zankaon

June 29, 2012

Hematite, photosynthesis, silicates – connections? Martian rock ice? No sedimentary layers? olivine on Mars

Might hematite be the only marker of eroded ancient sedimentary seabed sites? Has billions of years of erosive wind action resulted in an unconformity? That is, might significant sedimentary layers not be found, nor present, anywhere on Mars, secondary to erosive wind effect over billions of  years? Thus the prediction of no hematite at deeper bored levels. Might Gale crater be a counter example to such lack of sedimentary layer scenario, or contrarily, an aeolian effect?

Could one integrate an area for abundance of hematite, and thus oxygen content? Thus inferring the amount of oxygenation for given seas’ volume, or just per hematite distribution? The latter would supposedly denote only areas, within geographical seas, for photosynthesis, since no significant aeolian re-distribution of hematite. Then would this set limits on amount of photosynthesis that occurred? Also would any oxygenation of martian atmosphere be very limited, in light of very slow oxygenation of our atmosphere?

Would widespread prevalence of unweatherized olivine on Mars, without secondary mineralization, be consistent with most of surface water disappearing very early; hence likewise for surface life? Thus a constrain on life’s duration on Mars; a fast start and finish?

Or might a thick atmosphere (protection from UV radiation), and intermittent dew and/or frost be sufficient for origin of life on a dryer surface? Would the latter dryer surface be consistent with importance of stability in the preservation of any newly formed molecular combinations, in a transient aqueous environment?

Also Tharsis plateau volcanic complex is of a shield volcanic nature, and not explosive. Hence consistent with no viscous silicates (silicon oxides), and hence consistent with no significant past oxygenated atmospheric weathering effect for Mars.

For any so-called martian rock ice to form sub-surface, still a significant vapor pressure and thus significant atmosphere (1/10 bar?) must have been present.

Perhaps micro frozen ‘fossils’ might be found in such rock ice. Not multi-cellular, since not enough time for multi-cellularity to evolve. For example, Animalia and metazoa evolved much later on earth. One could drill into sub-surface smooth (not a glass from amorphous rapid cooling?) martian rock ice, and compare amperage etc. to a similar fine bore drilling for earth ice; the difference being proportional to density. Also infrared spectroscopy for such probe? Thus might such martian rock ice formation be considered as a gradual ongoing solid physical phase change?

Would a gradual increase in hydrogen bond strength for between water molecules then account for lack of sublimation of such ice, both sub-surface and on the surface, in part at mid latitude, and also at North Pole especially? That is, why is there snow at all at North Pole, especially in summer? ~6 millibars should result in sublimation of snow at the pole. Would the retention of such not so thick snow be consistent with increased (covalent ?) strenght of hydrogen bond for between water molecules, not only sub-surface, but also for surface water ice/snow, any where on Mars? Might one utilize orbital infrared spectroscopy of residual polar cap snow, to look for such increased hydrogen bond strength for between water molecules?

So billion year old effect of increasing bond strength and stiffness (i.e. bending, stretching) for hydrogen bond (i.e. for between water molecules) – giving almost covalent bond strength? There is wide variation in hydrogen bond strength.

Infrared spectroscopy measures vibration modes of water, and all modes of vibration are infrared active. Then compare such infrared signature of bond strength to earth ice. Also such martian rock ice would look like rock, and seem hard like rock, but much lighter; consistent with lower density than rock. Also a different melting temperature from earth ice, and becomes mottled from exposure to ultraviolet light. Likewise for any Martian meteorites on earth ; so slicing, and looking for any pitting after uv exposure, with comparative controls, would seem to confirm it’s origin. TMM

olivine on Mars

Martian sub-surface ice, mid latitude

Infrared_spectroscopy

Hydrogen_bond

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