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Impact of Cosmic-Ray Distribution on the Growth and Saturation of Bell Instability

  • Authors: Saikat Das, Siddhartha Gupta, Prateek Sharma

Saikat Das et al 2026 The Astrophysical Journal 1005 .

  • Provider: AAS Journals

Caption: Figure 8.

CR distributions fcr(pμ) for the runs with monenergetic (left) and power-law (right) CRs at different times. The monenergetic CRs isotropize with time. For the power-law case, lower-energy CRs isotropize with time, unlike the higher-energy CRs. It is indicated with three white contours: 4πp2fcr ≈ 1.6 × 10−3 (left), 6.2 × 10−5 (middle), 4 × 10−6 (right). The white dashed line marks ﹩p{{\prime} }_{{\rm{eff}}}\approx 9.3p{{\prime} }_{{\rm{\min }}}﹩ (Equation (20)), a cutoff above which the CRs do not isotropize effectively until saturation (﹩t\approx 10{\gamma }_{\,\rm{fast}\,}^{-1}﹩).

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