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Tuning the Exospace Weather Radio for Stellar Coronal Mass Ejections

  • Authors: Julián D. Alvarado-Gómez, Jeremy J. Drake, Federico Fraschetti, Cecilia Garraffo, Ofer Cohen, Christian Vocks, Katja Poppenhäger, Sofia P. Moschou, Rakesh K. Yadav, and Ward B. Manchester IV

2020 The Astrophysical Journal 895 47.

  • Provider: AAS Journals

Caption: Figure 3.

Snapshot during the temporal evolution of the weakly confined CME (﹩{E}_{{\rm{B}},1}^{\mathrm{FR}}\simeq 4.1\times {10}^{35}﹩ erg, ﹩{E}_{{\rm{K}},1}^{\mathrm{CME}}\simeq 1.7\times {10}^{32}﹩ erg, ﹩{M}_{1}^{\mathrm{CME}}\simeq 9.4\times {10}^{15}﹩ g) within our M-dwarf simulation. The stellar surface is color-coded (purple-green) by the radial magnetic field driving the ambient AWSoM solution. A secondary color scale (magenta-yellow) denotes the density contrast, n(t)/nSS, which is used to trace the CME front by the indicated isosurface. The nominal shock condition, calculated from the Alfvénic Mach number of the CME front (﹩{M}_{{\rm{A}}}^{\mathrm{CME}}﹩, Equation (1)), is encoded simultaneously by the size of the scatter distribution (spheres) and by a tertiary color scale (cyan-red). The field of view is 32 R, with a set of selected large-scale magnetic field lines in gray.

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