and oxygen ion O+ mainly control the ionospheric density. During the intense geomagnetic storms, a large number of oxygen atoms are ionized that leads to an increase in the ionospheric electron density along with the high O∕N2 density ratio. This in turn affects the ionospheric TEC and vTEC. The global view of the thermospheric O∕N2 ratio obtained from the TIMED/GUVI for the days before, during and after the storm of September 2017 is shown in Fig. 6. It is evident that a severe storm-time depletion of the O∕N2 ratio occurs in the higher latitudes while a significant enhancement in the O∕N2 ratio is observed in the lower latitudes and equatorial regions. The O∕N2 ratio is mainly controlled by the thermospheric neutral winds that are, in turn, related to the Joule heating in high latitudes. Therefore, the severe reduction of the thermospheric O∕N2 density ratio in the polar region is caused by the upwelling wind due to enhanced Joule and particle heating in the high latitudes. According to Yuan et al. (2015), the O∕N2 density depletion extends from the high- to mid-latitudes due to the expansion of the storm-induced heating zone, which causes upward flow of the heated N2-enriched air. The storm-time depletion of the O∕N2 ratio is found to extend to middle and lower latitudes over the North American and western Pacific sectors. On the other hand, the storm-time enhancement of the O∕N2 density ratio can be seen in the midlatitudes over the African, Asian and eastern Pacific sectors as compared to the quiet-time pattern. The storm-time longitudinal asymmetry of the ionospheric and thermospheric disturbances is associated with the asymmetric longitudinal distribution of the O∕N2 density ratio. Moreover, the asymmetric structure of the O∕N2 density ratio strongly depends on the location of northern and southern magnetic poles in different hemispheres (Wang et al., 2018; Fuller-Rowell et al., 1994). After the recovery of the storm on 11 September, the thermospheric composition returns to its normal profile. This observation is consistent with the behavior of the vTEC during the storm period.
We presented the impact of the geomagnetic storm of 7–9 September 2017 on the low- to mid-latitude ionosphere over the four longitudinal sectors, i.e., the Pacific, Asia, Africa and the Americas. The storm effects are characterized by using the diverse parameters including the global, regional and vertical total electron content derived from the GPS data, the geomagnetic field measured at the ground magnetic observatories and the thermospheric neutral composition obtained from the TIMED/GUVI instrument. It is observed that the positive storm effects occur in the local dayside stations. The temporal response of the four sectors shows that the positive storm effects in the REC and vTEC over the Asian and Pacific sectors are observed earlier than the American and African sectors. During geomagnetically quiet conditions, most of the TEC is confined to the equatorial and low-latitude regions. However, the latitudinal extent of the bulk of the TEC increases up to the midlatitudes during the storm period. The vTEC enhancements observed on the other days are due to the high-speed solar wind stream event. The analysis of the magnetometer data shows the largest disturbance of the horizontal component of the magnetic field occurred at MBO as compared to that of GUA and KOU. The storm-time variation of the horizontal component is associated with the Chapman–Ferraro and the ring currents. The magnetic field component associated with the disturbed ionospheric current follows the anti-Sq variations, which depend on the prompt penetration electric field and the disturbance dynamo electric field. On the day of the storm, the O∕N2 density ratio is larger than that in the quiet time over the low latitudes and equatorial region. However, the high- and mid-latitudes exhibit storm-time depletion of the thermospheric O∕N2 density ratio. The storm-time longitudinal asymmetric behavior of the thermosphere can also be observed in the lower and middle latitudes over the four sectors. It is found that the thermospheric O∕N2 density ratio in the lower and middle latitudes over the African, Asian and eastern Pacific sectors is larger than that it is observed over the American and western Pacific sectors. Moreover, the storm-time enhancement in the thermospheric composition (i.e., O∕N2 ratio) over the low latitudes and equatorial region is consistent with the observed vTEC behavior. Overall, the positive storm phase occurred on the dayside sectors during the G4 geomagnetic storm of 7–9 September 2017. It can be concluded that the thermosphere–ionosphere dynamics and electrodynamics play an important role in the observed perturbations in the low- to mid-latitude ionosphere during the geomagnetic storms of 4–14 September 2017. This study can be useful to understand the response of the low- to mid-latitude ionosphere during geomagnetic storms.
The information about the solar wind parameters for the characterization of the space weather events is provided by the Goddard Space Science Data Center through 1 min OMNI data that is available on https://omniweb.gsfc.nasa.gov/form/omni_min_def.html (Goddard Space Science Data Center, 2019). The information about the arrival of CMEs and resulting SSC is obtained from the Ebro Observatory via http://www.obsebre.es (Ebro Observatory, 2019). The information about the space weather events is provided by the National Oceanic and Atmospheric Administration Space Weather Prediction Center via ftp://ftp.swpc.noaa.gov/pub/indices/events/20170908events.txt (last access: 22 April 2019). The magnetic observatories data is made available by the International Real-time Magnetic Observatory Network via web http://www.intermagnet.org (International Real-time Magnetic Observatory Network, 2019). The global thermospheric composition maps are provided by the GUVI Data Processing Payload Operations Center that are available on http://guvitimed.jhuapl.edu/data_products (GUVI Data Processing Payload Operations Center, 2019).
The main idea of the collaborative work on the study of response of the low- to mid-latitude ionosphere to the geomagnetic storm of September 2017 was proposed by NI. WY as a MPhil student carried out this work under the supervision of NI and MK. The MATLAB codes used as a tool for the GPS and magnetic field data analysis were developed by WY with the help of MK. After cross checking the results, the paper was successfully prepared and defended by NI.
The authors declare that they have no conflict of interest.
The authors are grateful to the space weather data resources: the OMNI database https://omniweb.gsfc.nasa.gov/form/dx1.html (last access: 20 April 2019) for providing the solar wind data; the World Data Center for Geomagnetism at Kyoto University, Japan, for providing the geomagnetic data: http://wdc.kugi.kyoto-u.ac.jp/ (last access: 20 April 2019); and the International GNSS Service (IGS) team for providing the GPS data. Nadia Imtiaz acknowledges the UNOOSA/ICTP for providing the financial support to attend the GNSS workshop and learn these data analysis techniques. The authors are very grateful to the anonymous referees for their constructive and insightful comments for improving the paper. The authors would like to thank Anton Kashcheyev and Christine Amory Mazaudier for their valuable suggestions.
This research work was partly supported by the HEC Pakistan (grant no. 7632/Federal/NRPU/RD/HEC/2017).
This paper was edited by Georgios Balasis and reviewed by three anonymous referees.
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