An evaluation of models for Martian gully formation using remote sensing and in situ measurments of Svalbard analogs.
Författare och institution:
Ella Carlsson (-); Henrik Johansson (-); Andreas Johnsson (Institutionen för geovetenskaper); Jennifer Heldmann (-); Chris McKay (-); Mats Olvmo (Institutionen för geovetenskaper); S. Fredriksson (-); H.T. Schmidt (-)
Lunar and Planetary Science Conference 39, XXXIX ( 1852 )
The newly discovered gully systems on Mars have been found on rather young geologi-cal surfaces such as dunes and polygons. This in combination with the general absence of superimposed impact craters suggests that the gullies are relatively young geological features. Their morphology indicates that they have been eroded by a liquid fluid, most probably water. A recent discovery suggests that gully formation is an ongoing process, which appears to occur even today. This is a paradox since water in current Martian atmospheric conditions cannot be found in a stable form on the surface due to the low pressure and temperature during normal conditions.
Several formation mechanisms have been proposed for the Martian gullies such as liquid carbon dioxide reservoirs, shallow liquid water aquifer, melting ground ice, dry landslide, snow melt and deep liquid water aquifer. However, none of these models can alone explain all the gullies discovered on Mars. So far Martian gullies have only been studied from high orbit via satellites.
Gullies found in Arctic climates on Earth could be an equitable analog for the Martian gullies and a com-parative analysis could help disclose the formation mechanisms of the Martian gullies as well as their eroding agent.
Ämne (baseras på Högskoleverkets indelning av forskningsämnen):
Astronomi, astrofysik och kosmologi ->
Geovetenskap och miljövetenskap
Geovetenskap och miljövetenskap ->
Meteorologi och atmosfärforskning
Mars, gully, ice, climate change, snow melt
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