Introduction

Scintillation of transionospheric radio signals is a consequence of electron density irregularities that may occur within the ionosphere and is characterized by rapid fluctuations in the amplitude and phase of these signals when they pass through the ionosphere (Kintner et al. 2001). The occurrence of scintillation shows considerable spatial and temporal variability, with dependence on local time, season, latitude, solar and geomagnetic activity. The global morphology of ionospheric L-band scintillation occurrence is presented in Basu et al. (2002), which reports that scintillation occurrence is strong over the equatorial latitudes extending from 20°N to 20°S geomagnetic latitudes, moderate to strong over the high latitudes extending from 65° to 90° geomagnetic latitudes and almost absent over the midlatitudes. The midlatitude ionosphere is generally considered to lack the necessary processes required to generate the irregularities causing scintillation and hence is regarded as a less scintillation active region. However, Maruyama (1990) has shown that over the midlatitudes, the ExB instability can be excited when a significantly strong eastward electric field is present, giving rise to intense irregularities and L-band scintillation.

A number of midlatitude scintillation studies have been carried out mainly using the VHF radio transmissions from geostationary satellites, as lower frequencies are more severely affected (Kersley et al. 1980; Hajkowicz and Minakoshi 2003). Using a 5-year data set from 150 MHz radio transmissions, Hajkowicz (1994) reported that localized midlatitude scintillation patches frequently occur during sunspot minimum, in association with the occurrence of midlatitude spread F. The observations of L-band scintillation at midlatitudes are mostly reported during severe geomagnetic storms (Ogawa and Kumagai 1985; Bust et al. 1997; Ma and Maruyama 2006) and during the equatorward movement of the ionospheric trough along with a storm time-enhanced density (SED) (Ledvina et al. 2002). Using the data from a geostationary satellite over Japan, Fujita et al. (1982) reported that the scintillation activity at 1.7 GHz is enhanced at night in June. Otsuka et al. (2006) carried out a statistical study on the latitudinal dependence of the irregularity characteristics over Japan by using total electron content (TEC) data obtained from the Global Positioning System (GPS) network in Japan during 2000. Their study revealed that at the midlatitudes, i.e., between 29 and 38°N, scintillation occurrence is highest during summer nighttime. A climatological study on the midlatitude (50–51°N geographic latitude) ionospheric quiet time disturbances based on 10 years of GPS data in Belgium revealed that the occurrence of summer night time disturbances is lower than that of their winter day time counterparts (Wautelet and Warnant 2014). The results from this study showed that the winter day time disturbances correspond to the classical medium scale traveling ionospheric disturbances (MSTIDs), exhibit properties matching the results reported in the literature (Tsugawa et al. 2007), whereas the summer night time disturbances correspond to non-classical MSTIDs of electrical origin. The origin of these two types of disturbances were further investigated in Wautelet and Warnant (2015), which showed that summer night time disturbances were related to the spread F phenomenon, linked to the appearance of sporadic E (Es) layers. In the United Kingdom (UK), Aquino et al. (2005) reported on the occurrence of GPS L1 phase scintillation recorded by the GPS NovAtel GSV4004B scintillation monitor receiver at the midlatitude station of Nottingham, corresponding geographic latitude and longitude of 52.95oN and 1.18oW, during the severe geomagnetic storm of November 6, 2001. They also reported on strong correlation between high levels of phase scintillation and positioning accuracy degradation at the same station during the Halloween storm of October 2003.

The observation of moderate amplitude scintillation on the GPS L1C/A signal recorded by a Septentrio PolaRxS receiver on a geomagnetically quiet day at the midlatitude station of Nicosia in Cyprus, is presented and discussed. The geographic latitude and longitude of Nicosia are 35.14°N and 33.48°E, respectively, and the corresponding geomagnetic latitude is 31.79°N. The next section describes the data and the method of analysis. The results and discussions are then presented in the subsequent section. Finally, the conclusions are presented in last section.

