This image of the volcano Sapas Mons on Venus is based on images taken by the Soviet spacecraft Venera 13 and
Venera 14. Which of these events explains the presence of the volcano?
Answers
Answer:
Venus in Color
The bluish hue of Venus is an effect of the colorization technique used to enhance subtle contrasts in cloud patterns and indicates that this image was taken through a violet filter. Features in the sulfuric acid clouds near the top of the planet's atmosphere are most prominent in violet and ultraviolet light. This image shows the east to west cloud banding and the brighter polar hoods. The features are embedded in winds that flow from east to west at about 370 kph (230 mph).
Impact Craters
Three large impact craters with diameters ranging from 37 km (23 mi) to 65 km (40 mi) are visible in the fractured plains. Features typical of meteorite impact craters are also visible. Rough radar-bright ejecta surrounds the perimeter of the craters; terraced inner walls and large central peaks can be seen. Crater floors appear dark because they are smooth and have been flooded by lava. Domes of probable volcanic origin can be seen in the southeastern corner. The domes range in diameter from 1-12 km (0.6-7 mi); some have central pits typical of volcanic shields or cones.
Bright Plains
Located along the left central edge of the image is a cluster of volcanic domes that ranges from 1.5 km (1 mi) to 7.5 km in diameter (5 mi). The domes and their deposits are located at the convergence of radar-bright lineaments that are interpreted to be faults and troughs. In some places the domes overlie the faults. The faults and troughs extend into the lower part of the image where they terminate against dark plains deposits and are crosscut at right angles by additional faults. The relationship between these features indicates that multiple episodes of faulting and volcanism have occurred.
Ovda Regio
The tectonic fabric of this region of Ovda Regio trends predominantly east-west. The large radar-dark areas are probably tectonically formed basins that have been filled in by fluid lava flows, thus presenting a smooth surface to the Magellan radar system.
Ridges and Troughs
On this bright, lineated terrain Alpha Regio is a series of troughs, ridges, and faults running in every direction. The lengths of these features range from 10 km (6.3 mi) to 60 km (37 mi). The elevation of Alpha Regio varies over a range of 4 km (2.5 mi). Low-lying areas appear dark in the radar images and may be filled with lava. Volcanoes appear as bright spots on the smooth plains. Notice the large volcano in the upper right. At the center of this 35 km (22 mi) volcano is a caldera; its western edge appears to be either a debris flow or a lava flow. The black square represents missing data.
Highlands
Several tectonic events formed this complex terrain, which is part of the interior of Ovda Regio. An underlying fabric of ridges and valleys lies NE-SW. These ridges are spaced 10-20 km (6-12 mi) apart and may have been caused by compression of the crust at right angles to the ridge. The ridges are cut by bright features extending NW-SE. The largest valleys, particularly the 20 km (12 mi) wide valley extending across the image, were filled with dark material, probably lava. The complexity of Ovda Regio attests to a long history of tectonic deformation.
Eastern Lakshmi
Lava flows blanket the flat plains region of eastern Lakshmi. The dark flows most likely represent smooth flows similar to pahoehoe flows on Earth, while the brighter areas are rougher flows resembling Earth's aa flows. Three dark splotches mark the tops of these lava flows. Because of the thick atmosphere surrounding Venus, small impactors break up before they hit the surface. The fragments are deposited over the surface and produce the dark splotches seen here. Notice the splotch on the far right has a crater at its center, indicating that the impactor was not completely destroyed.