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Seasonal variations of nighttime D-region ionosphere in 2013 solar maximum observed from a low-latitude station
Earth, Planets and Space volume 67, Article number: 163 (2015)
We present the observation of tweek atmospherics with harmonics m = 1–8 during the solar maximum year, 2013, at Tay Nguyen University, Vietnam (Geog. 12.65° N, 108.02° E). The analysis of 33,690 tweeks on ten international quiet days during 2 months each season, summer (May, August), winter (February, November), and equinox (March, September), shows that tweeks occur about 51 % during summer, 22 % during winter, and 27 % during equinox. The D-region ionosphere is more sharply bounded for harmonics m = 5–6 around an altitude of 85.5 km. The environment of the D-region is more inhomogeneous during winter and equinox seasons. The mean electron density varies from 28.4–225 cm −3, which corresponds to the harmonics m = 1–8 at the mean reflection height of 81.5–87.7 km. The results reveal that the lower reference height in our work as compared to other works is due to the higher level of solar activity. The equivalent electron density profile of the nighttime D-region ionosphere using tweek method during summer, equinox, and winter seasons shows lower values of electron density by 12–58 %, 3–67 %, and 24–76 % than those obtained using the International Reference Ionosphere (IRI-2012) model.
Collisions between charged and neutral particles dominate the physical interaction of the D-region ionosphere (∼60–90 km). These activities play an important role in the propagation of the extremely low frequency (ELF; 3–3000 Hz) and the very low frequency (VLF; 3–30 kHz) waves through the Earth-ionosphere waveguide (EIWG) (Hargreaves 1992; Kumar and Kumar 2013). By monitoring the ELF-VLF waves, Friedrich and Rapp (2009) showed that the nighttime D-region properties varies with zenith angle, solar flux, season, and latitude. The D-region ionosphere is too high for balloons and too low for the satellite measurements (Ohya et al. 2003). The attachment and recombination processes are too fast and that makes the free electron density very low (< 103 cm −3), especially in the nighttime. This inhibits the observability of the ionosondes and incoherent scatter radars (Hargreaves 1992). Rockets are used to measure the ionospheric parameters (Maeda 1971; Nagano and Okada 2000), but they are restricted by the timing of flights. Therefore, observing ELF-VLF from the ground is an effective tool to study the D-region ionosphere.
Lightning discharges emit ELF-VLF signals, which propagate into the EIWG and expose as “hooks” on the frequency-time spectrogram. They appear as chirping sounds on a loudspeaker. This type of sferics is called “tweeks” (Helliwell 1965; Yamashita 1978). Using the tweek method, many researchers have investigated the properties of the lower ionosphere. In the previous works, the first modes of tweeks are used to study the seasonal variations of the nighttime D-region ionosphere during the low solar activity period (Maurya et al. 2012a,b). However, the seasonal variation of those parameters at higher harmonics is poorly understood, which limits our view of the overall morphology of the low-latitude D-region.
We observed tweeks at Tay Nguyen university, Vietnam (Geog. 12.65° N, 108.02° E) during winter, equinox, and summer seasons of 2013 to calculate the cut-off frequency, reflection height, and electron density of the D-region ionosphere. From these parameters, we evaluate the morphology of this region. Our survey site is at low latitudes around the equatorial region, which is near the Asia Oceanic Region; hence, the lightning density is very high. This creates favorable opportunities to study the turbulence of the D-region using the ELF-VLF waves radiated by lightning. Furthermore, the observation period is during the high solar activity year of the solar cycle 24, which we expect that the D-region perturbs much more violently. We present our experiment and data analysis method in section “Experimental data and analysis”. In section “Results and discussion”, we will discuss the results obtained over the year 2013 and compare them with the International Reference Ionosphere (IRI-2012) model. Finally, we draw out conclusion in section “Conclusions”.