Data and methodology

A Septentrio PolaRxS GNSS receiver (Septentrio PolaRxS application manual 2010) was deployed in Nicosia under the UK Engineering and Physical Sciences Research Council (EPSRC) funded “Polaris” project (http://www.bath.ac.uk/elec-eng/polaris/) and has been routinely collecting ionospheric scintillation data since December 2011. This study is based on the analysis of one-minute scintillation indices, namely S4 and σ φ, recorded on the GPS L1C/A signal during June 11–13, 2014. The amplitude scintillation index, S4, is the standard deviation of the received signal power normalized by its mean value and the phase scintillation index, σ φ, is the standard deviation of the detrended carrier phase computed over 60 s, using a filter of 0.1 Hz cutoff (Van Dierendonck et al. 1993). Also, the S4 recorded on the L1 frequency by the EGNOS (European Geostationary Navigation Overlay Service) satellites is used. A satellite elevation angle cutoff of 20° is applied in order to reduce the impact of non-scintillation-related errors, e.g., induced by multipath. In order to investigate the presence of electron density gradients leading to the occurrence of scintillation, the Slant TEC (STEC) values recorded by the receiver at every minute interval are used to estimate the Rate of TEC (ROT), i.e., temporal change in STEC. The latitude and longitude of the ionospheric pierce point (IPP) for the different ray paths have been calculated assuming a thin single shell ionospheric model at an altitude of 350 km (Ciraolo and Spalla 1997).

In addition, data obtained from three GNSS receivers of the International GNSS Service (IGS) network is also used, in order to identify the presence of electron density irregularities. The approximate geographic and geomagnetic coordinates of these receivers are listed in Table 1. The data from the geodetic receiver at Nicosia are also used in the analyses to confirm the presence of irregularities recorded by the PolaRxS receiver. For the study, the data from station “Nama” represent the anomaly crest, while the data from “Haly” and “Nico” represent the locations beyond the anomaly crest. The RINEX observation files recorded by these receivers are processed to estimate the uncalibrated STEC values every 30 s for each ray path with elevation angle greater than 20°. The rate of TEC index (ROTI), defined as the standard deviation of ROT (Pi et al. 1997), is then computed over 5-min intervals to identify the presence of large-scale electron density irregularities.

Table 1 GNSS receiver type, geographic and geomagnetic coordinates of the station locations
Full size table

The data acquired by the GPS Occultation Experiment (GOX) on the COSMIC (Constellation Observing System for Meteorology, Ionosphere, and Climate) satellite for the same period, downloaded from the COSMIC Data Acquisition and Analysis Center (CDAAC) web site (http://cosmic-io.cosmic.ucar.edu/cdaac/login/cosmic/), has also been used to confirm the L-band scintillation occurrence. This data are composed of “scnLv1″ files containing the 1 s S4 index calculated on the GPS L1C/A code (1.575 GHz), along with the signal-to-noise ratio on the L1C/A channel (caL1_SNR), produced for each observation and occultation of the GPS satellites observed by COSMIC (Carter et al. 2013). The values of S4max9s, defined as the 9 s average of the S4 values surrounding the time of maximum S4 (S4max) recorded in each occultation event, were extracted from these files. Along with the S4max9 s, the values of the alttp S4max, lcttp S4max, lattp S4max and lontp S4max were also extracted, which represent, respectively, the altitude, local time, latitude, and longitude of the occultation tangent point at the time the maximum S4 was measured.

To complement the data from the GNSS receivers, the ionograms, skymaps and drift velocities recorded at every 5 min by the DPS-4D digisonde operating at Nicosia are used. The Nicosia digisonde is a state-of-the-art ionosonde which performs optimal ionogram recordings based on the digisonde Precision Group Height Measurement (PGHM) technique (Reinisch et al. 2005) and ionospheric “drifts” using Doppler interferometry (Reinisch et al. 1998). The skymap is an interpretation view of the interferometry technique employed in digisonde to resolve individual echoes from the ionosphere (‘sources’) in terms of their position and velocity and therefore useful in providing direct confirmation for the presence of ‘sources’ in oblique directions.

The ionogram observations during June 11–13, 2014, are also analyzed based on the height–time–reflection intensity (HTI) methodology that is analogous to the technique producing range–time–intensity (RTI) radar displays within a given interval of time. The HTI technique is described in detail in Haldoupis et al. (2006) and in Lynn et al. (2013). In brief, this method considers an ionogram as a “snapshot” of reflected intensity as a function of height and ionosonde signal frequency, and uses a sequence of ionograms to compute, for a given frequency bin, an average HTI plot, i.e., a 3-D plot of reflected signal-to-noise ratio in dB as a function of height within a given time interval.

