Abstract
1988 Arecibo Observatory dual‐polarization radar images are presented for Western Eisila Regio, Venus. The polarization information and Pioneer‐Venus Orbiter reflectivity and altimetry data are analyzed for volcanic deposits on two 400–500 km radius constructs, Sif and Gula Montes. Many of the large effusive deposits studied appear to require superposed flows or multiple vents to explain the observed progression of roughness along their length. High Fresnel reflectivity material may be present along the summit region of Gula Mons and in an embayed tessera‐like region to the N. Radar‐dark units on the flanks of Sif Mons are inferred to be pyroclastic deposits, but radar‐dark features near the summits of both edifices are more consistent with very smooth lava flows. Higher spatial resolution Magellan data will be useful in testing these predictions.
Published Version
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call