Experimental data and analysis
Our ELF-VLF receiver consists of a magnetic antenna, a preamplifier, an ADC (Analog to Digital Converter), a SU (Service Unit), a Global Positioning System (GPS) receiver, a PC, and recording software. The details of this receiver are described in our previous work (Tan et al. 2014). It has been developed to record the atmospheric signals. The antenna includes two orthogonal loops which are right isosceles triangles with the base of 2.6 m. Each loop consists of 8 turns of 18 American Wire Gause copper wire. The surface of one loop orients in the north-south (N-S) direction, while the surface of other loop orients in the east-west (E-W) direction. If the magnetic component of electromagnetic waves changes and passes the loop of antennas, a voltage will be generated in the coils of the antenna (Ramo et al. 1994). In order to minimize signal interference, the loops are wrapped with the silver shields. The plane of the antenna which is perpendicular to E-W is chosen because it is very sensitive to sferics generated by lightning discharges (Dahlgren et al. 2011; Wood 2004). The signals from antenna are amplified and filtered by a preamplifier near the antenna and then transmitted by the coaxial cable to the ADC at a distance of 150 m. The preamplifier is powered by a particular DC power supply to remove the AC noise. The ELF-VLF signals from the E-W channel of the preamplifier go into the sound card. The SpectrumLab v2.77b22 records the sferics with audio files having extension “wav.” The GPS is utilized for time synchronization with an accuracy of 100 ns. To record the sferics, SpectrumLab is configured with the sample rate of 44.1 kHz, 16-bit sampling, and fast Fourier transform (FFT) input size of 512. The Sonic visualiser software developed by Cannam et al. (2010) is used to analyze the audio files.
Figure 1 a–c shows the spectrograms on 22 February 2013 at 0:30 LT (local time (LT) = UT + 7 h), 13 March 2013 at 2:00 LT, and 15 May 2013 at 2:30 LT, respectively. Figure 1 shows the tweeks as the “hooks” appeared on the vertical lines. The third, fourth, and eighth harmonic tweeks clearly occurred on the spectrogram. The propagation of ELF-VLF waves in the EIWG is analyzed in term of quasi-transverse electric (QTE) and quasi-transverse magnetic (QTM) modes with the first mode cut-off frequency of about 1.8 kHz. The zero-order mode or quasi- transverse electromagnetic (QTEM) mode has the frequency components below the cut-off frequency of the first-order mode and its polarization is linearly polarized (Budden 1961; Hayakawa et al. 1994). The formation of tweeks near the mode cut-off frequency is examined by estimating the attenuation coefficient and excitation factor of waveguide for QTM and QTE modes (Yamashita 1978). For frequencies less than 15 kHz, the lower order QTM and QTE modes approximate pure TM and TE modes (Wood 2004). We therefore treat the modes in the EIWG as pure TM modes. The QTEM modes below the first mode cut-off frequency are shown in the spectrograms (Fig. 1). The broadband data are recorded for a duration of 2 min at every 15 min interval. The tweeks were recorded on ten international quiet days during 2 months each season: summer (May, August), winter (February, November), and equinox (February, September). Tweeks rarely appear during sunset, 10:00–12:00 UT (17:00–19:00 LT) and during sunrise, 22:00–24:00 UT (05:00–07:00 LT). Therefore, we consider only tweeks obtained during the period from 12:00–22:00 UT (19:00–5:00 LT). All clearly visible tweeks were selected with the intensity levels ≥ –35 dB as seen in the spectrogram. The cut-off frequency captured from tweeks during three seasons is used to estimate the parameters of the lower ionosphere.
We used the method of Ohya et al. (2003) to estimate the electron density of the nighttime D-region ionosphere via the following equation:
where f H is the gyrofrequency and f p is the plasma frequency. Considering the low-latitude (30° N-30° S) location of our site, we assume f H = 1.3 ± 0.16 MHz by using the IGRF (International Geomagnetic Reference Field) model. This result is consistent with the results calculated by Saini and Gwal (2005) and Kumar et al. (2009).