The characterization of the geomagnetic conditions during this period is performed using the planetary geomagnetic activity index Kp, the disturbance storm time index Dst, and the auroral electrojet index AE, obtained from the World Data Center for Geomagnetism, Kyoto (http://wdc.kugi.kyoto-u.ac.jp/).

Results and discussions

Figure 1 shows the variations of the indices Kp (top), AE (middle) and Dst (bottom) during June 11–13, 2014. The 3-hourly Kp index is noticeably low during this period, reaching a maximum value of 2+ on June 11. The one-minute AE index is also generally low, and only few high values (>400 nT) are observed on that day. However, according to Prölss (1993), these are not large enough to trigger intense substorms. The hourly Dst index does not show high variability and the values fluctuate between +10 nT and −10 nT, suggesting that the disturbances are too small to be considered as a geomagnetic storm. The Dst reaches values close to +30nT during the late evening hours on June 13. Altogether, these variations in the Kp, AE and Dst indices suggest that this period is characterized by quiet geomagnetic conditions.

Fig. 1
figure 1

Variation in the 3 hourly Kp (top), 1 min AE (middle) and 1 h Dst (bottom) indices during June 11–13, 2014

Full size image

GNSS measurements

The variations in the amplitude and phase scintillation indices, S4 and σ φ, recorded by the PolaRxS receiver on the GPS L1C/A signal during June 11–13, 2014, over Nicosia are shown in Fig. 2. From this figure, moderate levels of amplitude scintillation, characterized by 0.3 < S4 < 0.7 (Alfonsi et al. 2011), can be observed during 20:00–24:00 UT on June 12. The corresponding σ φ values are much lower, with maximum values around 0.3. For the GPS L1 frequency, the most effective spatial size of the electron density irregularities that causes amplitude scintillation is the first Fresnel scale, which corresponds to about 330–400 m when the altitude of the ionospheric F-region is about 300–400 km. Thus, the L-band moderate amplitude scintillation occurrence on the night of June 12, as observed in Fig. 2, indicates the presence of electron density irregularities at hundred-meter scale sizes.

Fig. 2
figure 2

Variation in the S4 and σ φ indices recorded on the GPS L1C/A signal over Nicosia during June 11–13, 2014

Full size image

In order to obtain an insight on the prevailing electron density gradients leading to the occurrence of scintillation, the variations in S4 (top) and ROT (bottom) are shown in Fig. 3 for 6 satellites in view during 20:00–24:00 UT on June 12. It can be observed that higher S4 values occur in correspondence with the steep electron density gradients indicated by the large variations in ROT. The high S4 values and varying ROT are mainly observed for the 4 satellites SV03, SV16, SV19, and SV27.

Fig. 3
figure 3

S4 (top) and ROT (bottom) variations during 20:00–24:00 UT on June 12, 2014

Full size image

In order to investigate the geographic location of the electron density irregularities leading to the scintillation occurrence, Fig. 4 shows the S4 variations as a function of IPP latitude and longitude for individual satellite-receiver links during 20:00–24:00 UT. The location of the receiver at Nicosia is shown as a red circle in the figure. The satellite corresponding to each IPP trace is labeled as “SV” followed by the satellite number. The ‘+’ sign indicates the initial location of the satellite. It can be observed from this figure that high S4 values are located within the latitudinal band of about 28–35°N and correspond only to satellites traveling southwards, namely SV03, SV16, SV19, and SV27, of the receiver location. Northward traveling satellites, i.e. SV22 and SV14, do not record any significant S4 values. On comparing the temporal and spatial variations in S4, as shown in Figs. 3 and 4 respectively, an eastward propagation of the irregularities can be observed.

