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New Releases. Regata OS The Regata OS is free and open source. Thanks to the community, it has evolved a lot. The eclipse conditions at the ground levels are shown in Fig. The central line of the eclipse totality path at ground level is shown in black colour. The global path of the central totality line at ground level is shown in Fig. The path of the totality at altitude km is shown with a continuous green line in Fig. The global path of the solar eclipse was from the South Pacific ocean, southern South America, and the South Atlantic region.
These results are provided in the supplementary information see Figs. The 12 GPS sites six sites from each side of totality lines shown in red-coloured filled circles are provided as supplementary information Fig S3. The details about the GPS sites and eclipse conditions at the ground level can be found in Table 1. Geographic map of Chile and the total solar eclipse on Dec 14, The orange color dots represent totality path at altitude km for the TEC analysis.
The blue dots represent the north GPS site of the totality and green color dots south of the totality. Inset A the path of the total solar eclipse central line on the world map. The Figure is prepared using the GMT 5. The GPS receivers collect dual-frequency signals operated at L1 The two pseudo-random numbers PRNs. PRN29 and PRN31 have been chosen based on their paths, elevation angle and duration suitable for eclipse analysis.
It is important to have a satellite covering a longer time before and after the eclipse and in the high elevation range to avoid the multipath and other signal diffraction phenomenon.
The red arrows in both Figs. The three days include eclipse day 14th December , the day before the eclipse 13th December , and the day after the eclipse 15th December Each plot is shown for 4 h duration i. The dashed grey vertical line on each subplot shows the maximum eclipse time and dim grey vertical dotted lines show the initial and ending of the solar eclipse. The GPS sites in each subplot of Fig. The GPS sites in totality region named with orange color.
Eclipse magnitude at each site added at the upper left corner. The grey dotted vertical line is showing maximum eclipse time at each site. This time approximates the local noontime at the Chilean GPS sites, which provides an opportunity to study ionospheric perturbation in the total solar eclipse effect during the peak of ionization.
Thus, present results further verified the delay time lag , which is very well reported in many previous works 16 , Figure 3 suggests that background TEC values are higher in the north of the totality path compare to the south. Hence, the higher values of TEC on the sites located north of the totality path most probably related to the low latitude of these sites.
Further, the percentage decrease in TEC on eclipse day with reference to mean of two days is also estimated for both PRNs and shown in Fig. As mentioned above, for PRN29, satellites path is along the totality path, thus observed almost constant totality effect for longer duration whereas, for PRN31, satellites path is across the totality path, and observe varying totality effect for comparatively short duration. This is also supported by timing of the maximum decrease in TEC and maximum eclipse timing at each site for both PRNs as discussed above.
The South American TSE provides a rare opportunity to investigate the significant role of eclipse generated AGWs on the modification of ionospheric plasma density. Before, studying the eclipse effect on the ionosphere, it is essential to identify the space weather solar flare and geomagnetic storm conditions which are important contributors of VTEC variability 25 , We have checked three hourly planetary K index K p and disturbance storm time index Dst providing the conditions for the geomagnetic activity for three days during Dec 13—15, These values show quiet geomagnetic conditions.
Thus, there was no magnetospheric input during the analysis period i. The peculiar features observed during TSE were explained based on the interplay between the eclipse effect on the ionospheric plasma density and eclipse generated AGWs, whose propagation towards northward was supported by background wind. Thus, the results of TSE indicated an important role of eclipse generated AGWs and background wind in affecting ionospheric plasma.
In the present work, we are revisiting the role of eclipse induced AGWs and their effect on the ionosphere to explain the observations. To see the presence of AGWs, we have analyzed VTEC data using the Morlet wavelet analysis technique as discussed in many of the previous works 4 , 27 , 28 and also used in Maurya et al.
The wavelet analysis results are shown in Fig. For the analysis, first, we have filtered fluctuations greater than 2 h to see the high-frequency fluctuations caused by the eclipse. For the filtered time series, we performed the Morlet wavelet analysis for the site running from south to north. In Fig. As one can see in Fig.
The AGWs at totality sites are very weak in intensity, while the site away from totality shows strong intensity. This is because the wave amplitude increases away from the source regions. Further, at the site far north and south of the totality line, intensity is again very weak. As shown in Fig. As suggested by Somsikov 29 , AGWs generated by the solar eclipse, propagates as a wave, away from the totality path. Further, the amplitude of AGWs is higher for the sites north of totality and also for the PRN29, moving along the eclipse path.
Thus, we speculate, it is possible that background conditions supporting AGWs propagation northward and along the eclipse path. Six representative GPS sites are shown.
As suggested in many previous works 12 , 30 , 31 the background winds and vertically sheared horizontal wind affect AGWs propagation. The music information for this update was selected by Gracenote Inc. The content of the update data is not publicly available, so Mitsubishi Motors cannot respond to any inquiries concerning specific music information.
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