Assuming that f p <<f H and the wave experience of reflection, i.e. f c =f p , we obtain:
Substituting the value of f H in Eq. (2), we obtain:
The reflection height h of the EIWG is determined from the cut-off frequency for each mode as (Budden 1961):
where c is the speed of light in free space, m is the mode number and f cm is cut-off frequency.
where R is the radius of the Earth.
Equation (5) shows that as f reaches near f cm , v gm approaches zero, while as f becomes much larger than f cm , v gm approaches the speed of light. In the case of f is less than cut-off frequency, the radio wave is quickly attenuated along the propagation distance (Wood 2004).
The propagation distance of tweek sferics is obtained by (Ohya et al. 1981):
where t 2 - t 1 is the difference in arrival times of the two frequencies, f 2 and f 1, close to the tweeks of any mode, and v g f1 and v g f2 are the corresponding group velocities of the radio waves centered at frequencies f 1 and f 2.
The cut-off frequency captured from tweeks during three seasons is used to estimate the ionospheric refection height and D-region electron density at the reflection height. The arrival times t 1 and t 2 of two frequencies f 1 and f 2 closed to cut-off frequency from tweek spectrograms were measured to estimate the propagation distance of the tweeks. The frequency and time resolutions of measurement are 35 Hz and 1 ms, respectively. The estimated error in the reflection height is about 1.5 km for first-order mode, and it reduces with the increase in the modes. The errors in the electron density and propagation distance for all modes are found to be ∼ 0.6 cm −3 and ∼ 470 km, respectively.
Results and discussion
Tweek occurrence observed at low latitudes
Table 1 presents a total of 33,690 tweeks with m = 1–8 observed at Tay Nguyen University, a low-latitude site. Seven thousand four hundred fourteen (22 %), 8974 (27 %), and 17302 (51 %) tweeks were captured during winter, equinox, and summer seasons, respectively. We found that the mean tweek’s duration varies from 8–43 ms. Maurya et al. (2012a) found that tweek duration is about 8–48 ms for tweeks observed at the other low-latitude stations, Allahabad and Nainital (India). Kumar et al. (2008) recorded tweeks at Suva (Fiji) and estimated the duration of tweeks varies from 15–60 ms. Our results on the mean tweek’s duration show lower than those reported by those authors because our survey site is located in the Asian storm center; hence, many sources of tweeks are around the station. The higher harmonic tweeks often occurred during summer season, whereas lower harmonic tweeks mainly occurred during equinox and winter seasons (Table 1). The occurrences of different harmonic tweeks are not much different between pre-midnight and post-midnight (Table 2). During winter season, the second harmonic tweeks are most popular (50 %). During equinox season, the third harmonic tweeks dominate (34 %). During summer season, the fifth harmonic tweeks are most often (27 %). In all cases, the higher harmonic tweeks occurred rarely, especially eighth harmonic tweeks. Kumar et al. (2008) found that the attenuation of ELF-VLF waves in the D-region increases for the higher modes. Therefore, it suggests that the absorption of the D-region is stronger for higher modes during winter and equinox seasons as compared to that during summer season.
Figure 2 shows that most tweeks occurred with the propagation distance in the range of 2000–3000 km. The occurrence rate of tweeks with the propagation distance in the range of 1000–5000 km during equinox, winter, and summer seasons varies about 92, 89, and 92 %, respectively. Tweeks with the propagation distance in the range of 1000–2000 km occurred more often during summer as compared to those during equinox and winter. Observing tweeks at a low-latitude station, Kumar et al. (2008) reported that 90 % of tweek propagation distance are in the range of 1000–5000 km with maximum in the range of 2000–3000 km. Overall, our results in the tweek propagation distance are in accordance with those reported by Kumar et al.(2008). Maurya et al. (2010) and Kumar et al. (2008) found that the propagation distances are up to 12,000 km and also illustrated that the attenuation offered by EIWG is higher for tweeks with higher modes. Thus, these tweeks from propagating larger distance are limited. At our site, during the equinox, we can record a maximum propagation distance of 12,000 km. The majority of the direction of propagation of tweeks came from east to west, as most of tweeks came from over the sea which is in the east of our site. The propagation of ELF-VLF waves over the sea undergoes less attenuation as compared to that over the land (Ohya et al. 1981).
