Super-Earth LHS3844b is Tidally Locked

• Published in: The Astrophysical journal Vol. 964; no. 2; pp. 152 - 162
• Main Authors: Lyu, Xintong, Koll, Daniel D. B., Cowan, Nicolas B., Hu, Renyu, Kreidberg, Laura, Rose, Brian E. J.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.04.2024; IOP Publishing
• Subjects: Atmosphere; Circular orbits; Empirical analysis; Exoplanet surface characteristics; Exoplanet surfaces; Exoplanets; Extrasolar planets; Extrasolar rocky planets; Heating; Hypotheses; Impact analysis; Irradiation; Light curves; Mercury; Mercury (planet); Orbital resonances (celestial mechanics); Planetary rotation; Planets; Regolith; Solid body tides; Space weather; Space weathering; Terrestrial planets; Thermal analysis; Thermal models; Tidal effects; Tidal interaction; Weathering
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad2077

Abstract Short-period exoplanets on circular orbits are thought to be tidally locked into synchronous rotation. If tidally locked, these planets must possess permanent day- and night-sides, with extreme irradiation on the dayside and none on the nightside. However, so far the tidal locking hypothesis for exoplanets is supported by little to no empirical evidence. Previous work showed that the super-Earth LHS 3844b likely has no atmosphere, which makes it ideal for constraining the planet’s rotation. Here we revisit the Spitzer phase curve of LHS 3844b with a thermal model of an atmosphere-less planet and analyze the impact of nonsynchronous rotation, eccentricity, tidal dissipation, and surface composition. Based on the lack of observed strong tidal heating we rule out rapid nonsynchronous rotation (including a Mercury-like 3:2 spin–orbit resonance) and constrain the planet's eccentricity to less than ∼0.001 (more circular than Io's orbit). In addition, LHS 3844b’s phase curve implies that the planet either still experiences weak tidal heating via a small-but-nonzero eccentricity (requiring an undetected orbital companion), or that its surface has been darkened by space weathering; of these two scenarios we consider space weathering more likely. Our results thus support the hypothesis that short-period rocky exoplanets are tidally locked, and further show that space weathering can significantly modify the surfaces of atmosphere-less exoplanets.