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Saturn's largest moon, Titan, has an Earth-like volatile cycle, but withmethane playing the role of water and surface liquid reservoirs geographicallyisolated at high latitudes. We recreate Titan's characteristic dry hydroclimateat the equator of an Earth-like climate model without seasons and with water asthe condensable by varying a small set of planetary parameters. We use threeobservationally motivated criteria for Titan-like conditions at the equator: 1)the peak in surface specific humidity is not at the equator, despite it havingthe warmest annual-mean temperatures; 2) the vertical profile of specifichumidity in the equatorial column is nearly constant through the lowertroposphere; and 3) the relative humidity near the surface at the equator issignificantly lower than saturation (lower than 60%). We find that simplyreducing the available water at the equator does not fully reproduce Titan-likeconditions. We additionally vary the rotation period and volatility of water tomimic Titan's slower rotation and more abundant methane vapor. Longer rotationperiods coupled with a dry equatorial surface meet fewer of the Titan-likecriteria than equivalent experiments with shorter rotation periods. Experimentswith higher volatility of water meet more criteria than those with lowervolatility, with some of those with the highest volatility meeting all three,demonstrating that an Earth-like planet can display Titan-like climatology bychanging only a few physical parameters.

Effects of Varying Land Coverage, Rotation Period, and Water Vapor on Equatorial Climates that Bridge the Gap between Earth-like and Titan-like