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Toward a Quantitative Model for Simulation and Forecast of Solar Energetic Particle Production during Gradual Events. I. Magnetohydrodynamic Background Coupled to the SEP Model

  • Authors: D. Borovikov, I. V. Sokolov, I. I. Roussev, A. Taktakishvili, and T. I. Gombosi

2018 The Astrophysical Journal 864 88.

  • Provider: AAS Journals

Caption: Figure 5.

Top: spheromak configuration for β0 = 0.02: meridional (left) and equatorial (right) planes. Magnetic field direction is marked with arrows; the off-plane component of the magnetic field is normalized per B0 (see Equation (26)) and shown by color. Local values of plasma parameter ﹩\beta ({\boldsymbol{r}})={\mu }_{0}P({\boldsymbol{r}})/{B}^{2}({\boldsymbol{r}})﹩ are shown, with orange curves corresponding to levels β = 0.04, 0.08, 0.12, and 0.16 as marked explicitly. Bottom: radial dependence of thermal pressure, ﹩{\mu }_{0}P(r)/{B}_{0}^{2}﹩ (red curve), and magnetic pressure, ﹩{B}^{2}(r)/{B}_{0}^{2}﹩ (blue curve), in the equatorial cut z = 0, for β0 = 0.02 (left) and for ﹩{\beta }_{0}=-2.87\times {10}^{-2}﹩ (right).

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