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Large channels, apparently formed by episodes of flooding, exist primarily in the equatorial regions of Mars. Craters and other landforms were obstacles to these floodwaters and consequently experienced modification during the flooding. Highstanding rim topography channeled the rushing floodwaters around the crater. The tadpole-like tails behind the craters result from decreased erosion in the lee of the crater. The water flowed from left to right in this image. Crater is 15
km in diameter and located at 22.49° N, 31.42° W; Viking Orbiter
frame 827A21 Right
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