The recently selected NASA VERITAS and DAVINCI missions, the ESA EnVision, the Roscosmos Venera-D will open a new era in the exploration of Venus. One of the key targets of the future orbiting and in-situ investigations of Venus is the identification of volcanically active areas on the planet. The study of the areas characterized by recent or ongoing volcano-tectonic activity can inform us on how volcanism and tectonism are currently evolving on Venus. Following this key target, the manuscript by Brossier et al. (2022) (https://doi.org/10.1029/2022GL099765) extends the successful approach and methodology used by previous works to Ganis Chasma in Atla Regio. We comment here on the main results of the manuscript published by Brossier et al. (2022) (https://doi.org/10.1029/2022GL099765) and discuss the important implications of their work for the future orbiting and in-situ investigation of Venus. Their results add further lines of evidence indicating possibly recent volcanism on Venus.

Combining geologic mapping and stratigraphic reconstruction of lava flows at Sapas, Maat and Ozza Montes, three potentially young volcanic structures of Atla Regio on Venus, with analysis of the spectral signature (radar emissivity anomalies) characterizing each mapped flow, Brossier et al. (2021) conclude that some of the lava flows at Maat Mons may be geologically recent (~25 Ma). The lava flows of Sapas and Ozza Montes are more consistent with weathered lava flows forming chlorapatite and some perovskite oxides. We discuss the reasons why, besides the importance of the results they obtained, the methodology they used can be very valuable for future investigations with higher resolution datasets. The importance of combining geologic interpretation with spectral analysis in the reconstruction of the volcanic history of Venus Considering its size, gravity and the presence of an atmosphere, Venus is typically considered as the twin sister of the Earth, but despite the apparent similarities with our planet, Venus is notably different because it is characterized by its extreme surface environment. With 90 bars and 475 °C, its surface is a very inhospitable place for life as we know it. Venus does not show evidence for a present plate tectonics-like activity, having a major part of its surface volcanic deposits younger than 300 Ma. It has been hypothesized that Venus underwent a catastrophic event of global resurfacing about 300 Ma ago, which may have almost entirely rejuvenated its surface (Schaber, 1992; Nimmo and McKenzie, 1998; Romeo and Turcotte, 2010; Strom et al., 1994; Turcotte et al., 1999). Some other studies instead favor a more equilibrium resurfacing model of the surface (Phillips et al, 1992; Phillips and Hansen, 1994; Bjonnes et al., 2012; O’Rourke and Korenaga, 2015). It is also possible that the past volcanic history of Venus somehow reflected an intermediate situation between these two end-member scenarios. Related to this topic, there has been a subject of debate whether or not the volcanism on Venus is currently evolving toward an equilibrium stage, with occurrences of smaller and more frequent localized eruptions. In this regard, it is vital to identify areas with current or recent volcanism, to measure the actual rate and volume of the most recent volcanic eruptions. The geologic interpretation and analysis of spectral signatures (both in radar and infrared wavelengths) can help us constraining the age of surface volcanic deposits on Venus. In geology, the so called “cross-cutting interrelationships” can constrain the relative age of two lava flows as it has been applied to young, possibly very recent lava flows and tectonic features on

We present a 1:10M scale map of the Niobe Map Area (NMA) of Venus (0N-57N/60E-80E). Geologic mapping employed NASA Magellan synthetic aperture radar and altimetry data. The NMA geologic map, and its companion Aphrodite Map Area (AMA), cover ~25% of Venus’ surface, providing with an important and unique perspective to study global and regional geologic processes. Both areas display a regional coherence of preserved geologic patterns that record three sequential geologic eras: the ancient era, the Artemis superstructure era, and the youngest fracture zone era. The NMA preserves a limited record of the fracture zone era, contrary to the AMA. However, the NMA host a diverse and rich assemblage of material and structures of the ancient era, and structures that define the Artemis superstructure era, with a footprint covering more than 25 percent of the surface of Venus. These two eras likely overlap in time and account for the formation of basement materials and lower plain units. Impact craters formed throughout the NMA recorded history. Approximately 40% of the impact craters show interior flood deposits, indicating that a significant number of NMA impact craters experienced notable geological events after impact crater formation. This and other geologic relations record a geohistory inconsistent with postulated global catastrophic resurfacing. Together, the NMA and the AMA record a rich geologic history of the surface of Venus that provide a framework to formulate new working hypotheses of Venus evolution, an to plan future studies of the planet.

We present a 1:10M scale geologic map of the Aphrodite Map area (AMA) of Venus (0N-57S /60E-80E). Geologic mapping employed NASA Magellan synthetic aperture radar and altimetry data. The AMA geologic map, with detailed structural elements and geologic units covering over one eighth of Venus’ surface, affords an important and unique perspective to test models of global scale geologic processes through time. Geologic relations record a history inconsistent with global catastrophic resurfacing. The AMA displays a regional coherence of preserved geologic patterns that record three sequential geologic eras: the ancient era, the Artemis superstructure era, and the youngest fracture zone era. The ancient era and Artemis superstructure, with a footprint covering more than 25 percent of the surface, are recorded in the Niobe map area to the north. The latter two eras likely overlap in time. The fracture zone domain, part of a globally extensive province, marks the most spatially focused tectonomagmatic domain within the AMA. Impact craters are both cut by, and overprint, fracture zone structures. Twelve percent of AMA impact craters that occur within the fracture zone domain predate or formed during fracture zone development. This observation indicates the relative youth of the fracture zone era and is consistent with the possibility that this domain remains geologically active. The AMA records a rich geologic history of large tract of the surface of Venus and provides an important framework to formulate new working hypotheses of Venus evolution, and contribute to planning future studies of the surface of planets.