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Non Gaussianity and cross scale coupling in interplanetary magnetic field turbulence during a rope–rope magnetic reconnection event

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Figure

Figure 1. Cluster-1 magnetic field and plasma parameters from00:00 to 12:00 UT on 2 February 2002
Table 1. Beginning and end of the intervals depicted in Fig. 1, cor-responding to the boundary layers of three interplanetary magneticflux ropes (IMFRs) on 2 February 2002.
Fig. 4a shows the power spectral density (PSD) as a func-tion of frequency f of the time series of |B| from the be-ginning of IMFR-1 at 00:32 UT until the end of IMFR-3 at
Table 4. The least-square fits of Eq. (7) computed from the scatterplots of Fig. 7 (τ = 100 s)
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