@Article{GuedesPereCeca:2015:WaAnCM,
author = "Guedes, M{\'a}rcia Regina Guimar{\~a}es and Pereira, Eduardo dos
Santos and Cecatto, Jos{\'e} Roberto",
affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto
Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de
Pesquisas Espaciais (INPE)}",
title = "Wavelet analysis of CME, X-ray flare, and sunspot series",
journal = "Astronomy \& Astrophysics",
year = "2015",
volume = "573",
number = "A64",
pages = "10pp",
month = "Jan.",
keywords = "coronal mass ejections, data analysis.",
abstract = "Context. Coronal mass ejections (CMEs) and solar flares are the
most energetic transient phenomena taking place at the Sun.
Together they are principally responsible for disturbances in
outer geospace. Coronal mass ejections and solar flares are
believed to be correlated with the solar cycle, which is mainly
characterized by sunspot numbers. Aims. Here, we search for
pattern identification in CMEs, X-ray solar flares, and sunspot
number time series using a new data mining process and a
quantitative procedure to correlate these series. Methods. This
new process consists of the combination of a decomposition method
with the wavelet transform technique applied to the series ranging
from 2000 until 2012. A simple moving average is used for the
time-series decomposition as a high-pass filter. A continuous
wavelet transform is applied to the series in sequence, which
permits us to uncover signals previously masked by the original
time series. We made use of the wavelet coherence to find some
correlation between the data. Results. The results have shown the
existence of periodic and intermittent signals in the CMEs,
flares, and sunspot time series. For the CME and flare series, few
and relatively short time intervals without any signal were
observed. Signals with an intermittent character take place during
some epochs of the maximum and descending phases of the solar
cycle 23 and rising phase of solar cycle 24. A comparison among
X-ray flares, sunspots, and CME time series shows a stronger
relation between flare and CMEs, although during some short
intervals (four eight months) and in a relatively narrow band.
Yet, in contrast we have obtained a fainter or even absent
relation between the X-ray flares and sunspot number series as
well as between the CMEs and sunspot number series.",
doi = "10.1051/0004-6361/201323080",
url = "http://dx.doi.org/10.1051/0004-6361/201323080",
issn = "0004-6361 and 1432-0746",
label = "self-archiving-INPE-MCTI-GOV-BR",
language = "en",
targetfile = "aa23080-13_proof.pdf",
urlaccessdate = "27 abr. 2024"
}