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Accretion Rates and Thermohaline Convection in Polluted White Dwarfs

  • Authors: J. R. Fuentes, Matias Castro-Tapia, Jim Fuller, Marcus N. King

J. R. Fuentes et al 2026 The Astrophysical Journal Letters 1011 .

  • Provider: AAS Journals

Caption: Figure 3.

Evolution of the thermohaline layer using the parameters of G 29–38 for an accretion rate ﹩{\dot{M}}_{{\rm{acc}}}=1{0}^{10}\,{\rm{g}}\,{{\rm{s}}}^{-1}﹩. Panel (a): thermohaline layer depth h(t) as a function of time since the onset of accretion. Panel (b): mass fraction of heavy elements at the surface, Xsurf(t) over the same period. In both panels, the dotted and dashed lines show the shallow-layer and deep-layer asymptotic scalings, respectively. The horizontal dashed line in panel (a) marks the scale height z0 = (17/4)H0 ≈ 2.5 km, which sets the transition between the two regimes.

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