Dynamics and Evolution of Venus' Mantle Through Time

The dynamics and evolution of Venus’ mantle are of first-order relevance for the origin and modification of the tectonic and volcanic structures we observe on Venus today. Solid-state convection in the mantle induces stresses into the lithosphere and crust that drive deformation leading to tectonic signatures. Thermal coupling of the mantle with the atmosphere and the core leads to a distinct structure with substantial lateral heterogeneity, thermally and compositionally. These processes ultimately shape Venus’ tectonic regime and provide the framework to interpret surface observations made on Venus, such as gravity and topography. Tectonic and convective processes are continuously changing through geological time, largely driven by the long-term thermal and compositional evolution of Venus’ mantle. To date, no consensus has been reached on the geodynamic regime Venus’ mantle is presently in, mostly because observational data remains fragmentary. In contrast to Earth, Venus’ mantle does not support the existence of continuous plate tectonics on its surface. However, the planet’s surface signature substantially deviates from those of tectonically largely inactive bodies, such as Mars, Mercury, or the Moon. This work reviews the current state of knowledge of Venus’ mantle dynamics and evolution through time, focussing on a dynamic system perspective. Available observations to constrain the deep interior are evaluated and their insufficiency to pin down Venus’ evolutionary path is emphasised. Future missions will likely revive the discussion of these open issues and boost our current understanding by filling current data gaps; some promising avenues are discussed in this chapter

VERITAS (Venus Emissivity, Radio Science, InSAR, Topography, and Spectroscopy): Surface Science Objectives

The VERITAS mission is designed to understand Venus’ evolution through acquiring foundational, high resolution global datasets including those that inform our understanding of Venus’ surface and interior. VERITAS is the first in a trio of #DecadeofVenus missions, launching in December of 2027 and acquiring data beginning in 2029

VERITAS (Venus Emissivity, Radio Science, InSAR, Topography, and Spectroscopy): A Selected Discovery Mission

VERITAS was selected as a Discovery class mission on June 2, 2021. It is designed to understand Venus’ evolution through acquiring foundational, high resolution global datasets. A deep understanding of planetary habitability requires identifying key factors that govern the environment over time. Venus is the ultimate control case for studying how Earth developed and maintained conditions suited to life. Venus is very likely to have had elements essential to habitability [1,2] such as (past) surface water and even a dynamo. Tectonism and volcanism, with associated outgassing and driven by a robust internal energy budget, very likely persist today. Current interactions among the interior, surface, and atmosphere may include exchange of volatiles

Habitability, Geodynamics, and the Case for Venus

Geodynamics, like Earth’s plate tectonics (PT), governs long-term planetary evolution and habitability. Beyond Earth, only Venus may have key elements of PT: subduction (the 1st step in PT) and continents. Revealing Venus’ geodynamics is key to understanding how PT began on Earth, and how to predict the geodynamic evolution of other rocky bodies