Fig. 4
figure 4

IPP tracks shaded with the S4 index as indicated in the color bar, for individual satellite-receiver links during 20:00–24:00 UT on June 12, 2014

Full size image

To further ascertain the propagation direction and to determine the approximate zonal drift velocity of the irregularities, the temporal variations of S4 recorded on the L1 frequency by two EGNOS geostationary satellites, SES-5 and Inmarsat 4-F2, are shown in Fig. 5. The EGNOS SES-5, namely PRN136, is located at 5°E with a satellite elevation angle of 39°. The corresponding IPP latitude and longitude are 32.552°N and 30.957°E, respectively. The Inmarsat 4-F2, namely PRN126, is located at 25°E with a satellite elevation angle of 48°. The corresponding IPP latitude and longitude are 32.626°N and 32.743°E, respectively. This combination of two geostationary satellites to estimate the zonal drift velocity has been used due to the absence of multiple zonally separated ground receivers, which would provide the ideal configuration (Ledvina et al. 2004). Though the S4 values along the two satellite-receiver links (PRN136 and PRN126) have been recorded by the same GNSS receiver at Nicosia, different regions of the ionosphere were probed due to the difference in the viewing geometry. The occurrence of scintillation on PRN136 (red line) precedes that on PRN126 (blue line), as the former is located west of the latter, clearly indicating the eastward propagation of the irregularities. As the two satellites are located along nearly the same IPP latitude, the longitudinal separation of the IPP points would correspond to the zonal separation. This distance along with the time lag between two nearby identifiable features, around 21:00 UT on PRN136 and around 22:00 UT on PRN126, yields an eastward component of the irregularity drift velocity as about 49 m/s.

Fig. 5
figure 5

S4 as observed by PRN136 (red) and PRN126 (blue) on June 12, 2014

Full size image

Past research has shown that the apparent eastward zonal drift velocity of the plasma bubble peaks around 20:00–21:00 LT with average values of 150–200 m/s. After 22:00 LT, a gradual decrease in the zonal drift velocity from 100 to 200 m/s to below 50 m/s after local midnight is reported (Ji et al. 2015). The estimated drift velocity of about 49 m/s is observed around 22:00 UT, corresponding to the local midnight hours (LT = UT + 2.25 h) and thus matching the expected values.

An analysis of the scintillation data recorded by the COSMIC satellite on June 12 showed an S4max9 s value of 0.49 around 18:36 UT during an occultation event on GPS satellite SV25. Figure 6 shows the temporal variations in the 1 s S4 and L1 SNR. Fluctuations in the SNR along with high values of S4 can be clearly observed from this figure, indicating scintillation occurrence. The observed value of S4max is 0.787 at a tangent latitude and longitude of 26.1°N and 29.1°E, respectively. The corresponding tangent point altitude was 386 km, thus indicating the presence of electron density irregularities in the F-region (Carter et al. 2013). The scintillation observation from the COSMIC data further confirmed the presence of F-region irregularities on the night of June 12.

Fig. 6
figure 6

Temporal profile of the 1 s S4 scintillation index (top) and SNR (bottom) of the LEO-GPS link on June 12, 2014

Full size image

The observed scintillation on the night of June 12 can be attributed to an extension of the equatorial plasma bubbles or to locally generated irregularities. The Perkins instability is widely considered as the most likely mechanism for the generation of F-region irregularities over the midlatitudes and is known to cause oscillations in the TEC (Perkins 1973). On the other hand, the equatorial plasma bubbles can rise to high apex height and extend to higher latitudes by diffusing along the magnetic field lines (Huang et al. 2007). The presence of equatorial plasma bubbles can be identified from the TEC variations as they manifest as depletions in TEC and characterized by sudden reduction in TEC followed by a recovery to the level of TEC preceding the reduction. Therefore, TEC variations will provide an invaluable insight on the possible source of the observed irregularities causing scintillation.

Figure 7 shows the variations in STEC (red) along with the S4 (black) for four satellite-receiver links, namely SV03, SV16, SV19 and SV27, at Nicosia, which recorded moderate scintillation. It can be observed from the figure that scintillation occurrence is coincident with TEC depletion and that these are observed on both the east as well as the west walls of the depletion. The increased S4 values at the depletion walls are most likely to be caused by the larger background electron density at the walls as opposed to the lower electron density in the interior of the depletion. An interpretation of the above observation along with the observed propagation direction (eastward) in Figs. 4 and 5 suggests that the possible source of the observed irregularities is an extension of the equatorial plasma bubbles.

Fig. 7
figure 7

Time variations in S4 (black) and STEC (red) along 4 different satellite-receiver links

Full size image

In order to better understand the presence of electron density irregularities, Fig. 8 shows the temporal variations in the ROTI values, estimated from the three receivers listed in Table 1, during 16:00–24:00 UT on June 11 (top), June 12 (middle), and June 13 (bottom). The IPP latitudes in geomagnetic coordinates are shown in the color bar. The ROTI values have been estimated using data at a sampling rate of 30 s and hence ROTI values >0.5 TECU/min can only be used to indicate the presence of large-scale electron density irregularities with scale lengths of a few kilometers (Pi et al. 1997; Basu et al. 1999).

