Fig. 2: Convective dynamics in the mantle of tidally-locked exoplanets obtained through the laboratory analog.
From: Convective dynamics in mantle of tidally-locked exoplanets
Snapshots of velocity fields (top), Hovmöller diagram of vertical velocity uz obtained at the middle depth z = 0.5 (middle), and time-averaged vertical velocity uz (bottom) for (a) steady, (b) periodic, and (c) unsteady conditions. The left half and the right half of each panel represent the dayside and the nightside, respectively. d Time evolution of the Reynolds number, \({{{\rm{Re}}}}\), for the three conditions shown in (a, b, and c). Dotted horizontal lines represent \({{{\rm{Re}}}}\) obtained before imposing Θ, i.e., Rayleigh–Bénard convection. Each inset corresponds to the period shown in the Hovmöller diagram, 4000 < t < 5000. e Péclet number \({{{\rm{Pe}}}}={{{\rm{Re}}}}\,\Pr\) plotted over the hybrid Rayleigh number Ra = (1 + Θ) Raz, collapsing the data. Colors correspond to Pr, and the conditions highlighted correspond to (a, b, and c). The solid line is the power-law curve, Pe ∝ Ra0.58, acquired with the least-squares fitting. The inset shows \({{{\rm{Re}}}}\) plotted over the classical Rayleigh number, Raz, showing deviations originating from Θ and differences across Pr. All variables are nondimensionalized with the length scale H, the velocity scale U, and the time scale H/U. The original videos visualized using the TLC particles corresponding to (a, b, and c) are provided as Supplementary Movies1, 2, and 3, along with the hemispherical projection.