The variations of reflection height and fundamental frequency with mode number
We consider tweeks with the propagation distance less than 5000 km to avoid the errors caused by the daytime propagation path particularly for tweeks coming from East to West directions (Maurya et al. 2012a). Table 3 gives an example of calculation (see also Fig. 1). The results show that the reflection height (h) varies from 70.3–83.2 km, the electron density (n e ) changes in the range of 29.4–234.7 cm −3, and the mean fundamental frequency (f cm /m) varies within 1.8–2.1 kHz. In addition, the propagation distance (d) varies from 648–3553 km.
From Fig. 3 a, it can be seen that the mean h during winter, equinox and summer seasons varies between 84.2–87.0 km, 83.9–87.6 km and 84.3–86.4 km, respectively. Overall, the mean h during three seasons increases sharply from m = 1 to m = 4, then stays constant up to m = 5, and increase linearly to m = 8. The mean h increases as the harmonics of tweeks increases, which means that the higher harmonics of the same tweeks penetrate deeper into the nighttime lower ionosphere while reaching to the receiving station by multiple reflections (Kumar et al. 2008). Tweeks are reflected at the altitudes where the plasma frequency equals the individual cut-off frequency of each harmonic, and therefore the waves with the higher harmonics are reflected at higher altitude due to the plasma frequency is higher (Shvets and Hayakawa 1998). We fit a linear function to the mean reflection height and mode number relation. The trend of variation of h with mode number for winter is h winter = 0.50 m + 83.0 with R 2=0.83, for equinox is h equinox=0.56 m + 82.8 with coefficient of determination R 2=0.94, and for summer seasons is h summer = 0.18 m+84.7 with R 2=0.49. The slope of the linear function is lower during summer season (0.18) as compared to that during winter (0.50) and equinox (0.56) seasons. Figure 3 a shows that tweeks with m = 5 and 6 are reflected at the same altitude for all seasons. Theoretically, for a waveguide with perfectly conducting boundaries, the higher modes can be reflected at the same altitude. Since the conductivity of the boundary is not perfect, the higher modes are reflected at the higher altitude (Maurya et al. 2012a). Therefore, the D-region ionosphere is less inhomogeneous for harmonics m = 5–6 around an altitude of 85.5 km.
Figure 3 b shows the variation of f cm /m with the harmonics m. It reveals that f cm /m during winter, equinox and summer seasons slightly reduces from 1.81–1.72, 1.81–1.71, and 1.79–1.74 kHz, respectively. The trend of reduction of f cm /m with mode number for winter is f winter=−11.60m+1816 with R 2=0.85, for equinox is f equinox=−13.08m+1823 with R 2=0.96, and for summer is f summer=−5.17m+1782 with R 2=0.58. The variation of f cm /m is less steep during summer season as compared to that during winter and equinox seasons.
Morphology of nighttime D-region ionosphere
Each panel in Fig. 4 presents the temporal variation of the reflection height with different harmonics. The mean h varies from 81.5 to 87.7 km for m = 1–8. The mean value of n e increases from 28.4–225.0 cm −3 in the altitude range of 81.5–87.7 km. During winter season (February and November), the variation of h makes a dip around 22:00 LT and has a crest around 3:00 LT, and then it slightly decreases. During summer (May and August), the temporal variation of h has the crest around 20:30 LT and reduces to the dip from 1:00–2:00 LT and then increases. During equinox season, the h decreases from 19:00–23:00 LT for March 2013 and increases from 19:00–21:00 LT for September 2013. The trend of the variation of h on panels (a) and (c), (b) and (d), and (e) and (f) is nearly symmetric. In other words, there is the near opposite of reflection height variation between the two seasons. The differences of h for higher harmonics during summer season are not significant (Fig. 5). This reveals that the D-region is more delicate and homogeneous during summer as compared to that during winter and equinox seasons.