Fig. 8
figure 8

Temporal variations of ROTI on June 11 (top), 12 (middle) and 13 (bottom) of 2014. Color bar show the IPP geomagnetic latitudes in °N

Full size image

From Fig. 8, ROTI values greater than 0.5 TECU/min are observed during 17:30–18:30 UT on June 12 around 0–20°N geomagnetic latitudes, indicating the presence of large-scale irregularities near the anomaly crest. Such an enhancement in the ROTI values is not observed on June 11 or 13. This indicates that the background electrodynamic/neutral dynamic conditions on the night of June 12 were significantly different from those observed on the previous/next day. Similarly, enhanced ROTI with values greater than 1 TECU/min are observed during 20:00–23:00 UT around 20–40°N on June 12. ROTI values in the same range are observed on June 11 and 13; however, the maximum latitudinal extent of the observed irregularities is shorter, i.e., only around 10–30°N. An interesting feature to note from the figure is that on June 12, ROTI values even greater than 3 TECU/min are observed around 30–40°N during 22:00–23:00 UT, which coincides with the time when moderate L-band scintillation was recorded on SV27 (refer to Fig. 3). Thus, the presence of large-scale irregularities with a large latitudinal extension on the night of June 12 is confirmed from Fig. 8.

An interesting observation from Fig. 3 is that the presence of irregularities was first detected on SV16 at an IPP geographic latitude of about 32°N and geomagnetic latitude of about 25°N, corresponding to an apex height of about 1850 km at the geomagnetic equator. Simulations using the mean flux tube density model by Mendillo et al. (2005) have shown that density depletions associated with Equatorial Spread F (ESF) can easily reach altitudes above 2000 km in the equatorial plane. There have also been several observations showing that the ESF density depletions can reach very high altitudes, in some cases as high as 2500 km. However, these observations refer to times of strong geomagnetic storms, when the F-region plasma has been lifted considerably (Ma and Maruyama 2006; Huang et al. 2007). This is the first observation of an equatorial bubble reaching altitudes as high as 1850 km on a geomagnetically quiet day. As the upward velocities produced by the pre-reversal enhancement (PRE) over the equatorial latitudes during the summer months are smaller than those during the equinoxes, the probability of equatorial irregularities reaching apex heights of about 1850 km on a geomagnetically quiet day during the month of June is very low.

The irregularities observed over the midlatitude station of Nicosia are connected through the magnetic field lines to around 1850 km over the geomagnetic equator in the African longitude sector. Limited studies have been carried out in this sector as compared to the Asian/South American sector. Paznukhov et al. (2012) reported on the longitudinal, seasonal and local time occurrence of equatorial plasma bubbles and L-band scintillation over equatorial Africa during the solar minimum year of 2010. They have shown that over the East African longitude (about 40°E), shallower plasma bubbles are observed even during the summer solstice, a result that was consistent with the DMSP (Defense Meteorological Satellite Program) satellite observations reported in Gentile et al. (2006). Further to this, using ROCSAT-1 (Republic of China Satellite) data at 600 km, Su et al. (2006) have shown that the occurrence of topside equatorial plasma density irregularities over the African longitudinal sector is more prominent during the two equinoxes as well as the June solstice. Our observation of a plasma bubble reaching the midlatitudes is therefore quite consistent with these results.

The background ionospheric conditions on the night of June 12 are also investigated using the digisonde data from Nicosia and are presented in the next section.

Ionosonde measurements

It has been extensively reported in the literature that, at midlatitudes, scintillation occurrence is usually associated with the appearance of Range Spread F (RSF) on ionograms, which is identified as ‘spread’ in the F-region trace height due to irregular structures in electron density. Such irregular structures have been attributed to F-layer altitude modulation by large-scale atmospheric gravity waves (Bowmen 1990) and to electrodynamic forces and large-scale plasma instabilities (Miller et al. 1997). The sequence of ionograms on June 11 and 12 recorded by the digisonde at Nicosia between 18:40 and 23:25 UT is shown in Figs. 9 and 10 respectively. The x axis is the frequency in MHz, and the y axis shows the virtual height in km.

