Figure 13: The topmost strong layer is interrupted by a crater, but is seen on either side of it on the chasma slope, and may be present within the bowl of the crater itself. (a) Portion of THEMIS nighttime IR image I07486008. The bowl of the crater is dark and therefore has a lower temperature relative to the surrounding terrain. These temperatures may mean that there is more lower-thermal-inertia dust within the crater than outside. However, a bright layer can be seen within the bowl of the crater that could correspond to the topmost strong layer. (b) Portion of THEMIS VIS image V06831002, the black boxes show the locations of c and d. (c) Portion of MOC image M02/03108. A faint hint of a break in the slope of the crater 75 m in elevation below the rim height, the arrows indicate this slope break. Slope break may be the expression of the topmost layer in the crater. (d) Portion of MOC image M09/04413. The topmost strong layer is evident here below a 100 m thickness of weaker materials.
Return to Layering stratigraphy of eastern Coprates and northern Capri Chasmata, Mars.
A version of this figure was published by Elsevier Inc. Copyright © 2005 Ross A. Beyer.