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A planet's climate can be strongly affected by its orbital eccentricity andobliquity. Here we use a 1-dimensional energy balance model modified to includea simple runaway greenhouse (RGH) parameterization to explore the effects ofthese two parameters on the climate of Earth-like aqua planets - completelyocean-covered planets - orbiting F-, G-, K-, and M-dwarf stars. We find thatthe range of instellations for which planets exhibit habitable surfaceconditions throughout an orbit decreases with increasing eccentricity. However,the appearance of temporarily habitable conditions during an orbit creates aneccentric habitable zone (EHZ) that is sensitive to orbital eccentricity andobliquity, planetary latitude, and host star spectral type. We find that thefraction of a planet's orbit over which it exhibits habitable surfaceconditions is larger on eccentric planets orbiting M-dwarf stars, due to thelower broadband planetary albedos of these planets. Planets with largerobliquities have smaller EHZs, but exhibit warmer climates if they do not entera snowball state during their orbits. We also find no transient runawaygreenhouse state on planets at all eccentricities. Rather, planets spend theirentire orbits either in a RGH or not. For G-dwarf planets receiving 100% of themodern solar constant and with eccentricities above 0.55, an entire Earth oceaninventory can be lost in 3.6 Gyr. M-dwarf planets, due to their larger incidentXUV flux, can become desiccated in only 690 Myr with eccentricities above 0.38.This work has important implications for eccentric planets that may exhibitsurface habitability despite technically departing from the traditionalhabitable zone as they orbit their host stars.

Habitability and Water Loss Limits on Eccentric Planets Orbiting Main Sequence Stars