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PIA03904: Nepenthes Mensae
This NASA Mars Odyssey image shows a location near the highland-lowland boundary scarp in a region called Nepenthes Mensae with relatively smooth plains dotted with some craters and stepped mesas and knobs.
 Target Name:  Mars
 Is a satellite of:  Sol (our sun)
 Mission:  2001 Mars Odyssey 
 Spacecraft:  2001 Mars Odyssey
 Instrument:  THEMIS 
 Product Size:  320 x 1393 pixels (w x h) 
 Produced By:  Arizona State University 
 Producer ID:  20020723A  
 Full-Res TIFF:  PIA03904.tif (381.3 kB)
 Full-Res JPEG:  PIA03904.jpg (57.29 kB)  

Click on the image above to download a moderately sized image in JPEG format (possibly reduced in size from original)

Original Caption Released with Image:


(Released 23 July 2002)
This image shows relatively smooth plains dotted with some craters and stepped mesas and knobs. This image is located near the highland-lowland boundary scarp in a region called Nepenthes Mensae. These eroded mesas and knobs commonly display a stepped topography. Some of these mesas and knobs have flat ledges partway up their slopes. These ledges are made of more resistant layers of rock and are the last remnants of layers that once were continuous across this entire region. Erosion has completely removed these layers in most places, leaving behind only the small isolated mesas and knobs. This one band IR (band 9 at 12.6 microns) image shows some minor bright and dark textures, which are primarily due to differences in the abundance of rocks on the surface. No significant variation in thermophysical properties of surface materials is visible in this image. The relative uniformity of the surface properties suggests that a process (or processes) has mantled or homogenized the surface layer. The mantling layer in this region is most likely dust. The relatively cool (dark) regions during the day are rocky or indurated materials whereas fine sand and dust are warmer (bright). The brightness levels show daytime surface temperatures, which range from about minus 39 degrees to minus 17 degrees Celsius (minus 38 degrees to plus 1 degrees Fahrenheit). Many of the temperature variations are due to slope effects, with sun-facing slopes warmer than shaded slopes. The dark rings around several of the craters are due to the presence of rocky (cool) material ejected from the crater (best seen near bottom of image).

Daytime temperature variations are produced by a combination of topographic (solar heating) and thermophysical (thermal inertia and albedo) effects. The surface morphologies seen in THEMIS daytime IR images due to topographic heating are similar to those seen in previous imagery and MOLA topography.
Image Credit:
NASA/JPL/Arizona State University

Image Addition Date:
2002-07-24