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Re-analysis of Lepping’s Fitting Method for Magnetic Clouds: Lundquist Fit Reloaded

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Abstract

Magnetic clouds (MCs) are a subset of ejecta, launched from the Sun as coronal mass ejections. The coherent rotation of the magnetic field vector observed in MCs leads to envision MCs as formed by flux ropes (FRs). Among all the methods used to analyze MCs, Lepping’s method (Lepping, Burlaga, and Jones in J. Geophys. Res.95, 11957, 1990) is the broadest used. While this fitting method does not require the axial field component to vanish at the MC boundaries, this idea is largely spread in publications. We revisit Lepping’s method to emphasize its hypothesis and the meaning of its output parameters. As originally defined, these parameters imply a fitted FR which could be smaller or larger than the studied MC. We rather provide a re-interpretation of Lepping’s results with a fitted model limited to the observed MC interval. We find that typically the crossed FRs are asymmetric with a larger side both in size and magnetic flux before or after the FR axis. At the boundary of the largest side we find an axial magnetic field component distributed around zero which we justify by the physics of solar eruptions. In contrast, at the boundary of the smaller side the axial field distribution is shifted to positive values, as expected with erosion acting during the interplanetary travel. This new analysis of Lepping’s results has several implications. First, global quantities, such as magnetic fluxes and helicity, need to be revised depending on the aim (estimating global properties of FRs just after the solar launch or at 1 au). Second, the deduced twist profiles in MCs range quasi-continuously from nearly uniform, to increasing away from the FR axis, up to a reversal near the MC boundaries. There is no trace of outsider cases, but a continuum of cases. Finally, the impact parameter of the remaining FR crossed at 1 au is revised. Its distribution is compatible with weakly flattened FR cross-sections.

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Acknowledgements

We thank the referee for his/her comments which broaden the potential audience of the paper. S.D. acknowledges partial support from the Argentinian grants UBACyT (UBA), and PIP-CONICET-11220130100439CO. This work was partially supported by a one-month invitation of P.D. to the Instituto de Astronomía y Física del Espacio, and by a one-month invitation of S.D. to the Observatoire de Paris. This work was supported by the Programme National PNST of CNRS/INSU co-funded by CNES and CEA. S.D. is member of the Carrera del Investigador Científico, CONICET.

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  1. LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris Diderot, Sorbonne Paris Cite, 5 place Jules Janssen, 92195, Meudon, France

    Pascal Démoulin

  2. Instituto de Astronomía y Física del Espacio, CONICET, Universidad de Buenos Aires, CC. 67, Suc. 28, 1428, Buenos Aires, Argentina

    Sergio Dasso

  3. Facultad de Ciencias Exactas y Naturales, Departamento de Ciencias de la Atmósfera y los Océanos and Departamento de Física, Universidad de Buenos Aires, 1428, Buenos Aires, Argentina

    Sergio Dasso & Vanina Lanabere

  4. Institut d’Astrophysique Spatiale, UMR8617, Univ. Paris-Sud-CNRS, Université Paris-Saclay, Bâtiment 121, 91405, Orsay Cedex, France

    Miho Janvier

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  1. Pascal Démoulin
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Démoulin, P., Dasso, S., Janvier, M. et al. Re-analysis of Lepping’s Fitting Method for Magnetic Clouds: Lundquist Fit Reloaded. Sol Phys 294, 172 (2019). https://doi.org/10.1007/s11207-019-1564-x

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