Spin states and climates of eccentric exoplanets

The known extrasolar planets exhibit a wide range of orbital eccentricities e. This has a profound influence on their rotations and climates. Because of tides in their interiors, mostly solid exoplanets are expected eventually to despin to a state of spin-orbit resonance, where the orbital period is some integer or half-integer times the rotation period. The most important of these resonances is the synchronous state, where the planetʹs spin period exactly equals its orbital period (like Earthʹs Moon, and indeed most of the regular satellites in the Solar System). Such planets seem doomed to roast on one side and freeze on the other. However, synchronous planets rock back and forth by an angle of ∼ 2 Arcsin e with respect to the sub-stellar point. For e = 0.055 (as for the Moon), this optical libration amounts to only ∼6°; but for a synchronous planet with e = 0.50 , for example, it would rise to ∼59°. This greatly expands the temperate “twilight zone” near the terminator and considerably improves the planetʹs prospects for habitability. For e ≳ 0.72389 , the optical libration exceeds 90°; for such planets, the sector of permanent night vanishes, while the sunniest region splits in two. Furthermore, the synchronous state is not the only possible spin resonance. For example, Mercury (with e ≈ 0.206 ) has an orbital period exactly 1.5 times its rotation period. A terrestrial exoplanet with e = 0.40 , say, is liable to have an orbital period of 2.0, 2.5, or 3.0 times its spin period. The corresponding insolation patterns are generally complicated, and all different from the synchronous state. Yet these non-synchronous resonances also protect certain longitudes from the worst extremes of temperature and solar radiation, and improve the planetʹs habitability, compared to non-resonant rotation. These results also have implications for the direct detectability of extrasolar planets, and the interpretation of their thermal emissions.