2026/02/01 by C. A. Denton, J. E. C. Scully, J. C. Castillo‐Rogez +6 · 1 voice
Earth and Planetary Sciences · Physics and Astronomy · #Astro and Planetary Science #Geological and Geochemical Analysis #Impact crater #Impact structure #Morphology (biology) #Planetary Science and Exploration #Solar System #Thermal
paper · doi:10.1029/2025je009282
openalex publication_date 2026/02/01 · openalex created_date 2026/02/10 · openalex updated_date 2026/05/21
Abstract The imaged portion of Umbriel's surface is dark and cratered, suggesting limited geologic activity. However, bright deposits occupying the Wunda impact crater may be of endogenic origin, similar to proposed cryovolcanic sources for fresh bright material occupying Occator crater on Ceres. Here, we model the formation of Wunda using iSALE‐2D. Our goal is to determine whether Wunda's inferred morphology is consistent with the interior structure predicted for Umbriel and whether Wunda's interior might originate from impact‐induced cryovolcanism and/or was sourced from a subsurface ocean. We find that, if Wunda is indeed a complex crater, as coarsely resolved imagery suggests, Umbriel's ice shell may have been much thinner (50 km) and/or warmer (240 K) than predicted at present or subject to significant structural/compositional differences, such as abundant volatiles. These results help assess the thermal evolution of the Uranian satellites as potential ocean worlds.