Maps of <I>fo</I>F2, <I>hm</I>F2, and plasma frequency above F2-layer peak in the night-time low-latitude ionosphere derived from Intercosmos-19 satellite topside sounding data

Abstract

Abstract. Maps of foF2, hmF2, and plasma frequency, fp, in the topside ionosphere at low latitudes, derived from Intercosmos-19 satellite topside sounding data, obtained from March 1979 to January 1981 and covering all longitudes, are presented for quiet geomagnetic conditions in June and December solstices at solar maximum for several local time intervals during the night. Based on these maps, features of the equatorial anomaly (EA) at different longitudes and their change during the night are considered. The maps show that averaged foF2, hmF2, and fp longitudinal variations are rather complicated, their structure looks wave-like with quasi-periods in longitude of about 75-100 • , similar to that on individual days revealed previously at low latitudes using Intercosmos-19 data. Positions of the structure extrema in certain longitude intervals are stable enough so that they are clearly seen in the maps after averaging over a large number of measurements made on different days and even in different years. Such structure seems to need at least five harmonics for its description.The maps derived from Intercosmos-19 data were compared with the maps given by the IRI model. Along with general resemblance, essential distinctions between them were found. Intercosmos-19 maps show more complicated and pronounced longitudinal structure than IRI maps. They also show that at solar maximum, in general, at night, EA is stronger and persists for a longer time (on average, until 04:00 LT) than that presented in IRI model. Besides, much stronger asymmetry between the characteristics of the EA northern and southern crests in certain longitude intervals was revealed, most evident in hmF2 maps.

Wave structures of the plasma density and vertical E × B drift in low‐latitude F region

“…We note that the presence of the wavelike density structure was identified earlier by topside soundings from the Russian satellite Intercosmos‐19 [ Kochenova , 1987, 1988; Karpachev , 1988; Benkova et al , 1990; Karpachev et al , 2003; Deminova , 2003, 2007]. The daytime morphologies of the upward drift velocity, electric field, and equatorial electrojet that were calculated using the latitudinal profile of the F peak electron density [ Benkova et al , 1990] showed a good agreement with the recent observations.…”