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3D Simulations of Convective Entrainment in Gas Giants: Rotation and Decreasing Luminosity as Barriers to Mixing

  • Authors: Shu Zhang, 舒 张, J. R. Fuentes, Andrew Cumming

Shu Zhang et al 2025 The Astrophysical Journal Letters 991 .

  • Provider: AAS Journals

Caption: Figure 1.

3D snapshots of the z-component of the vorticity ω = ∇ × u for the nonrotating case (panel (a)) and rotating case (panel (b)), both cooling with a decreasing flux from the top boundary. For both cases, the snapshots are shown at the same time, when the heat flux that drives convection has decreased to 10% of its initial value. The Rossby number of the convective flow in the rotating case is Ro ≈ 0.01, computed using the averaged flow velocity in the convection zone and the thickness of the convection zone. At t = 8 × 10−2, the convection zone depth in units of the box size H is h = 0.37 for the rotating case and h = 0.56 in the nonrotating case.

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