Fig. 9
figure 9

Sequence of ionograms recorded by the DPS-4D ionosonde on June 11, 2014, over Nicosia. The x axis is the frequency in MHz and the y axis shows the virtual height in km

Full size image
Fig. 10
figure 10

Sequence of ionograms recorded by the DPS-4D ionosonde on June 12, 2014 over Nicosia. The x axis is the frequency in MHz and the y axis shows the virtual height in km

Full size image

The spread in the F-region trace, indicating the occurrence of RSF, during 22:10–23:25 UT on June 12 is very clear from Fig. 10. Such a spread in the F-region trace is not observed in Fig. 9, indicating the absence of RSF on June 11. It is well known that ionosonde observations are sensitive to electron density irregularities with scale sizes of the order of kilometers, so the gradual development of RSF on June 12, as observed on the ionograms, indicates the presence of irregularities of those scale sizes. The sequence of ionograms in Fig. 10 also shows a semi-transparent Es layer at 18:40 UT, when it can be observed at an altitude of 100 km. Between 19:50 and 22:10 UT, the Es layers have disappeared and range spread in the F-layer started to develop. On comparing Figs. 3 and 10, it can be observed that there is a difference in time when the L-band scintillation was first observed on SV16 at around 20:30 UT and when the RSF was observed on the ionograms, i.e., around 22:10 UT. This time difference is attributed to the fact that the GNSS receiver can monitor a wider ionospheric region as compared to the digisonde and therefore detects the presence of irregularities earlier. The digisonde detects the irregularities only after they have drifted to its field of view. Furthermore, a simultaneous occurrence of scintillation and RSF can be observed at about 22:10 UT, indicating the presence of hundred-meter- as well as kilometer-scale-size irregularities. This corroborates the earlier observation that these two scale size irregularities generally coexist, due to the fact that diffusion can induce an earlier decay of the smaller scale size irregularities (Rodrigues et al. 2004).

Figure 11 presents the variations in the F-region zonal drift velocity estimated from the digisonde during June 11–13, with positive values indicating eastward drifts. East–west drift velocities exceeding values of 40 m/s during 20:00–24:00 UT on June 12 can be clearly observed from this figure, indicating a strong eastward drift of the irregularities. Two distinct peaks in the drift velocity, with values of about 57 m/s at 19:48 UT and about 74 m/s at 22:22 UT, respectively, are observed. This is in agreement with the estimated velocity and propagation direction based on GNSS measurements as discussed earlier.

Fig. 11
figure 11

East–west F-region drift velocities recorded over Nicosia during June 11–13, 2014

Full size image

Figures 12, 13 and 14 illustrate three skymaps on the night of June 12 displaying the reflection points in the F-region within a cone of 40° around the zenith and with concentric circles at 10o intervals. The color bar indicates the Doppler frequency in Hz and the ‘+’ and ‘o’ symbols indicate positive and negative values of the frequency, respectively. The direction of the arrows in Figs. 12, 13 and 14 represents the dominant direction of the plasma motion in the horizontal plane, while the size and shape of the arrows is analogous to the magnitude of the plasma drift velocity. If the ionosphere is smooth and horizontally stratified, the skymaps will show a single source location at zero zenith angle. However, in the presence of horizontal gradients/tilts, the ‘sources’ will align along the direction of the gradient. The skymap at 21:33 UT, presented in Fig. 12, shows ‘sources’ with a negative Doppler frequency (o symbols) up to 10° zenith angle. The frequency and range span of these sources vary between 5.6–5.95 MHz and 317–330 km, respectively. The total number of sources was 205, and the center of the sources was about at zenith 3° and azimuth −87°. There is only a very small deviation from zero zenith angle, which indicates that during this time; the horizontal gradients/tilts in the ionosphere were very small.