To present the seasonal variation of h for different modes, the data was smoothed by using the Adjacent-Averaging method with 5 points of window (Fig. 5). In the pre-midnight, the h for m = 1–6 is higher during summer season as compared to that during winter and equinox seasons. In the post-midnight, the seasonal variation of h for m = 2–3 is not significant, and the h for m = 4–6 is lower during summer season as compared to that during winter and equinox seasons. The trend of variation of h for the first harmonic is not clear because lower harmonics may interfere with AC noise. The increase of h at nighttime corresponds to the decrease of electron density due to its loss by the attachment and recombination processes. The scattered Lyman- α is an important source of the D-region ionization. Ohya et al. (2011) found that about 67 % of the nighttime D-region ionization is caused by Lyman- α and Lyman- β which ionize NO and O2 at altitude of 95 km. The lower h in the pre-midnight period during winter as compared to equinox and summer seasons is explained by the fact that the lower n e of daytime during winter giving rise to slower the loss processes of electrons in the pre-midnight period (Maurya et al. 2012b). Those phenomena clearly show at lower altitudes of the D-region. The h for m = 4–6 in the post-midnight period is higher during winter and equinox seasons as compared to that during summer season. It can be explained that tweek with higher modes could reflect at the less different altitudes because the D-region during summer season becomes less inhomogeneous. Around 19:00 LT, the tweek reflection height during winter season is higher than that during summer for m = 3–4. The higher h of winter after sunset transition could be caused by lower daytime n e during winter season.
Recording tweeks with a maximum up to the eighth harmonics from January–April, 1991 (R z =140), Shvets and Hayakawa (1998) calculated h which varies from 81–83 km. Capturing tweeks with m = 1–6 during the period of September, 2003–July, 2004 (R z =45) at Suva (Geog. 18.2° S; 178.3° E), Kumar et al. (2008) found that h varied from 83–92 km. At a low-latitude station, Allahabad (India), Maurya et al. (2012a) observed tweeks with m = 1–6 from April, 2007 (R z =7.5) to March 2008 (R z = 2.9), the mean h increased from 80–95 km. In our work, the mean h varies from 81.5–87.7 km, which is higher than that reported by Shvets and Hayakawa (1998), but lower than that shown in the results of Kumar et al. (2008) and Maurya et al. (2012a). Shvets and Hayakawa (1998) indicated that when the Sun ,s activity decreases hence the reflection height increases. Bremer and Singer (1977) and Danilov (1998) also illustrated that the Sun ′s activities affect the electron density of the nighttime D-region. Surveying the seasonal variation of tweek reflection height over three solar cycles, Ohya et al. (2011) found that the reflection height was relatively low in March–April and high in July–October.
The seasonal variation of Wait ′s parameters and electron density profiles
Using first three modes of tweeks, Kumar et al. (2009) and Maurya et al. (2012a) calculated the reference height (h ′) and sharpness factor (β) by using the Wait ′s formula. Maurya et al. (2012a) used two tweeks in 1 min at each 15 min interval during pure nights from 21:00–02:00 LT of 2010, meanwhile, Kumar et al. (2009) used tweeks in 5 min at each hour interval during nights from 21:00–03:00 LT. In present work, we use the previous method of Kumar et al. (2009) and Maurya et al. (2012a) to obtain h ′ and β. We calculated the mean h and n e of the first three harmonics of tweeks recorded in 2 min at every 15 min interval. We analyzed tweeks in August, September, and November of 2013, as representative of summer, equinox, and winter seasons. Tweeks having d less than 5000 km observed from 21:00–02:00 LT are chosen, so that the error contribution due to in the pre-midnight period, some tweeks coming from dayside part (from west side of the station) and in post-midnight period, some tweeks coming from dayside part (from east side of the station) is avoided.
