@Article{GonzálezMendDomiMenc:2014:ToStIn,
author = "Gonz{\'a}lez, Arian Ojeda and Mendes Junior, Odim and Domingues,
Margarete Oliveira and Menconi, Varlei Everton",
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)}",
title = "Daubechies wavelet coefficients: A tool to study interplanetary
magnetic field fluctuations",
journal = "Geof{\'{\i}}sica Internacional",
year = "2014",
volume = "53",
number = "2",
pages = "101--115",
keywords = "astronomy, electrodynamics, magnetic field, magnetosphere,
spacecraft, wavelet analysis.",
abstract = "We have studied a set of 41 magnetic clouds (MCs) measured by the
ACE spacecraft, using the discrete orthogonal wavelet transform
(Daubechies wavelet of order two) in three regions: Pre-MC (plasma
sheath), MC and Post-MC. We have used data from the IMF
GSM-components with time resolution of 16 s. The mathematical
property chosen was the statistical mean of the wavelet
coefficients (Dd1 ). The Daubechies wavelet coefficients have been
used because they represent the local regularity present in the
signal being studied. The results reproduced the wellknown fact
that the dynamics of the sheath region is more than that of the MC
region. This technique could be useful to help a specialist to
find events boundaries when working with IMF datasets, i.e., a
best form to visualize the data. The wavelet coefficients have the
advantage of helping to find some shocks that are not easy to see
in the IMF data by simple visual inspection. We can learn that
fluctuations are not low in all MCs, in some cases waves can
penetrate from the sheath to the MC. This methodology has not yet
been tested to identify some specific fluctuation patterns at IMF
for any other geoeffective interplanetary events, such as
Co-rotating Interaction Regions (CIRs), Heliospheric Current Sheet
(HCS) or ICMEs without MC signatures. In our opinion, as is the
first time that this technique is applied to the IMF data with
this purpose, the presentation of this approach for the Space
Physics Community is one of the contributions of this work.",
issn = "0016-7169",
label = "scopus 2014-05 OjedaGonz{\'a}lezMendOlivMenc:2014:ToStIn",
language = "en",
urlaccessdate = "29 mar. 2024"
}