Impact‐induced hydrothermal activity on early Mars

@article{Abramov2005ImpactinducedHA,
  title={Impact‐induced hydrothermal activity on early Mars},
  author={Oleg Abramov and David A. Kring},
  journal={Journal of Geophysical Research},
  year={2005},
  volume={110}
}
[1] We report on numerical modeling results of postimpact cooling of craters with diameters of 30, 100, and 180 km in an early Martian environment, with and without the presence of water. The effects of several variables, such as ground permeability and the presence of a crater lake, were tested. Host rock permeability is the main factor affecting fluid circulation and lifetimes of hydrothermal systems, and several permeability cases were examined for each crater. The absence of a crater lake… 

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References

SHOWING 1-10 OF 102 REFERENCES

Numerical modeling of an impact‐induced hydrothermal system at the Sudbury crater

[1] Large impact events, like the one that formed the Sudbury crater in Ontario, Canada, at 1.85 Ga, significantly increase the temperature of target rocks. The heat sources generated by such an

Starting Conditions for Hydrothermal Systems Underneath Martian Craters: Hydrocode Modeling

Mars is the most Earth-like of the Solar System s planets, and the first place to look for any sign of present or past extraterrestrial life. Its surface shows many features indicative of the

Multiphase groundwater flow near cooling plutons

We investigate groundwater flow near cooling plutons with a computer program that can model multiphase flow, temperatures up to 1200°C, thermal pressurization, and temperature-dependent rock

On the thermal history, thermal state, and related tectonism of a moon of fission origin

The thermal history of an initially totally molten moon of fission origin properly accounts for (1) the mare basalt epoch, in terms of its duration, the depth of the source region, and degrees of

The case for rainfall on a warm, wet early Mars

[1] Valley networks provide compelling evidence that past geologic processes on Mars were different than those seen today. The generally accepted paradigm is that these features formed from

Location and sampling of aqueous and hydrothermal deposits in martian impact craters.

TLDR
Large craters may represent giant Petri dishes for culturing preexisting life on Mars and promoting biogeochemical processes, and landing sites must be identified in craters where access to the buried lacustrine sediments and impact melt deposits is provided by processes such as erosion from outflow channels, faulting, aeolian erosion, or excavation by later superimposed cratering events.

Hydrothermal hydration of Martian crust: illustration via geochemical model calculations.

TLDR
The alteration of Shergotty shows the greatest potential for storing water as hydrous minerals, and the alteration of Icelandic rhyolite has the lowest potential, in accord with studies of low-grade alteration of terrestrial rocks.

Hydrothermal systems associated with martian impact craters

Abstract With widespread evidence of both heat sources and water (either liquid or solid), hydrothermal systems are likely to have existed on Mars. We model hydrothermal systems in two sizes of fresh

A model for the hydrologic and climatic behavior of water on Mars

Past studies of the climatic behavior of water on Mars have universally assumed that the atmosphere is the sole pathway available for volatile exchange between the planet's crustal and polar

Environmental Effects of Large Impacts on Mars

TLDR
The martian valley networks formed near the end of the period of heavy bombardment of the inner solar system, about 3.5 billion years ago, and warmed the surface, keeping it above the freezing point of water for periods ranging from decades to millennia, depending on impactor size.
...