Ionospheric E-region drifts at Yamagawa during IQSY.

Patel, V. P.; Chandra, H.

doi:10.5636/jgg.32.129

Cited by 4 publications

(3 citation statements)

References 10 publications

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“…But it was the ionospheric drift data at Thumba, which showed that the drift speed during the midday hours in the E and F regions of the ionosphere decreased progressively with increasing Kp index (Rastogi et al, 1971b). Patel and Chandra (1982) showed that with the increasing Kp index, the drift speed at stations within the Sq focus latitude and the equator, Thumba, Tiruchirapalli and Ahmedabad decreased steadily. However at station north of the Sq focus latitude, Yamagawa and Sibzimir, the daytime drift speed (eastward) increased steadily with the increase of Kp index.…”

Section: Equatorial Ionospheric Driftsmentioning

confidence: 99%

Magnetic storm effects at equatorial electrojet stations

Rastogi

2006

Earth Planet Sp

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It is shown that there are distinctly two different mechanisms for the interaction of solar wind with the earth's magnetosphere to produce electric field in the ionospheric heights at low and middle latitudes. A persistent or slowly varying southward Interplanetary magnetic field i.e. negative IMF-B z generates dawn to dusk electric field at polar latitudes and a westward (dusk to dawn) electric field at dayside electrojet region which is anti-Sq in direction. A rapid increase of IMF-B z (northward turning) imposes a westward (dusk to dawn) electric field at all latitudes of the dayside hemisphere. The process involved is the imposition of −V × B z electric field at the magnetosphere transmitted instantaneously to the magnetic equator through the polar latitudes. The changes in the H field at ground are largest at stations close to the magnetic equator and the midday longitudes. During magnetic storms, associated with the southward IMF-B z , there are definite enhancements in the decrease of H field at the dayside equatorial electrojet stations. These changes may be coincident with the development of auroral or magnetospheric ring currents. These enhancements may be observed during the main phase as well as during the recovery phase of the magnetic storm, but the essential condition is that the IMF-B z has to be steadily significant southward. Sometimes during the storm period abnormally large changes in H field at day side equatorial electrojet regions are observed associated with large sudden changes in IMF-B z following the second mechanism of solar wind magnetospheric interaction. Thus the equatorial magnetic storm effects are due to combined effects of disturbance ring current, slow and steady IMF-B z as well as due to sudden large changes in IMF-B z .

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Section: Equatorial Ionospheric Driftsmentioning

confidence: 99%

Magnetic storm effects at equatorial electrojet stations

Rastogi

2006

Earth Planet Sp

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“…The results reported from low altitude and equatorial belt region suggested that drift speed decreases with magnetic activity index.Kelleher 9 , noticed an increase in the Es drift at Slough (51. 12 , studied the effect of magnetic activity on drift speed at various stations and found a negative correlation between drift speed and magnetic activity index in both E and F regions at all stations located between equator and 35 o N geog.latitude. They have also reported that a positive correlation at high latitudes beyond Sq.…”

Section: Literature Reviewmentioning

confidence: 99%

Untitled

2017

jusps-B

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The variation of drift and anisotropy parameters of Ionospheric irregularities in the E-region at Waltair (dip 17.7 o N; 83.3 o E) during 3 geomagnetic storms has been studied mainly to resolve the controversy that has been reported in the literature about the effect of magnetic activity on the drift and anisotropy parameters. E-region spaced antenna drift records taken on frequency 2.4 MHz during the period September 1983-May 1984 at Waltair are used in the present study. In the E-region, the true drift velocity during storm period appears to be larger than the control day values. The ratio of V a /V shows a gradual decrease during storm period and random velocity during storm time is quiet less compared to the control day values. No significant variation is observed in the apparent drift direction and structure size on storm days with respect to the control days. The orientation of the semi-major axis mostly lies in the range of 120 o -150 o N of E, both on storm days as well as on control days but the average value of the axial ratio shows a higher value compared to the average on control days.

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“…Briggs and Spencer, 1954;Patel and Chandra, 1982), equatorial latitudes (Skinner et al, 1963;Rastogi et al, 1972;Vyas and Chandra 1979), and low latitudes (Rastogi et al, 1978;Patel and Chandra 1980;Vyas 1989). These studies have given rise to a fair understanding of various morphological features, including seasonal variations of the horizontal ionospheric drifts.…”

Section: Introductionmentioning

confidence: 99%

Night-time F-region and daytime E-region ionospheric drifts measured at Udaipur during solar flares

Vyas

Pandey

2002

Ann. Geophys.

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Abstract. Ionospheric drifts measured at a low latitude station, Udaipur (Geomag. Lat. 14.5 • N), in the night-time Fregion and daytime E-region during solar flares have been studied. The night-time observations, which correspond to the F-region drifts, were carried out on five different nights. The daytime observation corresponding to the E-region drifts is only for one day. It is found that the apparent drift during the solar flare period is reduced considerably, in the daytime E-region as well as in the night-time F-region. The East-West and North-South components of the apparent drift speed are also similarly affected. For the daytime E-region drifts during a flare, increased ionization and subsequent reduction of reflection height is proposed to be the cause of reduced drift speeds. For the night-time F-region drifts, a reduced electric field at the F-region heights resulting from coupling of sunlit and dark hemispheres has been proposed to be the possible cause.

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Ionospheric E-region drifts at Yamagawa during IQSY.

Cited by 4 publications

References 10 publications

Magnetic storm effects at equatorial electrojet stations

Magnetic storm effects at equatorial electrojet stations

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Night-time F-region and daytime E-region ionospheric drifts measured at Udaipur during solar flares

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