paper

Post-Keplerian obliquity variations and the habitability of rocky planets orbiting fast spinning, oblate late M dwarfs

arXiv:2102.07815

Abstract

A couple of dozen Earth-like planets orbiting M dwarfs have been discovered so far. Some of them have attracted interest because of their potential long-term habitability; such a possibility is currently vigorously debated in the literature. I show that post-Keplerian (pK) orbit precessions may impact the habitability of a fictitious telluric planet orbiting an oblate late-type M dwarf of spectral class M9V with at , corresponding to an orbital period , inducing long-term variations of the planetary obliquity which, under certain circumstances, may not be deemed as negligible from the point of view of life's sustainability. I resume the analytical orbit-averaged equations of the pK precessions, both classical and general relativistic, of the unit vectors of both the planet's spin and orbital angular momenta entering , and numerically integrate them by producing time series of the pK changes of the obliquity. For rapidly rotating M dwarfs with rotational periods of the order of , the planet's obliquity can undergo classical pK large variations up to tens of degrees over timescales , depending on the mutual orientations of the star's spin , of , and of . Instead, are for the planet b of the Teegarden's Star. In certain circumstances, the M dwarf's oblateness should be considered as one of the key dynamical features to be taken into account in compiling budgets of the long-term habitability of rocky planets around fast spinning late M dwarfs. (Abridged)

LaTex2e, 26 pages, 6 figures, no tables. Changes suggested by an anonymous referee implemented

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