In Table 4, results reveal that h ′ during winter, equinox, and summer seasons varies between 82.2–86.9 km with a mean value of 84.4 ± 1.5 km, 81.1–86.9 km with a mean value of 83.7 ± 1.5 km, and 81.2–87.5 km with a mean value of 83.3 ± 1.8 km, respectively. The β during winter, equinox, and summer seasons varies between 0.49–0.65 km −1 with a mean value of 0.57 ± 0.07 k m −1, 0.46–0.66 km −1 with a mean value of 0.55 ± 0.06 km −1, 0.43–0.66 km −1 with a mean value of 0.55 ± 0.06 km −1, respectively. The h ′ is lower during summer season as compared to that during winter and equinox season. The β is higher during winter season as compared to that during summer and equinox seasons.
Observing tweeks at Allahabad, India (16.05° N) during the low solar activity period, Maurya et al. (2012a) found that the mean h ′ during winter, equinox, and summer seasons are 85.9, 85.7, and 83.5 km, respectively, and the mean β during winter, equinox, and summer seasons are 0.51, 0.54, and 0.61 km −1, respectively. In our work, the mean h ′ during three seasons is lower by 0.2–2.2 km than that reported by Maurya et al. Our mean β is higher by 0.06 and 0.01 km −1 during winter and equinox seasons but lower by 0.06 km −1 during summer season than those reported by Maurya et al. (2012a), respectively. Cummer et al. (1998) observed sferics at mid-latitude of 37.43° N in July 1996 (R z =10) and used the Long Wave Propagation Capability (LWPC) program to calculate h ′ and β with 83.3 and 0.49 km −1, respectively. Using LWPC modeling of amplitude and phase of VLF signals, Thomson et al. (2007) studied the nighttime mid-latitude D-region near solar minimum and estimated the Wait’s parameters of h ′=85.1 km and β=0.63 km −1. Cheng et al. (2006) recorded sferics during 16 nights of summer season at Duke (36° N) and found that h ′ and β varied from 83.6–85.6 km and 0.4–0.5 km −1, and the mean h ′ and β are 84.5 km and 0.45 km −1, respectively. Our results on h ′ during summer are lower than those reported by those authors.
Figure 6 presents the seasonal variation of electron density profiles obtained by different methods. In order to plot the electron density from the IRI model, we selected five quiet days corresponding to five observing nights during August, September, and November of 2013 and obtained the n e in the altitude range of 80–100 km at the midnight (0:00 LT). The values of n e calculated by tweek method during summer, equinox, and winter seasons are lower by 12–58 %, 3–67 %, and 24–76 % than those obtained by IRI-2012 model, respectively, and show a good comparison with IRI-2012 in the altitude ranges of 82–89 km, 87–92 km, and 88–93 km for summer, equinox, and winter seasons, respectively. Observing the nighttime D-region during March–December 2006 at Suva (18.2° S 178.3° E) Fiji, Kumar et al. (2009) found that the values of n e obtained by tweek method are lower by 20–45 % at altitudes 82–86 km than those obtained by IRI2001 model. Observing tweeks during 2010 (R z =16.5), Maurya et al. (2012a) found that the n e of the nighttime lower ionosphere shows lower by 5–60 % than that obtained using IRI-2007 model at low-latitude stations and also concluded that tweek method shows significant seasonal variation in n e , whereas IRI-2007 model does not have any significant seasonal variation. Our results in the values of n e of the electron density profile at the altitude range of 80–88 km during summer season show a good comparison with results reported by Maurya et al. However, the values of n e in our results during winter and equinox seasons are significantly higher by 3–26,841 cm −3 and 7–23,818 cm −3 than those found by Maurya et al. (2012a). This explains that the higher solar activity increases the electron density, and hence, decreases the reference height of the nighttime D-region. We also found that the deviations of n e between summer and winter vary from 7–9912 cm −3 and 6–94,449 cm −3 for our result and Maurya et al. ′s result, respectively. The deviations of n e between summer and equinox vary from 3–9167 cm −3 and 6–90681 cm −3 for our result and Maurya et al. ′s result (Maurya et al. 2012a), respectively. This is probably due to the variation of Galactic Cosmic Rays in different solar periods. Thomson et al. (2012a) reported that GCRs is another important source of ionization of the nighttime D-region, which has nearly half of the ionization rate of Lyman- α at 85 km altitude. The intensity of GCRs is the highest during solar minimum and the lowest during solar maximum (Badhwar and O’Neill 1996). The seasonal variation of electron density profile in the study of Maurya et al. (2012a) shows more significance. The period of study of these authors is under solar minimum; GCRs are important ionizing source and their variation at different season caused the D-region electron density variation (Maurya et al. 2012a). Ohya et al.(2007) indicated that GCR ionization is less intense under solar maximum conditions and the decrease of GCRs due to high solar activities may cause the decrease in the electron density in the D and lower E region of the ionosphere. Since the period of our study is during strong solar activity period of solar cycle 24, the GCRs are not important for the ionization of the nighttime D-region ionosphere. Therefore, the seasonal variation of nighttime D-region electron density due to the variability of GCRs is not significant.
