Geographical analysis of equatorial plasma bubbles by GPS and nightglow measurements

Nade, D.P.; Shetti, Dadaso J.; Sharma, Ashok; Taori, A.; Chavan, G.A.; Patil, P. T.; Ghodpage, R. N.; Gurav, O.B.; Nikte, S.S.

doi:10.1016/j.asr.2015.03.030

Cited by 8 publications

(6 citation statements)

References 43 publications

(50 reference statements)

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“…EPBs are frequently observed over Indian region using all-sky imaging observations [Sinha and Raizada, 2000;Mukherjee, 2003;Rajesh et al, 2010;Narayanan et al, 2012;Nade et al, 2013Nade et al, , 2015Sharma et al, 2014;Taori and Sindhya, 2014]. We utilize all-sky imaging of OI 630 nm emission obtained from Indian station Panhala (16.8°N, 74.1°E geographic, 11.1°N dip latitude) in campaign mode observations during January to March 2008.…”

Section: Databasementioning

confidence: 99%

Shrinking equatorial plasma bubbles

et al. 2016

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The formation of equatorial plasma bubbles (EPBs) associated with spread F irregularities are fairly common phenomenon in the postsunset equatorial ionosphere. These bubbles grow as a result of eastward polarization electric field resulting in upward E × B drift over the dip equator. As they grow they are also mapped to low latitudes along magnetic field lines. The EPBs are often observed as airglow depletions in the images of OI 630 nm emission. On occasions the growth of the features over the dip equator is observed as poleward extensions of the depletions in all‐sky images obtained from low latitudes. Herein, we present interesting observations of decrease in the latitudinal extent of the EPBs corresponding to a reduction in their apex altitudes over the dip equator. Such observations indicate that these bubbles not only grow but also shrink on occasions. These are the first observations of shrinking EPBs. The observations discussed in this work are based on all‐sky airglow imaging observations of OI 630.0 nm emission made from Panhala (11.1°N dip latitude). In addition, ionosonde observations made from dip equatorial site Tirunelveli (1.1°N dip latitude) are used to understand the phenomenon better. The analysis indicates that the speed of shrinking occurring in the topside is different from the bottomside vertical drifts. When the EPBs shrink, they might decay before sunrise hours.

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Section: Databasementioning

confidence: 99%

Shrinking equatorial plasma bubbles

et al. 2016

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“…The different aspects of EPBs have been studied by many researchers such as occurrence characteristics (e.g., Candido et al, 2011;Makela et al, 2004;Sahai et al, 1994;Sharma et al, 2014;Sun et al, 2016), morphology and evolution (e.g., Aggson et al, 1996;Huba et al, 2015;Wu et al, 2017), statistical features of EPBs (e.g., Narayanan et al, 2017;Sinha & Raizada, 2000;Sun et al, 2016), and zonal drift velocity (e.g., Abalde et al, 2004;Immel et al, 2004;Mukherjee & Shetti, 2008;Nade et al, 2013;Paulino et al, 2011;Pimenta et al, 2001;Taori et al, 2013;Yao & Makela, 2007). However, there are different techniques to monitor and study the evolution and characteristics of these large-scale structures (EPBs) such as incoherent scatter radar (e.g., Fejer et al, 1991), VHF spaced receiver system (e.g., Bhattacharyya et al, 2003;Sharma et al, 2018), Fabry-Pérot interferometer (e.g., Sahai et al, 1992), GPS (e.g., Haase et al, 2011;Ji et al, 2011;Nade et al, 2015), and ASI (e.g., Fagundes et al, 1997;Ghodpage et al, 2018;Kishore & Mukherjee, 2007;Nade et al, 2013;Sobral et al, 2009;Taori & Sindhya, 2014). Sun et al (2016) investigated the statistical features of EPBs using airglow images from 2012 to 2014, which lies in the increasing phase of 24th solar cycle from a ground-based network of four ASIs in the equatorial region of China.…”

Section: Introductionmentioning

confidence: 99%

Zonal Drift Velocity of Equatorial Plasma Bubbles During Ascending Phase of 24th Solar Cycle Using All‐Sky Imager Over Kolhapur, India

et al. 2018

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This paper reports the statistical analysis of zonal drift velocity of equatorial plasma bubbles (EPBs) inferred from advanced optical technique (all‐sky imager) with OI 630.0‐nm airglow emission from January to April of 2011 to 2013. Over 143 nights of observations have been carried out using all‐sky imager over low‐latitude station Kolhapur (16.8°N, 74.2°E; 10.6°N dip latitude), out of which 58 nights showed signatures of EPBs. We study the hourly, monthly, and seasonal variation in zonal drift velocity of EPBs. Also, the magnetically disturbed nights (Ap > 18) are separately studied. It is observed that (a) the daily peak zonal drift velocity is seen to be positively correlated to corresponding daily averaged 10.7‐cm solar flux. (b) The zonal drift velocity is found to be larger in the equinox months than that of winter months. (c) During the disturbed nights the zonal drift velocity gets slower and one of the disturbed nights showed the latitudinal variation in zonal drift velocity during the development phase of EPBs before midnight hours. We suggest that this variation might be occurred due to the disturbance dynamo electric fields at low latitude, which reduces the EPBs' eastward velocity. (d) The zonal drift velocity of EPBs presented in this paper is in good agreement with the previous studies as well as the HWM‐07 model values.

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“…The RINEX format of the GPS receiver was processed using GPS_Gopi_v3.03 TEC processing software developed by G. K. Seemala, (2017), https://seemala.blogspot.com/2017/09/gps-tec-program-ver-295.html, and the slant TEC were derived from the RINEX data files using an algorithm developed at Boston College, USA which uses phase and code values for both 𝐴𝐴 𝐴𝐴1 (𝑓𝑓1 = 1575.42 MHz) and 𝐴𝐴 𝐴𝐴2 (𝑓𝑓2 = 1227.60 MHz) GPS frequencies to remove differential clock error effects (Ciraolo & Spalla, 1997;Ciraolo et al, 2007;Nade et al, 2015;Odeyemi et al, 2022;Seemala & Valladares, 2011).…”

Section: Data Acquisition and Methods Of Analysismentioning

confidence: 99%