CHEOPS photometry improves radii for V1298 Tau b, c, and d, producing revised densities of 0.06-0.23 g cm^{-3} that indicate differential atmospheric evolution and no requirement for past dynamical excitation.
Deformation and tidal evolution of close-in planets and satellites using a Maxwell viscoelastic rheology
2 Pith papers cite this work. Polarity classification is still indexing.
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abstract
In this paper we present a new approach to tidal theory. Assuming a Maxwell viscoelastic rheology, we compute the instantaneous deformation of celestial bodies using a differential equation for the gravity field coefficients. This method allows large eccentricities and it is not limited to quasi-periodic perturbations. It can take into account an extended class of perturbations, including chaotic motions and transient events. We apply our model to some already detected eccentric hot Jupiters and super-Earths in planar configurations. We show that when the relaxation time of the deformation is larger than the orbital period, spin-orbit equilibria arise naturally at half-integers of the mean motion, even for gaseous planets. In the case of super-Earths, these equilibria can be maintained for very low values of eccentricity. Our method can also be used to study planets with complex internal structures and other rheologies.
fields
astro-ph.EP 2years
2026 2representative citing papers
Revised mass of 0.503 M_Earth and radius of 0.736 R_Earth for GJ 367 b give a density of 6.9 g cm^{-3} and an iron fraction of 50-70% via new tidal and composition modeling.
citing papers explorer
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CHEOPS observations of V1298 Tau: updated planetary densities and implications on the early evolution of the young system
CHEOPS photometry improves radii for V1298 Tau b, c, and d, producing revised densities of 0.06-0.23 g cm^{-3} that indicate differential atmospheric evolution and no requirement for past dynamical excitation.