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Formation of Suprathermal Electron Populations in the Expanding, Turbulent Solar Wind

  • Authors: Maximilien Péters de Bonhome, Fabio Bacchini, Luca Pezzini, Viviane Pierrard

Maximilien Péters de Bonhome et al 2026 The Astrophysical Journal Letters 1005 .

  • Provider: AAS Journals

Caption: Figure 4.

Time evolution of the perpendicular (fe(ve)) and parallel (fe(ve)) electron VDFs. The dashed green line corresponds to a Maxwellian fit at t = 0, while the dashed black line corresponds to a Kappa distribution fit (e.g., C. S. Salem et al. 2023) at ﹩t=1.5{\tau }_{{\rm{\exp }}}﹩ with parameter κ = 6.2 for fe(ve) and κ = 5 for fe(ve). The solid blue line indicates the electron VDF at ﹩t=0.5{\tau }_{{\rm{\exp }}}﹩ (onset time of expansion). The insets show the time evolution of the electron VDF at a fixed speed v* = {2.0, 2.5, 3.0}vthe0 associated with the vertical dashed lines displayed in their respective main panel.

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