the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
| 07 Oct 2024
Cairns-Tsallis distribution applied to differences of magnetic field intensity in solar wind
Abstract. Relevance of the Cairns-Tsallis probability distribution in its application to time series of spatial magnetic field differences is shown. In particular, we explore its ability to explain the data obtained by the Ulysses mission during solar cycles 23 and 24. Our findings reveal that the Cairns-Tsallis density function provides an optimal fit to the data, showing a sensitivity to the small time scale of magnetic field changes. Fit parameters obtained with this model were analyzed, as well as some multifractal indices obtained through corresponding time series analysis. Furthermore, significant discrepancies have been identified between our results and those obtained by other authors, highlighting the appropriateness of the Cairns-Tsallis distribution in capturing the underlying complexity in the data.
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RC1: 'Comment on npg-2024-20', Anonymous Referee #1, 18 Nov 2024
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In this work the Authors apply the Cairns-Tsallis (CT) probability distribution to time series of spatial magnetic field differences. The work discusses a best approximation of the observed distribution function of magnetic field increments using the CT distribution in respect to the very preliminary work by other authors on a similar topic. Anyway, in spite of the best fitting results I do not see any significant cultural/scientific advancement to justify the publication of this work in NPG. Furthermore, the Authors do not discuss other similar studies, as for instance those by M. Leubner and co-Authors, who apply the Tsallis statistics to solar wind study. Another critical issue that I have fond is that the analysis done by the Authors is related to solar wind feature during solar activity maximums and minimums. To me this is not the best appropriate way how to do this study. Indeed, the solar wind has a duplex character, i.e. fast and slow solar wind, whose physical properties (Alfvénic nature, presence of coherent structures, etc.) are different. A best approach would be to distinguish between fast and solar wind periods. The previous study, to which the Authors refer, is indeed a very long-standing period of slow solar wind. Following these general comments I cannot recommend this work for publication in NPG.
Citation: https://doi.org/10.5194/npg-2024-20-RC1
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