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DC Field | Value | Language |
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dc.contributor.author | Gurram, P. | |
dc.contributor.author | Kakad, B. | |
dc.contributor.author | Bhattacharya, A. | |
dc.contributor.author | Pant, T.K. | |
dc.date.accessioned | 2010-02-07T02:04:37Z | |
dc.date.accessioned | 2021-02-12T10:20:31Z | - |
dc.date.available | 2010-02-07T02:04:37Z | |
dc.date.available | 2021-02-12T10:20:31Z | - |
dc.date.issued | 2018 | |
dc.identifier.citation | JGR, 123, 7710–7725, doi: 10.1029/2018JA025705 | en_US |
dc.identifier.uri | http://localhost:8080/xmlui/handle/123456789/1489 | - |
dc.description.abstract | We examined the seasonal and solar flux dependence of the occurrence of freshly generated intermediate scale (100 m to few km) equatorial spread F (ESF) irregularities during magnetically quiet (Q) and disturbed (D) periods. We utilized long-term (1992–2006 and 2013–2015) amplitude scintillation data on a 251 MHz signal recorded at Tirunelveli (dip lat. 1.5∘N ). Also, ionosonde data (1990–2003) recorded at Trivandrum (dip lat. 0.5∘N) are used. The presence of fresh ESF (F-ESF) is identified using the maximum cross-correlation between intensity variations recorded by two spaced receivers on a magnetic east-west baseline. We find distinct differences in the seasonal and solar flux dependence of the usual postsunset (<22 LT) generation of F-ESF on both Q- and D-days. Interesting feature is that F-ESF linked moderate–strong scintillations are more prevalent on D-days as compared to Q-days in both early (18–22 LT) and later (>22 LT) phase of evolution of the irregularities. It directly hints toward the difference in the spatial structuring (spatial scales) of F-ESF on D-days as compared to Q-days. On D-days, the occurrence of F-ESF is more likely around midnight and early-morning hours in all seasons. Whereas on Q-days, the postmidnight F-ESF is found to occur mainly during solstices of low solar activity. The possible sources for the generation of F-ESF around midnight on Q-days of solstices during low solar activity are examined. We also find that perturbation electric field linked with F-ESF on D-days sustains for longer time, which results in longer durations of the active phase of equatorial plasma bubbles. | en_US |
dc.language.iso | en_US | en_US |
dc.subject | Equatorial spread F | en_US |
dc.subject | Equatorial plasma bubbles | en_US |
dc.subject | ESF | en_US |
dc.subject | EPBs | en_US |
dc.subject | F-ESF | en_US |
dc.subject | Perturbation electric field | en_US |
dc.title | Evolution of Freshly Generated Equatorial Spread F (F-ESF) Irregularities on Quiet and Disturbed Days | en_US |
dc.type | Article | en_US |
dc.identifier.accession | 091780 | |
Appears in Collections: | UAS_Reprints |
Files in This Item:
File | Description | Size | Format | |
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KakadB_GurramP_BhattacharyyaA_etal_JGR_2018.pdf | 2.47 MB | Adobe PDF | View/Open |
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