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Evidence of Magnetic Flux Ropes in the Solar Wind From Sigmoidal and non-Sigmoidal Active Regions

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Abstract

We have examined WIND magnetic field and plasma data during the first half of 1998 in order to find encounters of this spacecraft with magnetic clouds. From the events obtained through this search, we have selected four of them taking into account their solar origin. The four magnetic clouds are related to halo or partial halo CMEs, but the morphology of the active region before the eruption is sigmoidal for three of them and non-sigmoidal for the other one. We have analyzed these events in the solar wind by fitting the experimental data to a non-force-free flux-rope model. We conclude that both kinds of active regions develop in the solar wind an ejection with a flux-rope topology.

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Authors and Affiliations

  1. Departamento de Física, Universidad de Alcalá, Alcalá de Henares, Madrid, Spain (e-mail

    C. Cid, M.A. Hidalgo, J. Sequeiros, J. Rodríguez-pacheco & E. Bronchalo

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  1. C. Cid
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  2. M.A. Hidalgo
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  3. J. Sequeiros
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  4. J. Rodríguez-pacheco
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  5. E. Bronchalo
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Cid, C., Hidalgo, M., Sequeiros, J. et al. Evidence of Magnetic Flux Ropes in the Solar Wind From Sigmoidal and non-Sigmoidal Active Regions. Solar Physics 198, 169–177 (2001). https://doi.org/10.1023/A:1005210212973

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  • DOI: https://doi.org/10.1023/A:1005210212973

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