Determination of Venus’ Interior Structure with EnVision

Rosenblatt, P.; Dumoulin, Caroline; Marty, Jean‐Charles; Genova, Antonio

doi:10.3390/rs13091624

Cited by 21 publications

(10 citation statements)

References 36 publications

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“…VERITAS will measure global topography and gravity at much improved resolution over presently available data. EnVision will also measure topography and gravity (e.g., Rosenblatt et al 2021). Such refined data is expected to inform models on upper-mantle density anomalies, crustal thickness, and eventually elastic thickness from which thermal gradients and thus surface heat flux can be estimated.…”

Section: How Much Heat Does Venus Lose Today?mentioning

confidence: 99%

Dynamics and Evolution of Venus’ Mantle Through Time

et al. 2022

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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.

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Section: How Much Heat Does Venus Lose Today?mentioning

confidence: 99%

Dynamics and Evolution of Venus’ Mantle Through Time

et al. 2022

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“…VERITAS and EnVision are specifically dedicated to studying the surface and deep interior of Venus with radio science, radar and infrared spectroscopy. Among other things, the combined processing of Earth Doppler tracking and radar data will allow accurate determination of the planet's rotational state and moment of inertia factor in addition to the much more accurate determination of the Love number k2 from tracking alone (Rosenblatt et al 2021;Cascioli et al 2021). VERITAS will provide accuracies ( 3 ) in the estimates of the tidal Love number k 2 to 4.6 × 10 −4 , its tidal phase lag to 0.05 • , and the moment of inertia factor to 9.8 × 10 −4 (0.3% of the expected value) (Cascioli et al 2021).Those results will place much tighter constraints on the state and size of the core and the viscous response of the planet than is currently the case as shown in the analysis by Dumoulin et al (2017).…”

Section: Venusmentioning

confidence: 99%

Interiors of Earth-Like Planets and Satellites of the Solar System

Breuer¹,

Spohn

Hoolst

et al. 2021

Surv Geophys

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The Earth-like planets and moons in our solar system have iron-rich cores, silicate mantles, and a basaltic crust. Differentiated icy moons can have a core and a mantle and an outer water–ice layer. Indirect evidence for several icy moons suggests that this ice is underlain by or includes a water-rich ocean. Similar processes are at work in the interiors of these planets and moons, including heat transport by conduction and convection, melting and volcanism, and magnetic field generation. There are significant differences in detail, though, in both bulk chemical compositions and relative volume of metal, rock and ice reservoirs. For example, the Moon has a small core [~ 0.2 planetary radii (RP)], whereas Mercury’s is large (~ 0.8 RP). Planetary heat engines can operate in somewhat different ways affecting the evolution of the planetary bodies. Mercury and Ganymede have a present-day magnetic field while the core dynamo ceased to operate billions of years ago in the Moon and Mars. Planets and moons differ in tectonic style, from plate-tectonics on Earth to bodies having a stagnant outer lid and possibly solid-state convection underneath, with implications for their magmatic and atmosphere evolution. Knowledge about their deep interiors has improved considerably thanks to a multitude of planetary space missions but, in comparison with Earth, the data base is still limited. We describe methods (including experimental approaches and numerical modeling) and data (e.g., gravity field, rotational state, seismic signals, magnetic field, heat flux, and chemical compositions) used from missions and ground-based observations to explore the deep interiors, their dynamics and evolution and describe as examples Mercury, Venus, Moon, Mars, Ganymede and Enceladus.

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“…This result, although pathbreaking, does not allow us to determine the size of the core with useful accuracy (e.g., ∼ 3,500 ± 500 km). Fortunately, future Venus missions should improve this measurement of Venus's MoI thanks to radio science alone (e.g., Rosenblatt et al 2021) or radio science coupled with radar imagery (e.g., Cascioli et al 2021).…”

Section: Basic Properties Of the Interiormentioning

confidence: 99%

Venus, the Planet: Introduction to the Evolution of Earth’s Sister Planet

et al. 2023

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Venus is the planet in the Solar System most similar to Earth in terms of size and (probably) bulk composition. Until the mid-20th century, scientists thought that Venus was a verdant world—inspiring science-fictional stories of heroes battling megafauna in sprawling jungles. At the start of the Space Age, people learned that Venus actually has a hellish surface, baked by the greenhouse effect under a thick, CO2-rich atmosphere. In popular culture, Venus was demoted from a jungly playground to (at best) a metaphor for the redemptive potential of extreme adversity. However, whether Venus was much different in the past than it is today remains unknown. In this review, we show how now-popular models for the evolution of Venus mirror how the scientific understanding of modern Venus has changed over time. Billions of years ago, Venus could have had a clement surface with water oceans. Venus perhaps then underwent at least one dramatic transition in atmospheric, surface, and interior conditions before present day. This review kicks off a topical collection about all aspects of Venus’s evolution and how understanding Venus can teach us about other planets, including exoplanets. Here we provide the general background and motivation required to delve into the other manuscripts in this collection. Finally, we discuss how our ignorance about the evolution of Venus motivated the prioritization of new spacecraft missions that will rediscover Earth’s nearest planetary neighbor—beginning a new age of Venus exploration.

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Determination of Venus’ Interior Structure with EnVision

Cited by 21 publications

References 36 publications

Dynamics and Evolution of Venus’ Mantle Through Time

Dynamics and Evolution of Venus’ Mantle Through Time

Interiors of Earth-Like Planets and Satellites of the Solar System

Venus, the Planet: Introduction to the Evolution of Earth’s Sister Planet

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