Аннотация
Subsurface water processes are common for planetary bodies in the
solar system and are highly probable for exoplanets (planets outside
the solar system). For many solar system objects, the subsurface
water exists as ice. For Earth and Mars, subsurface saturated zones
have occurred throughout their planetary histories. Earth is mostly
clement with the recharge of most groundwater reservoirs from ample
precipitation during transient ice-and hot-house conditions, as recorded
through the geologic and fossilized records. On the other hand, Mars
is mostly in an ice-house stage, which is interrupted by endogenic-driven
activity. This activity catastrophically drives short-lived hydrological
cycling and associated climatic perturbations. Regional aquifers
in the Martian highlands that developed during past, more Earth-like
conditions delivered water to the northern plains. Water was also
cycled to the South Polar Region during changes in climate induced
by endogenic activity and/or by changes in Mars' orbital parameters.
Venus very likely had a warm hydrosphere for hundreds of millions
of years, before the development of its current extremely hot atmosphere
and surface. Subsequently, Venus lost its hydrosphere as solar luminosity
increased and a run-away moist greenhouse took effect. Subsurface
oceans of water or ammonia-water composition, induced by tidal forces
and radiogenic heating, probably occur on the larger sate lites Europa,
Ganymede, Callisto, Titan, and Triton. Tidal forces operating between
some of the small bodies of the outer solar system could also promote
the fusion of ice and the stability of inner liquid-water oceans.
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