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	<metadata ReferenceType="Conference Proceedings">
		<site>mtc-m16b.sid.inpe.br 802</site>
		<holdercode>{isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S}</holdercode>
		<author>Wrasse, Cristiano Max,</author>
		<author>Echer, Ezequiel,</author>
		<author>Dal Lago, Alisson,</author>
		<author>Fechine, Joaquim,</author>
		<affiliation>Instituto Nacional de Pesquisas Espaciais (INPE)</affiliation>
		<affiliation>Instituto Nacional de Pesquisas Espaciais (INPE)</affiliation>
		<affiliation>Instituto Nacional de Pesquisas Espaciais (INPE)</affiliation>
		<title>High speed streams and geomagnetic activity recurrency during different solar cycles revealed by wavelet analysis</title>
		<conferencename>Encontro Brasileiro de Física dos Plasmas, 9.</conferencename>
		<date>25-28 Nov.</date>
		<conferencelocation>São Pedro, SP</conferencelocation>
		<abstract>Solar wind velocity and the geomagnetic index Ap are used to verify the recurrency of the high speed streams and the geomagnetic activity in di®erent solar cycles. The wavelet technique is used to perform the spectral analysis of the solar wind velocity, interplanetary magnetic ¯eld parameters and geomagnetic index with 1-day resolution. The Ap index between 1978 and 2003 is also used. The solar wind velocity data come from three di®erent instruments in order to access di®erent time periods and solar cycles. The ISEE-3 is used for the period of 1978-1982. The WIND satellite is used for 1995-1997 and the ACE satellite is used for 1998-2002 period. The results suggest that the semi-annual variation in Ap index is stronger during descending phase of the solar cycle, while the annual variation in Ap is stronger during solar cycle 22 (1989-1990) maximum than during solar cycles 21 and 23. It is also observed that the 27-day periodicity is stronger for ~B components than for ~V components around 1998-2002. A semi-annual variation is clearly observed in ~V components than in ~B components around 1998-2002. Regarding the 27-day variation in solar wind speed and magnetic ¯eld strength, it can be seen that this periodicity is more visible in ~V than in ~B . This periodicity is also more stable (it exists for more time) during the 1995-1997 minimum than during the 1978-1982 maximum.</abstract>
		<secondarytype>PRE CN</secondarytype>
		<lastupdate>1970: lcp.inpe.br/ignes/2004/ administrator</lastupdate>
		<metadatalastupdate>2018: cptec.inpe.br/walmeida/2003/ administrator {D 2007}</metadatalastupdate>
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		<contenttype>External Contribution</contenttype>