The Origin And Nature Of Martian Valley Networks

Details The Origin And Nature Of Martian Valley Networks The Origin And Nature Of Martian Valley Networks

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf.1377c&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.1377

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Scientific paper

Valley networks are often cited as the best evidence that liquid water was stable on the surface of Mars early in its history [1]. However, geologic evidence is beginning to emerge indicating that the period of time valley networks were forming was actually short-lived and restricted primarily to the end of the Noachian/beginning of the Hesperian [2]. Other geologic features, such as modified impact craters, outflow channels, fluidized eject craters, putative evidence for ancient shorelines, and even volcanoes offer some evidence as to the ancient climatic conditions that may have existed on early Mars. These features suggest that the conditions were similar to the conditions that probably existed on the Earth when life was forming on our own planet. Valley networks are an important clue to the timing and intensity of fluvial processes that occurred on ancient Mars, but they must be placed into context with other features.

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