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Triaxial Deformation and Asynchronous Rotation of Rocky Planets in the Habitable Zone of Low-Mass Stars
Rocky planets orbiting M-dwarf stars in the habitable zone tend to be driven to synchronous rotation by tidal dissipation, potentially causing difficulties for maintaining a habitable climate on the planet.
However, the planet may be captured into asynchronous spin-orbit resonances if it has sufficiently large intrinsic triaxial deformation. We derive the analytic expression for the maximum triaxiality of a rocky planet, with and without a liquid envelope, as a function of the planet’s radius, density, rigidity and critical strain of fracture.
The derived maximum triaxiality is consistent with the observed triaxialities for terrestrial planets in the solar system, and indicates that rocky planets in the habitable zone of M-dwarfs can in principle be in a state of asynchronous spin-orbit resonances.
J. J. Zanazzi, Dong Lai
(Submitted on 23 Feb 2017)
Comments: 7 pages, 3 figures, submitted to MNRAS
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:1702.07327 [astro-ph.EP] (or arXiv:1702.07327v1 [astro-ph.EP] for this version)
From: John Zanazzi
[v1] Thu, 23 Feb 2017 18:31:04 GMT (237kb)