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Subsurface Magnetic Field and Flow Structure of Simulated Sunspots

  • Authors: Matthias Rempel

Rempel 2011 The Astrophysical Journal 740 15.

  • Provider: AAS Journals

Caption: Figure 4.

Properties of the azimuthally and temporally (15 hr from t = 35 hr to t = 50 hr) averaged flow in the simulation run without penumbra. Displayed are (a) radial and (b) vertical flow velocities relative to the convective rms velocity (positive values indicate outflow/upflow). Panel (c) presents the fraction of the mass flux present in the azimuthal mean component. Panel (d) presents the temperature perturbation relative to the mean stratification computed outside R = 25 Mm (i.e., corners of the domain) in units of the rms fluctuation (outside R = 25 Mm). It is evident that the main upflow coincides with an annulus of enhanced temperature between R = 8 and R = 16 Mm. The thermal signature of the large flow is comparable to that of convective flows. We indicated the field lines of the azimuthally averaged magnetic field for reference; the nearly horizontal line near the top indicates the τ = 0.1 level.

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