Recording the tweeks with harmonics m = 1–8 at Tay Nguyen University, Vietnam (Geog. 12.65° N, 108.02° E), we have found some new rules of the seasonal occurrences of tweeks as well as the seasonal variation of parameters of the nighttime D-region low-latitude ionosphere.
Tweeks occur about 51 % during summer season, 22 % during winter season, and 27 % during equinox season. Tweeks with m = 4–8 occur more often during summer season as compared to winter and equinox seasons.The occurrence rate of the tweeks with the propagation distance in the range of 1000–5000 km during equinox, winter, and summer seasons are 92, 89, and 92 %, respectively. The boundary of the waveguide becomes more sharp for tweeks with m = 5–6.
The mean n e increases from 28.4–225.0 cm −3 which corresponds to h of 81.5–87.7 km. During winter season, the variation of h makes a dip around 22:00 LT and has a crest around 3:00 LT and then slightly decreases. During summer season, the temporal variation of h has the crest around 20:30 LT and reduces to the dip from 1:00–2:00 LT and then increases. The h decreases from 19:00–23:00 LT for March and increases from 19:00–21:00 LT for September. The trend of the variation of h between 2 months which are in different seasons is nearly symmetric.
The h corresponding to higher harmonics (m = 4 – 6) in the post-midnight is higher during winter and equinox seasons as compared to summer season because n e is lower during winter and equinox seasons than that during summer season. At the higher altitudes, the D-region becomes less inhomogeneous during summer season as compared to that during other seasons; hence, the tweeks with higher modes during summer season could reflect at the less different altitudes, whereas those tweeks during winter and equinox seasons could reflect at the higher altitudes.
The mean h ′ during winter, equinox, and summer seasons are 84.4, 83.7, and 83.3 km, respectively. The β during winter, equinox, and summer seasons are 0.57, 0.55, and 0.55 km −1, respectively. The h ′ during summer season is lower in our work as compared to other works due to the higher level of solar activity.
The values of n e calculated by tweek method during summer, equinox, and winter seasons are lower by 12–58 %, 3–67 %, and 24–76 % than those obtained using the IRI-2012 model, respectively, and show a good comparison with IRI-2012 in the altitude ranges of 82–89 km, 87–92 km, and 88–93 km for summer, equinox, and winter seasons, respectively. The seasonal variation of the electron density profile during solar maximum period shows less significant than that during solar minimum activity period.
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The authors are grateful to Department of Physics, Faculty of Natural Science and Technology, Tay Nguyen University for their encouragement and support.
LMT analysed the tweek data and and drafted the manuscript. NGT participated in the sequence alignment. TQH participated in explaining the physics processes of the ionosphere and gave many suggestions. QNL participated in the design and coordination and helped to draft the manuscript. All authors read and approved the final manuscript.
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Tan, L.M., Thu, N.N., Ha, T.Q. et al. Seasonal variations of nighttime D-region ionosphere in 2013 solar maximum observed from a low-latitude station. Earth Planet Sp 67, 163 (2015). https://doi.org/10.1186/s40623-015-0331-y
- Local Time
- Winter Season
- Summer Season
- Propagation Distance
- Solar Maximum