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Thermally Regulated Viscoelastic Tidal Migration of Eccentric Planets

  • Authors: Cristobal Petrovich, Hareesh Gautham Bhaskar

Cristobal Petrovich and Hareesh Gautham Bhaskar 2026 The Astrophysical Journal Letters 1007 .

  • Provider: AAS Journals

Caption: Figure 7.

Equilibrium spin frequency feq = Ωs/n as a function of eccentricity for fixed values of the local Maxwell parameter M. The black curve shows the Hut pseudo-synchronous value. Horizontal guide lines mark the approximate spin–orbit resonances Ωs/n = N/2 associated with the dominant m = 2 harmonics. In the solid-like regime, the equilibrium spin can lock near these resonances. At lower eccentricity, the resonant structure is visibly discrete, whereas at high eccentricity the relevant N values are large and densely spaced, producing a smoother envelope.

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