2011
DOI: 10.1016/j.jastp.2011.05.004
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Day to day variability of h′F and foF2 during some solar cycle epochs

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Cited by 11 publications
(8 citation statements)
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“…Hence the IRI-2016 model attained its peak before OBS-TEC. Dabas et al (2003), Somoye et al (2011), Hajra et al (2016) andD'ujanga et al (2017) attributed the steep increase in TEC to the upward E × B vertical plasma drift and the rapid filling up of the magnetic field tube at sunrise due to solar extreme ultraviolet (EUV) ionization. During daytime, an eastward electric field at the Equator causes plasma to be lifted to greater heights.…”
Section: Methodsmentioning
confidence: 99%
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“…Hence the IRI-2016 model attained its peak before OBS-TEC. Dabas et al (2003), Somoye et al (2011), Hajra et al (2016) andD'ujanga et al (2017) attributed the steep increase in TEC to the upward E × B vertical plasma drift and the rapid filling up of the magnetic field tube at sunrise due to solar extreme ultraviolet (EUV) ionization. During daytime, an eastward electric field at the Equator causes plasma to be lifted to greater heights.…”
Section: Methodsmentioning
confidence: 99%
“…Same as Fig. 1 but for 2012. additional ionization (D'ujanga et al, 2017;Somoye et al, 2011). Suranya et al (2015) further mentioned that upward vertical E × B drift could lead to an equatorial ionization anomaly (EIA) and meridional winds.…”
Section: Methodsmentioning
confidence: 99%
“…From these results, and also considering that the F2 layer is by far the most important ionospheric layer for HF band radio communications, it emerges that F2‐layer variability is of much greater importance than that of the E region and F1 layer. For these reasons, over the years many studies have focused on the F2 layer and its variability [e.g., Elias , 2009; Jarvis , 2009; Rishbeth et al , 2009; Chen and Liu , 2010; David and Sojka , 2010; Liu et al , 2011; Somoye et al , 2011; Triskova et al , 2011; Zolotukhina et al , 2011].…”
Section: Introductionmentioning
confidence: 99%
“…Hence the IRI-2016 model attained its peak before OBS-TEC. The steep increase in TEC has been attributed to the solar EUV ionization together with the upward vertical E × B resulting from the rapid filling up of the magnetic field tube at sunrise (Dabas et al, 2003;Somoye et al, 2011;Hajra et al 2016;D'ujanga et al, 2017) and meridional winds (Suranya et al, 2015). These magnetic field tubes collapse after sunset due to low thermospheric temperature and Releigh Taylor Instability (RTI) (Ayorinde et al, 2016) giving rise to the minimum TEC values after sunset.…”
Section: Resultsmentioning
confidence: 99%