Figure 1 – The figure displays an elevation model of Idunn Mons (46 S; 146 W), a volcano with a diameter of 200 km located at Imdr Regio on Venus. Credit: NASA/JPL-Caltech/ESA
The European Space Agency’s Venus Express mission has provided a great amount of data from the surface and atmosphere of Earth’s inner twin planet. Among these observations was the mapping of the southern hemisphere of Venus in the near infrared spectral range using the VIRTIS (Visible and InfraRed Thermal Imaging Spectrometer) instrument. However the thick and permanent cloud cover of Venus limits the achievable resolution, similar to observing a scene through fog. Using a numerical model, planetary researchers at the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt, DLR) pushed the limits of the data resolution. With this new technique the emissivity anomalies were analyzed on the top and eastern flank of Idunn Mons, a volcano with a diameter of 200 kilometers at its base situated in the southern hemisphere of Venus. These anomalies provide an indication of geologically recent volcanism in this area.
“We could identify and map distinctive lava flows from the top and eastern flank of the volcano, which might have been recently active in terms of geologic time,” says Piero D’Incecco, planetary researcher at the DLR who is presenting these results today at the joint 48th meeting of the American Astronomical Society’s Division for Planetary Sciences (DPS) and 11th European Planetary Science Congress in Pasadena, California.
“With our new technique we could combine the infrared data with much higher-resolution radar images from the NASA Magellan mission, having been in orbit about Venus from 1990 until 1992. It is the first time that—combining the datasets from two different missions—we can perform a high resolution geologic mapping of a recently active volcanic structure from the surface of a planet other than Earth.” This study will also provide motivation for future projects focused on the exploration of Venus, as for example the NASA Discovery VERITAS mission proposal or the ESA EnVision M5 mission proposal that—in combining high-resolution radar and near-infrared mapping—will extend the frontiers of our current knowledge of the geology of Venus.
Search for Location and Extent of the Lava Flows
From 2006 until 2014 the ESA Venus Express probe was analyzing the atmosphere and surface of Earth’s twin planet. The Visible and InfraRed Thermal Imaging Spectrometer (VIRTIS) has provided data that indicate the occurrence of recent volcanic activity on Venus. DLR scientists Piero D’Incecco, Nils Mueller, Joern Helbert and Mario D’Amore selected the eastern flank of Idunn Mons—Imdr Regio’s single large volcano—as the study area, since it was identified in VIRTIS data as one of the regions with relatively high values of thermal emissivity at 1 micron wavelength.
Using the capabilities of specific techniques developed in the Planetary Spectroscopy Laboratory group at DLR in Berlin, the study intends to identify location and extent of the sources of such anomalies, thus the lava flows responsible for the relatively high emissivity observed by VIRTIS over the eastern flank of Idunn Mons. Therefore the lava flow units on the top and eastern flank of Idunn Mons are mapped, varying the values of simulated 1 micron emissivity assigned to the mapped units. For each configuration the total mismatch as root mean square error in comparison with the VIRTIS observations is calculated. In the best-fit configuration, the flank lava flows are characterized by high values of 1 micron simulated emissivity. Hence, the lava flow units on the eastern flank on Idunn Mons are likely responsible for the relatively high 1 micron emissivity anomalies observed by VIRTIS. This result is supported by the reconstructed post-eruption stratigraphy, displaying the relative dating of the mapped lava flows, that is independent of the 1 micron emissivity modeling. Values of average microwave emissivity extracted from the lava flow units range around the global mean, which is consistent with dry basalts.
Figure 3 – Geologic map of the eastern flank of Idunn Mons (46 S; 146 W), displaying the five lava flow units (lfu) identified during the mapping process. Lfu are classified from a to e. Lfu-a represents the summit composite unit of Idunn Mons, while the lfu-b, lfu-c, lfu-d and lfu-e are flank units of the volcanic edifice. Credit: NASA/JPL-Caltech/ESA/DLR
Source: Europlanet Media Centre
Joint 48th annual meeting of the Division for Planetary Sciences (DPS) of the American Astronomical Society (AAS) and 11th annual European Planetary Science Congress (EPSC), Abstract [105.03D]. Recently Active Lava Flows on the Eastern Flank of Idunn Mons on Venus, Piero D’Incecco (German Aerospace Center).