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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 5.

The saturated magnetic field ﹩{\left({B}_{\perp }/{B}_{0}\right)}_{{\rm{sat}}}﹩ vs. the anisotropy parameter ξ. The shapes and colors represent different simulations (see the table on the right; see Table 2 for the nomenclature of the runs). Momenta separated by “/” represent different runs (e.g., PLI:5-30/80 implies PLI:5-30 and PLI:5-80). For the points with the same colors and shapes, larger ξ’s correspond to larger momenta (e.g., for PLI:5-30/80, ξ for PLI:5-80 is larger than PLI:5-30). The gray dashed line represents the prediction, i.e., Equation (15). The runs with monenergetic CRs mostly follow this prediction, unlike those with power-law CRs. Upper inset: modeling of ﹩{\left({B}_{\perp }/{B}_{0}\right)}_{{\rm{sat}}}﹩ using Equation (18) (red dashed line). Lower inset: modeling of ﹩{\left({B}_{\perp }/{B}_{0}\right)}_{{\rm{sat}}}﹩ using Equation (17) (navy-blue dashed line).

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