@Article{SilvaSoSoDeBoSa:2019:IoPlBu,
author = "Silva, R{\'e}gia Pereira da and Souza, Jonas Rodrigues de and
Sobral, Jos{\'e} Humberto Andrade and Denardin, Clezio Marcos and
Borba, Gilvan Luiz and Santos, Marcos Aur{\'e}lio Ferreira dos",
affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto
Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de
Pesquisas Espaciais (INPE)} and {Instituto Nacional de Pesquisas
Espaciais (INPE)} and {Universidade Federal do Rio Grande do Norte
(UFRN)} and {Instituto Nacional de Pesquisas Espaciais (INPE)}",
title = "Ionospheric plasma bubble zonal drift derived from total electron
content measurements",
journal = "Radio Science",
year = "2019",
volume = "54",
number = "7",
pages = "580--589",
month = "July",
keywords = "equatorial ionosphere, plasma bubble, GNSS, zonal drift.",
abstract = "Equatorial plasma bubbles consist of field-aligned large-scale
depletions, or irregularities, characterized by drastic ion
density rarefactions of the nocturnal low latitude/equatorial
ionosphere. Understanding their behavior is important because of
their degrading effects on radio wave signals and, consequently,
their respective technological applications such as, for example,
Global Positioning System applications. In this sense, a
methodology of pattern recognition was developed and implemented
here using the Long-Term Ionospheric Anomaly Monitoring in order
to infer the plasma bubbles zonal drift velocities, using two
receiving stations of global navigation satellite systems data
from the Brazilian Continuous Monitoring Network, located near to
each other, in Salvador (BA) during geomagnetically quiet periods.
The study covered the years of 2012, 2013, and 2014 for the months
from September to January of the following year, choosing 10
representative days for each month. The average results for the
plasma bubble zonal velocities provided by the model calculations
were in agreement with the well-known values. However, monthly
individual analysis showed a behavior anticorrelated with that
expected for high solar flux. Probably, the unexpected behavior is
due to atypical configuration of the solar activity ascending
phase.",
doi = "10.1029/2018RS006727",
url = "http://dx.doi.org/10.1029/2018RS006727",
issn = "0048-6604",
language = "en",
targetfile = "silva_ionospheric.pdf",
urlaccessdate = "28 abr. 2024"
}