December 30, 2017

Drilling into Martian glacier – a simulation. Nature of the hydrogen bond

Filed under: Letters from Ionia — zankaon @ 1:36 pm

Several glaciers have been detected on the Martian surface. But they shouldn’t be there, since very low atmospheric pressure and vapor pressure. Hence the nature of the Martian rock ice must differ from earth ice. Surface appearance of the martian regolith and ice surface might be deceptively the same. How might one then distinguish the two?
One could perhaps land a lander within 150 miles of such glacier, and then use a jet powered drone to reach such glacier. One might further localize such glacier target by utilizing infrared camera of ~45 minute period of satellite to detect and follow a heated drone, and match it up with the infrared appearance of glacier; the latter having a different specific heat (and hence temperature) from surrounding regolith.

Once landed, one could drill into such martian rock ice, and compare it’s density to earth ice and rock. It should be greater than the former, and less than the latter.

Also one could use x-ray spectroscopy to detect a more rigid crystalline structure of such martian rock ice, as apposed to more amorphous earth ice. Such crystalline structure being more consistent with a shorter stronger hydrogen bond.

What basis might one have to explain such suposed unusual billion year old ice? That is, what is the nature of the hydrogen bonding for between water molecules of such martian glaciers?

Infrared absorption spectroscopy of such bond expected to be straight, shorten, not stretching, no librations, with negligible.vibration, even for higher catalytic martian temperature. Hence similar to covalent bonding? Might it even appear to have the strength and rigidity of hyrogen bonding in polymers, even though different connecting atoms?

water structure  M. Chaplin 

hydrogen bonding in water

water absorption spectrum


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