TEC and Density Profiles Associated With the Occurrence of Equatorial Spread-F in the American Sector

Details TEC and Density Profiles Associated With the Occurrence of Equatorial Spread-F in the American Sector TEC and Density Profiles Associated With the Occurrence of Equatorial Spread-F in the American Sector

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsa72b0538v&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SA72B-0538

Physics

2415 Equatorial Ionosphere, 2439 Ionospheric Irregularities, 2471 Plasma Waves And Instabilities

Scientific paper

We have used TEC values observed by a network of 10 GPS receivers located near Jicamarca to form latitudinal profiles of TEC. We have also employed data from the Jicamarca digisonde to construct profiles of the equatorial F-region bottomside. These profiles have been obtained concurrently with multi-sensor detections of the equatorial spread-F (ESF) phenomena. The characteristics of ESF have been measured with the digisonde, UHF scintillation receivers located at Ancon and Antofagasta, several GPS receivers, and sometimes with the JULIA radar. GPS scintillations are measured between 3° south of the equator and 23° north magnetic latitude. This large latitudinal coverage of the scintillation receivers allows us to know the maximum latitudinal extension of the irregularities and consequently set a lower limit of the maximum altitude of the plasma bubbles. The network of GPS receivers was completed on August 2001. Since then, we have been able to infer the maximum altitude of the plasma depletions on a day-to-day basis. The one-year span of these combined datasets provides an opportunity to study in detail the seasonal variability of the background ionospheric and investigate the relation of the day-to-day variability of the ionosphere with the occurrence of ESF. The maximum altitude of the plasma bubbles presents a large degree of variability even during magnetically quiet days. We have compared the maximum latitude of scintillations with distributions of TEC and the location of the crests of the anomaly. We have determined that during the majority of the cases scintillations reach the location of the crests of the Appleton anomaly. Only in very few cases, scintillations were seen poleward of the northern crest.

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