The possibility of a giant impact on Venus

¹ Department of Astrophysics, University of Zürich, Winterthurerstrasse 190, 8057 Zürich, Switzerland
² Space Research & Planetary Sciences, University of Bern, Sidlerstr. 5, 3012 Bern, Switzerland
³ Department of Earth and Planetary Sciences, ETH Zürich, Sonneggstrasse 5, 8092 Zürich, Switzerland

^★ Corresponding author: mirco.bussmann@uzh.ch

Received: 4 June 2025
Accepted: 2 August 2025

Abstract

Giant impacts were common in the early evolution of the Solar System, and it is possible that Venus also experienced an impact. A giant impact on Venus could have affected its rotation rate and possibly its thermal evolution. In this work, we explored a range of possible impacts using smoothed particle hydrodynamics. We considered the final major collision, assuming that differentiation already occurred and that Venus consists of an iron core (30% of Venus’ mass) and a forsterite mantle (70% of Venus’ mass). We used differentiated impactors with masses ranging from 0.01 to 0.1 M_⊕, impact velocities between 10 and 15 km s⁻¹, various impact geometries (head-on and oblique), different primordial thermal profiles, and a range of pre-impact rotation rates of Venus. We analysed the post-impact rotation periods and debris disc masses to identify scenarios that can reproduce Venus’ present-day characteristics. Our findings show that a wide range of impact scenarios are consistent with Venus’ current rotation. These include head-on collisions on a non-rotating Venus and oblique, hit-and-run impacts by Mars-sized bodies on a rotating Venus. Importantly, collisions that match Venus’ present-day rotation rate typically produce minimal debris discs residing within Venus’ synchronous orbit. This suggests that the material would likely reaccrete onto the planet, preventing the formation of long-lasting satellites – which is consistent with Venus’ lack of a moon. We conclude that a giant impact can be consistent with both Venus’ unusual rotation and lack of a moon, potentially setting the stage for its subsequent thermal evolution.