No Snowball on Habitable Tidally Locked Planets with a Dynamic Ocean
arXiv:1910.06285 · doi:10.3847/2041-8213/ab487d
Abstract
Terrestrial planets orbiting within the habitable zones of M-stars are likely to become tidally locked in a 1:1 spin:orbit configuration and are prime targets for future characterization efforts. An issue of importance for the potential habitability of terrestrial planets is whether they could experience snowball events (periods of global glaciation). Previous work using an intermediate complexity atmospheric Global Climate Model (GCM) with no ocean heat transport suggested that tidally locked planets would smoothly transition to a snowball, in contrast with Earth, which has bifurcations and hysteresis in climate state associated with global glaciation. In this paper, we use a coupled ocean-atmosphere GCM (ROCKE-3D) to model tidally locked planets with no continents. We chose this configuration in order to consider a case that we expect to have high ocean heat transport. We show that including ocean heat transport does not reintroduce the snowball bifurcation. An implication of this result is that a tidally locked planet in the habitable zone is unlikely to be found in a snowball state for a geologically significant period of time.
Accepted at ApJL Sept 25 2019
References in corpus (8)
- Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1
- A terrestrial planet candidate in a temperate orbit around Proxima Centauri
- The habitability of Proxima Centauri b II. Possible climates and Observability
- Atmospheric dynamics of Earth-like tidally locked aquaplanets
- Constraints on Climate and Habitability for Earth-like Exoplanets Determined from a General Circulation Model
- Water Trapping on Tidally Locked Terrestrial Planets Requires Special Conditions
- Ocean Dynamics and the Inner Edge of the Habitable Zone for Tidally Locked Terrestrial Planets
- Spectrum-driven Planetary Deglaciation Due to Increases in Stellar Luminosity