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@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"
}


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