Probing the Viscosity of Venus's Mantle From Dynamic Topography at Baltis Vallis

Abstract The Baltis Vallis channel on Venus preserves a record of long‐wavelength deformation generated by a convecting mantle, providing a unique window into the planet's geodynamics. Notably, the observed topography along the channel is not downhill, suggesting complex interactions between surface processes and mantle dynamics. We statistically compare the observed dynamic topography of Baltis Vallis with dynamic topographies generated by a suite of stagnant‐lid mantle convection models to constrain Venus' interior dynamics. Baltis Vallis's relatively young age (likely 250 Myr) and low root‐mean‐square relief of 217 m indicate vigorous convection in Venus's mantle, with a Rayleigh number 4 , implying a mantle viscosity 1–2 orders of magnitude lower than Earth's. This difference may result from either a water‐rich, less‐degassed interior or a higher‐temperature mantle beneath an insulating lid. Additionally, our simulations suggest that melt advection may dominate heat transport on Venus, potentially leading to non‐linear temperature profiles in the crust. Upcoming missions such as VERITAS and EnVision will deliver higher‐resolution gravity and topographic data, providing further constraints on Venus's present‐day internal dynamics and the origin of Baltis Vallis.