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About a dozen exoplanetary systems have been discovered with three or moreplanets participating in a sequence of mean-motion resonances. The unique andcomplex architectures of these so-called "resonant chains" motivate efforts tocharacterize their planets holistically. In this work, we perform acomprehensive exploration of the spin-axis dynamics of planets in resonantchains. Planetary spin states are closely linked with atmospheric dynamics andhabitability and are thus especially relevant to resonant chains likeTRAPPIST-1, which hosts several temperate planets. Considering a set ofobserved resonant chains, we calculate the equilibrium states of the planetaryaxial tilts ("obliquities"). We show that high obliquity states exist for$\sim60\%$ of planets in our sample, and many of these states can be stable inthe presence of tidal dissipation. Using case studies of two observed systems(Kepler-223 and TOI-1136), we demonstrate how these high obliquity states couldhave been attained during the initial epoch of disk-driven orbital migrationthat established the resonant orbital architectures. We show that theTRAPPIST-1 planets most likely have zero obliquities, with the possibleexception of planet d. Overall, our results highlight that both the orbital andspin states of resonant chains are valuable relics of the early stages ofplanet formation and evolution.

Spin Dynamics of Planets in Resonant Chains