New mapping along Ishtar Terra margins: use and limits of Magellan SAR data for testing Venus crustal plateau formation models
Abstract
The origins of crustal plateaus on Venus are poorly understood. Several formation models have been proposed, including four previously explored models: downwelling, upwelling, pulsating continents, and bolide impact models; as well as a waning heat-pipe model. Key predictions which vary across models include surface deformation, marginal deformation, and the tessera-plain onlapping relationships. Addressing this problem, we perform detailed mapping of five sites along the margin of Ishtar Terra, the highland region holding Venus’s highest peak, focusing on identifying surface units and sets of deformation lineaments. This work indicates that all tessera units and associated deformations are embayed by lava plains in four out of five studied areas. Plains-forming volcanism occurs after, or outlasts, all crustal plateau tectonism, which is consistent with three models: the pulsating continents, waning heat-pipe, and upwelling models. At the fifth site, tessera units appear to be embayed by plains, but it is also possible that this boundary is a linear fault system. Deformation relationships alone are unable to test models as they show a large variance in possible deformational histories given significant radar data uncertainties. A two times higher resolution radar imagery (i.e., 40 meters/pixel) and an order of magnitude better resolution topographic map (i.e., 450 meters/pixel) will be necessary to more rigorously test models via embayment relationships and deformation patterns. Our mapping also identifies some new features, including (1) embayment of tessera fractures alone on lava plains, as well as (2) 10-20 km long and 2-5 km wide eye-pattern ridges, composed of (3) V-shape lineaments.
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BibTeX
@misc{hansen2026mapping,
title = {{New mapping along Ishtar Terra margins: use and limits of Magellan SAR data for testing Venus crustal plateau formation models}},
author = {Hiu Ching Jupiter Hansen and Alex Webb and Joseph R. Michalski and William B. Moore},
howpublished = {EarthArXiv},
year = {2026},
month = sep,
doi = {10.31223/x56b94},
url = {https://eartharxiv.org/repository/view/15151/},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - New mapping along Ishtar Terra margins: use and limits of Magellan SAR data for testing Venus crustal plateau formation models
AU - Hiu Ching Jupiter Hansen
AU - Alex Webb
AU - Joseph R. Michalski
AU - William B. Moore
PY - 2026
DA - 2026/09/24
PB - EarthArXiv
DO - 10.31223/x56b94
UR - https://eartharxiv.org/repository/view/15151/
AB - The origins of crustal plateaus on Venus are poorly understood. Several formation models have been proposed, including four previously explored models: downwelling, upwelling, pulsating continents, and bolide impact models; as well as a waning heat-pipe model. Key predictions which vary across models include surface deformation, marginal deformation, and the tessera-plain onlapping relationships. Addressing this problem, we perform detailed mapping of five sites along the margin of Ishtar Terra, the highland region holding Venus’s highest peak, focusing on identifying surface units and sets of deformation lineaments. This work indicates that all tessera units and associated deformations are embayed by lava plains in four out of five studied areas. Plains-forming volcanism occurs after, or outlasts, all crustal plateau tectonism, which is consistent with three models: the pulsating continents, waning heat-pipe, and upwelling models. At the fifth site, tessera units appear to be embayed by plains, but it is also possible that this boundary is a linear fault system. Deformation relationships alone are unable to test models as they show a large variance in possible deformational histories given significant radar data uncertainties. A two times higher resolution radar imagery (i.e., 40 meters/pixel) and an order of magnitude better resolution topographic map (i.e., 450 meters/pixel) will be necessary to more rigorously test models via embayment relationships and deformation patterns. Our mapping also identifies some new features, including (1) embayment of tessera fractures alone on lava plains, as well as (2) 10-20 km long and 2-5 km wide eye-pattern ridges, composed of (3) V-shape lineaments.
ER -