Fig. 12
figure 12

Skymap over Nicosia on June 12, 2014, at 21:33 UT. The direction and size/shape of the arrows indicate that during this time, the resultant plasma motion was eastward with a small magnitude

Full size image
Fig. 13
figure 13

Skymap over Nicosia on June 12, 2014, at 21:58 UT. The direction and size/shape of the arrows indicate that during this time, the resultant plasma motion was eastward with an increasing magnitude

Full size image
Fig. 14
figure 14

Skymap over Nicosia on June 12, 2014, at 22:13 UT. The direction and size/shape of the arrows indicate that during this time, the resultant plasma motion was eastward with a high value

Full size image

The skymap at 21:58 UT, presented in Fig. 13, shows two sets of ‘sources’, one between 30° and 40° zenith angle with a positive Doppler (+ symbols) and the other between 5° and 15° zenith angle with a negative Doppler (o symbols). The total number of sources was 243, and the frequency and range span of these sources vary between 3.6–3.95 MHz and 280–305 km, respectively. During this time, the center of the ‘sources’ was about at zenith 18° and azimuth −82°. This deviation from zero zenith angle indicates the presence of horizontal gradients in the ionosphere, and the resultant azimuth of the ‘sources’ can be observed to be aligned along the east–west direction, which is typical of the magnetic field aligned irregularities.

The skymap at 22:13 UT, presented in Fig. 14, shows the situation after the RSF development. ‘Sources’ can be identified up to 10° zenith angle with both positive and negative Doppler (+ and o symbols). The frequency and range span of these sources vary between 5.6–5.95 MHz and 317–330 km, respectively. The total number of sources was 663, and the center of the sources was about at zenith 3° and azimuth −102°. The resultant azimuth is still aligned along the east–west direction. Thus, the skymap at 21:58 UT, i.e., just before the onset of RSF, on the night of June 12 indicates the presence of magnetic field aligned irregularities, typically associated with equatorial plasma bubbles.

Figure 15 is a HTI plot during June 11–13, 2014 considering 5-min ionogram traces received within the frequency range 1.5–3.5 MHz with the color scale varying from strongest (red) to weakest (blue) signals. HTI maps show the intensity of the reflected signal as a function of time and altitude. The small black dots indicate points where the signal reflection strength maximizes. From Fig. 15, variations in the F-region height can be clearly observed during 02:00–06:00 UT and during 14:00–24:00 UT. On June 11 and 13, the F-region height variations are smooth and the reflected signal is from virtual heights close to 300–350 km. During 22:00–24:00 UT on June 12, the HTI map is spread over a large F-region altitude range and the reflected signal intensity is greater than -1.5 dB, clearly showing the development of RSF. This large altitudinal spread in the HTI map is due to multiple reflections between the F2 layer peak and the ground, as the signal is very strong and indicates the presence of irregularities. A remarkable characteristic identified around this time is the periodic descend of reflections (as represented by the black dots) between 400 and 300 km. This feature can be attributed to off-angle reflections from electron density depletions and can be interpreted as an approaching ionospheric instability which caused the ionospheric F2 region to break up into spread F (Lynn et al. 2011).

Fig. 15
figure 15

Digisonde HTI maps recorded over Nicosia during June 11–13, 2014

Full size image

The results presented above indicate that under suitable background ionospheric conditions, equatorial plasma bubbles can map to very high altitudes and cause moderate amplitude L-band scintillation over the midlatitudes even during periods of quiet geomagnetic activity.

Conclusions

An insight on the observations of moderate GPS L1 amplitude scintillation over the midlatitude station of Nicosia, Cyprus, on a geomagnetically quiet day is presented. The scintillation data were recorded by a Septentrio PolaRxS GNSS scintillation monitor receiver. The high S4 values observed on the night of June 12, 2014, were found to correspond with large variations in ROT, indicating the presence of steep electron density gradients. The STEC and S4 variations indicate the presence of electron density depletions accompanying scintillation occurrence. The apparent horizontal drift velocity and propagation direction of the irregularities were estimated as about 49 m/s and eastward, respectively, value and feature consistent with those of equatorial plasma bubbles. An interpretation of the above observation is that the possible source of the irregularities causing L-band scintillation is an extension of the equatorial plasma bubbles to apex heights of about 1850 km over the magnetic equator. The occurrence of scintillation was associated with the appearance of RSF on the ionograms recorded at Nicosia. The HTI plot and the skymaps generated using the ionogram data showed the presence of electron density depletions. The overall conclusion is that the midlatitude ionosphere may be more active than previously thought and that further studies on the implications of equatorial and low latitude ionospheric behavior are necessary. This is particularly relevant for the GNSS user community and related applications.