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The rotation of planets hosting atmospheric tides: from Venus to habitable super-earths
Earth and Planetary Astrophysics · Submitted 17 Nov 2016
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We demonstrate the strong impact of the atmospheric properties and of the rheology of the solid part on the rotational dynamics of Venus-like planets, highlighting the key role played by dissipative mechanisms in the stability of equilibrium configurations.
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The abstract, sentence by sentence
The competition between the torques induced by solid and thermal tides drives the rotational dynamics of Venus-like planets and super-Earths orbiting in the habitable zone of low-mass stars. The tidal responses of the atmosphere and telluric core are related to their respective physical properties and strongly depend on the tidal frequency. The resulting torque determines the possible equilibrium states of the planet's spin. We compute here an analytic expression for the total tidal torque exerted on a Venus-like planet. This expression is used to characterize the equilibrium rotation of the body. Close to the star, the solid tide dominates. Far from it, the thermal tide drives the rotational dynamics of the planet. The transition regime corresponds to the habitable zone, where prograde and retrograde equilibrium states appear. We demonstrate the strong impact of the atmospheric properties and of the rheology of the solid part on the rotational dynamics of Venus-like planets, highlighting the key role played by dissipative mechanisms in the stability of equilibrium configurations.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The competition between the torques induced by solid and thermal tides drives the rotational dynamics of Venus-like planets and super-Earths orbiting in the habitable zone of low-mass stars. | background 1.00 | 0.13 | 0.21 | asserted 1.00 |
| s1 | The tidal responses of the atmosphere and telluric core are related to their respective physical properties and strongly depend on the tidal frequency. | background 0.98 | 0.19 | 0.05 | asserted 1.00 |
| s2 | The resulting torque determines the possible equilibrium states of the planet's spin. | background 0.80 | 0.13 | 0.09 | asserted 0.98 |
| s3 | We compute here an analytic expression for the total tidal torque exerted on a Venus-like planet. | contribution 0.71 | 0.96 | 0.06 | asserted 0.99 |
| s4 | This expression is used to characterize the equilibrium rotation of the body. | method 0.75 | 0.76 | 0.06 | asserted 0.98 |
| s5 | Close to the star, the solid tide dominates. | result 0.97 | 0.64 | 0.06 | asserted 1.00 |
| s6 | Far from it, the thermal tide drives the rotational dynamics of the planet. | result 0.96 | 0.69 | 0.13 | asserted 1.00 |
| s7 | The transition regime corresponds to the habitable zone, where prograde and retrograde equilibrium states appear. | result 0.96 | 0.72 | 0.26 | asserted 0.99 |
| s8 | We demonstrate the strong impact of the atmospheric properties and of the rheology of the solid part on the rotational dynamics of Venus-like planets, highlighting the key role played by dissipative mechanisms in the stability of equilibrium configurations. | interpretation 0.59 | 0.89 | 0.73 | asserted 1.00 |
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Original abstract
The competition between the torques induced by solid and thermal tides drives the rotational dynamics of Venus-like planets and super-Earths orbiting in the habitable zone of low-mass stars. The tidal responses of the atmosphere and telluric core are related to their respective physical properties and strongly depend on the tidal frequency. The resulting torque determines the possible equilibrium states of the planet's spin. We compute here an analytic expression for the total tidal torque exerted on a Venus-like planet. This expression is used to characterize the equilibrium rotation of the body. Close to the star, the solid tide dominates. Far from it, the thermal tide drives the rotational dynamics of the planet. The transition regime corresponds to the habitable zone, where prograde and retrograde equilibrium states appear. We demonstrate the strong impact of the atmospheric properties and of the rheology of the solid part on the rotational dynamics of Venus-like planets, highlighting the key role played by dissipative mechanisms in the stability of equilibrium configurations.
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