@Article{CorreiaSACGTHR:2017:IoFrRe,
author = "Correia, Emilia and Spogli, Luca and Alfonsi, Lucilla and
Cesaroni, Claudio and Gulisano, Adriana M. and Thomas, Evan G. and
Hidalgo Ramirez, Ray F. and Rodel, Alexandre A.",
affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Istituto
Nazionale di Geofisica e Vulcanologia} and {Istituto Nazionale di
Geofisica e Vulcanologia} and {Istituto Nazionale di Geofisica e
Vulcanologia} and {Instituto Ant{\'a}rtico Argentino} and
{Dartmouth College} and {Universidade Presbiteriana Mackenzie} and
{Universidade Presbiteriana Mackenzie}",
title = "Ionospheric F-region response to the 26 September 2011 geomagnetic
storm in the Antarctica American and Australian sectors",
journal = "Annales Geophysicae",
year = "2017",
volume = "35",
number = "5",
pages = "1113--1129",
month = "Oct.",
keywords = "Ionosphere (Ionospheric disturbances).",
abstract = "The ionospheric response at middle and high latitudes in the
Antarctica American and Australian sectors to the 26-27 September
2011 moderately intense geomagnetic storm was investigated using
instruments including an ionosonde, riometer, and GNSS receivers.
The multi-instrument observations permitted us to characterize the
ionospheric storm-enhanced density (SED) and tongues of ionization
(TOIs) as a function of storm time and location, considering the
effect of prompt penetration electric fields (PPEFs). During the
main phase of the geomagnetic storm, dayside SEDs were observed at
middle latitudes, and in the nightside only density depletions
were observed from middle to high latitudes. Both the increase and
decrease in ionospheric density at middle latitudes can be
attributed to a combination of processes, including the PPEF
effect just after the storm onset, dominated by disturbance dynamo
processes during the evolution of the main phase. Two SEDs-TOIs
were identified in the Southern Hemisphere, but only the first
episode had a counterpart in the Northern Hemisphere. This
difference can be explained by the interhemispheric asymmetry
caused by the high-latitude coupling between solar wind and the
magnetosphere, which drives the dawn-to-dusk component of the
interplanetary magnetic field. The formation of polar TOI is a
function of the SED plume location that might be near the dayside
cusp from which it can enter the polar cap, which was the case in
the Southern Hemisphere. Strong GNSS scintillations were observed
at stations collocated with SED plumes at middle latitudes and
cusp on the dayside and at polar cap TOIs on the nightside.",
doi = "10.5194/angeo-35-1113-2017",
url = "http://dx.doi.org/10.5194/angeo-35-1113-2017",
issn = "0992-7689",
language = "en",
targetfile = "correia_ionospheric.pdf",
urlaccessdate = "01 maio 2024"
}