Abstract: The Solar System furnishes the most familiar planetary architecture: many planets, orbiting nearly coplanar to one another. However, a typical system of planets in the Milky Way orbits a much smaller M dwarf. M dwarf hosts create very different conditions for their planetary systems than Sunlike stars, in ways that make dynamical information crucial. A planet orbiting a star 25% the mass of the Sun must orbit only 0.1 AU away to receive Earthlike insolation: this necessary proximity of the “habitable zone” to the star means that tides, whether due to planetary orbital eccentricity or spin obliquity, play an outsized role for temperate planets orbiting M dwarfs. Most temperate planets orbiting M dwarfs are assumed to have undergone tidal locking, though a permanent cold, night side and a roasting day side presents a potentially severe threat to habitability. Yet, tidal locking need not be the default assumption when planets retain non-zero spin obliquity. I will describe how a particular spin-orbit resonance, capture into Cassini State 2, is both (1) plausibly common in M dwarf multi planet systems and (2) relevant for planets in the habitable zone of M dwarfs. This effect, by which a high obliquity can be sustained over long timescale, can also ward off tidal locking. This finding challenges the near-universal assumption of tidal locking for temperate M dwarf planets, with important implications for atmospheric circulation.