Complex interplanetary ejecta and their association to multi-step magnetic storm main phase development

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It was observed long time ago that, although the classical definition of magnetic storms is quite simple, a magnetic storm could evolves in a much more complex way. It was recently shown that the main phase of intense magnetic storms usually develops in two or more steps. It occurs as a consequence of several energy injections during the main phase storm time. It was argued that the main source of these injections are associated to intense southward fields observed during the passage of interplanetary solar mass ejections, mainly in the sheath region, just behind the shock and in the ejecta itself. Recently, studies based on radio signatures and coronal observations have shown that the complex ejecta structures observed near 1 AU seems to be associated to the interaction of two or more coronal mass ejections. In this work we present a study of solar origin of the complex ejecta event observed near 1 AU in October 3-7, 2000 and of the multi-step magnetic storm main phase associated. In order to identify the solar origin it was used observations of the Large Angle and Spectroscopic Coronagraph (LASCO) and Extreme Infrared Telescope (EIT), which are instruments on board of Solar and Hemispheric Observatory (SOHO). The solar wind properties at 1 AU were studied using plasma, composition and ionization rates and interplanetary magnetic field observations of ACE spacecraft. The magnetospheric conditions were determined based on observations realized by in situ measurements and on geomagnetic global and auroral indices. In order to quantify the solar wind-magnetosphere coupling the energy injection functions were estimated. LT-UT diagrams were used to study the ring current asymmetries during the main phase.

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