Adebesin, B.O. and Adeniyi, J.O. and Adimula, I.A. and Reinisch, B.W. (2013) Low latitude nighttime ionospheric vertical E×B drifts at African region. Advances in Space Research, 52 (12). pp. 2226-2237. ISSN 0273 1177
Full text not available from this repository.Abstract
The nighttime vertical E x B drifts velocities of the F2-region were inferred from the hourly hmF2 values obtained from ionosonde data over an African equatorial station, Ilorin (8.50oN, 4.68oE; dip lat. 2.95o) during period of low solar activity. For each season, the plasma drift Vz is characterized by an evening upward enhancement, then by a downward reversal at 1900 LT till around 0000 LT, except for June Solstice. This was explained using the Rayleigh-Taylor (R-T) instability mechanism. The occasional drift differences in Vz obtained by inferred and direct measurement over Ilorin and Jicamarca respectively are reflective of the importance of chemistry and divergent transport system due to both the E region electric and magnetic fields instead of simple motions. The pre-reversal enhancement (PRE) magnitude is higher during the equinoctial months than the solsticial months over Jicamarca, highest during December solstice and the equinoctial months over Ilorin, suggesting the dominance of higher E x B fountain during equinoxes at both stations. The lowest PRE magnitude was in June Solstice. The appearance of post-noon peak in NmF2 around 1700LT is highest during the equinoctial months and lowest during the solsticial period. A general sharp drop in NmF2 around 1800 LT is distinct immediately after sunset, lowest during June solstice and highest in March equinox. Our result suggests that between 0930-2100 LT, the general theory that vertical drifts obtained by digisonde measurements only match the E x B drift if the F layer is higher than 300 km is reliable, but does not hold for the nighttime period of 2200-0600 LT under condition of solar minima. Hence, the condition may not be sufficient for the representation of vertical plasma drift at nighttime during solar minima. This assertion may still be tentative, as more equatorial stations needed to be studied for better confirmation.
| Item Type: | Article |
|---|---|
| Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
| Depositing User: | DR. B. OLUFEMI ADEBESIN |
| Date Deposited: | 12 Jun 2015 20:27 |
| Last Modified: | 12 Jun 2015 20:27 |
| URI: | https://eprints.lmu.edu.ng/id/eprint/232 |
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