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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 3.

(a) Distribution of (Te/Teβe) for electrons at ﹩t=0.5{\tau }_{{\rm{\exp }}}﹩ (left), ﹩t=1.0{\tau }_{{\rm{\exp }}}﹩ (middle), and ﹩t=1.5{\tau }_{{\rm{\exp }}}﹩ (right). The distribution is scaled as the amount of cells (nc) normalized by the total amount of cells (Nc). Isocontours of the theoretical oblique EFI are plotted as blue lines with ﹩{T}_{\perp e}/{T}_{\parallel e}=1-1.29/{\beta }_{\parallel e}^{0.97}﹩ (dotted), ﹩{T}_{\perp e}/{T}_{\parallel e}=1-1.32/{\beta }_{\parallel e}^{0.61}﹩ (dashed), and ﹩{T}_{\perp e}/{T}_{\parallel e}=1-1.36/{\beta }_{\parallel e}^{0.47}﹩ (solid) associated with growth rates of γ = 0.001, 0.1 and 0.2Ωe, respectively (S. P. Gary & K. Nishimura 2003), with Ωe = eB/(mec) and e is the electron charge. The green dashed line corresponds to the double-adiabatic expansion prediction (﹩{T}_{\perp e}/{T}_{\parallel e}={\beta }_{\parallel e}^{-1}﹩). (b) Logarithmic ratio between the electron VDFs (f) and a reference Maxwellian VDF (fM) in (veve)-space at ﹩t=0.5{\tau }_{{\rm{\exp }}}﹩ (left), ﹩t=1.0{\tau }_{{\rm{\exp }}}﹩ (middle), and ﹩t=1.5{\tau }_{{\rm{\exp }}}﹩ (right).

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