Potentially habitable flow-like features from Martian dry ice geyser dune spots: Difference between revisions

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==Southern hemisphere flow-like features==
==Southern hemisphere flow-like features==

This image shows the flow like features of the southern hemisphere.

{{Wide image | Flow-like-features.gif | 549 px | Flow-like features in Dunes on Richardson Crater, Mars. They form around the dark dune spots, in the debris of the hypothesized [[Geyser (Mars)|Martian Geysers]]. The dark material at the end of the flows moves at between 0.1 and 1.4 m/day in late spring / summer on Mars.<ref name=Kereszturi2008>Kereszturi, A., et al. [http://www.lpi.usra.edu/meetings/lpsc2008/pdf/1555.pdf "Analysis of possible interfacial water driven seepages on Mars"], Lunar and Planetary Science Conference. Vol. 39. 2008.</ref> All current models for it favour liquid water as a cause. Either interfacial layers, or else layers of water created through the solid state greenhouse effect.}}

The process starts with the dark dune spots which form in early spring. Here are some examples in [[Richardson (Martian crater)|Richardson Crater]] in the Martian southern hemisphere- one of the places where the Flow Like Features (FLFs) have been observed.
The process starts with the dark dune spots which form in early spring. Here are some examples in [[Richardson (Martian crater)|Richardson Crater]] in the Martian southern hemisphere- one of the places where the Flow Like Features (FLFs) have been observed.


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For details see the Dark Dune Spots section of Nilton Renno's paper<ref name="MartínezRenno2013DarkDuneSpots"/> which also has images of the two types of feature as they progress through the season.
For details see the Dark Dune Spots section of Nilton Renno's paper<ref name="MartínezRenno2013DarkDuneSpots"/> which also has images of the two types of feature as they progress through the season.

==Earlier hypotheses==
==Earlier hypotheses==


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