Signature of the 29 March 2006 eclipse on the ionosphere over an equatorial station

Adeniyi, J.O.; Radicella, S. M.; Adimula, I. A.; Willoughby, A. A.; Oladipo, O.A.; Olawepo, Olayinka

doi:10.1029/2006ja012197

Cited by 65 publications

(67 citation statements)

References 15 publications

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“…The results of Skinner (1967) were for a period of high solar activity when the F1 region is not very distinct from the F2, and 68 % reduction was noticed in the electron density of the F1 region. Adeniyi et al (2007) have also shown that maximum decrease in the peak electron density as deduced from the critical frequency for F1 was 68 % for the total solar eclipse of 29 March 2006 during low solar activity period. In Fig.…”

Section: F1 Layermentioning

confidence: 89%

“…The eclipse effect in the F2 region is larger at high solar activity than at low solar activity. In a recent study, the signatures of a total solar eclipse on ionospheric E, F1 and F2 regions, during the forenoon hours, have been reported by Adeniyi et al (2007), as observed over equatorial station Ilorin, Nigeria. In the present investigation, we find that the decrease in electron density occurs throughout the E and F1 layer heights at about the same time, while, in the F2 region, the electron density decrease began at lower heights and extended progressively towards the layer peak.…”

Section: Introductionmentioning

confidence: 99%

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The equatorial ionospheric response over Tirunelveli to the 15 January 2010 annular solar eclipse: observations

et al. 2012

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Abstract. In this paper we present a case study of the annular solar eclipse effects on the ionization of E and F regions of equatorial ionosphere over Tirunelveli [77.8 • E, 8.7 • N, dip 0.4 • N] by means of digital ionosonde on 15 January 2010. The maximum obscuration of the eclipse at this station was 84 % and it occurred in the afternoon. The E and F1 layers of the ionosphere showed very clear decrease in their electron concentrations, whereas the F2 layer did not show appreciable changes. A reduction of 30 % was observed in the foF1 during the maximum phase of the eclipse. During the beginning phase of the eclipse, an enhancement of 0.97 MHz was observed in the foF2 as compared to that of the control days. But the foF2 decreased gradually as the eclipse progressed and a decrease of 0.59 MHz was observed towards the end phase of the eclipse. Observed variations in the h F2 and hmF2 showed lower values than the control days, although hmF2 was found to increase a bit during the eclipse. Observed variability in the E, F1 and F2 layer ionospheric parameters on the eclipse day and their departure from the control days are discussed as the combined effect of annular eclipse and presence of counter equatorial electrojet (CEEJ).

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Section: F1 Layermentioning

confidence: 89%

Section: Introductionmentioning

confidence: 99%

The equatorial ionospheric response over Tirunelveli to the 15 January 2010 annular solar eclipse: observations

et al. 2012

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“…The Ilorin site has an advantage of being a Baseline Surface Radiation Network (BSRN) candidate site with several operational instruments for environmental monitoring (Pinker et [3]. These include Pyranometers, Pirgeometers, Pressure and temperature sensors and AERONET Cimel sensors.…”

Section: Methodsmentioning

confidence: 99%

“…Temperature: The temperature was measured on a flat rooftop at a site synonymous with Adeniyi, et al (2006). It showed a drop in value between 09:08 and 09:58 GMT with a minimum at about 9.32 GMT (Figure 1).…”

Section: Direct Solar Radiationmentioning

confidence: 99%

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Diminishing Solar Radiation as a Driving Factor of Changes in Space Laboratory: A Study of March 29th 2006 Eclipse As Viewed and Monitored In Katsina State, Nigeria

2017

IJACEBS

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Abstract-On Wednesday, 29 th 2006 suddenly a Solar Eclipse erupted in Katsina State (12 0 15"N, 7 0 30"E) in Northern Nigeria at around 11: 16 am Nigerian GMT, which also lasted for about 40 minutes. It was, before then speculated that it was going to happen. But then, many local Climatic predictors alongside ignorant local residents presumed it was just a speculation and mere fantasy. In the Eclipse, there was an instant cut-off of solar radiant energy which also affected the many Biological clocks of many Ecosystems and even beyond. During the incidence, there were many changes in Environmental parameters. At the time of the total eclipse of the sun by moon both the air temperature and the Radiant energy attained a maximum stage. Equally, Aerosol Optical Depth (AOD) and Relative Humidity (RH) rose to maximum before clocking back to normal values. Scientific calculations and or measurements are needed during this period in order to find out any adverse conditions on any living specie in the affected area. With abrupt decrease in incoming sun"s radiation and temperature and an increase in humidity, if prolonged could impose changes on precipitation, freezing points, flooding, and so on. Solar Eclipse in turn provides a natural space laboratory for measurement of diffused Radiation and its effect on Ecosystems, if there be. This paper observes some scientific changes as observed during the Eclipse that affected the optimum conditions of living species.

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Ionospheric vertical plasma drift and electron density response during total solar eclipses at equatorial/low latitude

2015

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The response of the vertical plasma drift (Vz) and the electron density (NmF2) during different solar eclipses was investigated. The diurnal values of the direct scaled measurement of F2 peak height and the one derived from M(3000) F2 data, acquired over an equatorial/low‐latitude stations, have been used to determine the vertical plasma drift. The ionosphere during a solar eclipse is significantly affected by the E × B vertical drift; the large depletion of electron density at low altitudes can be transported to high altitudes through the plasma vertical drift. The loss in ionization density during the eclipse phase decreases the electron density, which was accompanied by rapid increase in hmF2. This deviation in the NmF2 during eclipse compared to control days can be related to the increase in the loss rate due to recombination, as a result of reduction in thermal energy. However, the maximum reduction in NmF2 is not synchronous with the time of maximum totality but some minutes later. The differences in the solar epochs may contribute to the observed relative changes in the ionospheric F2 region behavior during the eclipse window. Lastly, it is very difficult to separate the influence of magnetic disturbances from solar eclipse. The deviation in NmF2 is higher during magnetic disturbed days than the quiet day. The reverse is the case for hmF2 observation. However, the NmF2 variation increases with an increase in solar activity.

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Signature of the 29 March 2006 eclipse on the ionosphere over an equatorial station

Cited by 65 publications

References 15 publications

The equatorial ionospheric response over Tirunelveli to the 15 January 2010 annular solar eclipse: observations

The equatorial ionospheric response over Tirunelveli to the 15 January 2010 annular solar eclipse: observations

Diminishing Solar Radiation as a Driving Factor of Changes in Space Laboratory: A Study of March 29th 2006 Eclipse As Viewed and Monitored In Katsina State, Nigeria

Ionospheric vertical plasma drift and electron density response during total solar eclipses at equatorial/low latitude

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