By National Research Council Staff
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Extra resources for A Scientific Rationale for Mobility in Planetary Environments (Compass Series)
Because Europa has no appreciable atmosphere, any liquid at the free surface would immediately freeze by evaporative self-cooling and by thermal radiation. If liquid water is present in the near subsurface, there are substantial ramifications for Europa, as both the ice tectonics and the interior heating change dramatically. Dissipation of tidal energy increases in the presence of a liquid water ocean because the surface ice shell experiences greater deformation. Movement of the ice at the surface and resurfacing of the planet, either by liquid or ice emplacement, are more efficient in the presence of liquid.
All rights reserved. 1). 25 m2 solar cell array. Navigation was controlled from Earth, but the rover was capable of avoiding obstacles by using laser sensors and a simple avoidance protocol included in its on-board processor (Intel 80C85). Navigation was accomplished with two forward-looking monochromatic cameras that provided a stereoscopic view of the terrain. Sojourner’s maximum speed was 1 cm/s for a total possible range of about 60 m/day, assuming continuous driving and no obstacles; actual speeds and distance traveled were much less.
These vary greatly Copyright © National Academy of Sciences. All rights reserved. html THE ROLE OF MOBILITY IN SOLAR SYSTEM EXPLORATION 23 from place to place on Jupiter but tend to be strong (~50 to 100 m/s). At these speeds, a lifetime of less than a week is probably sufficient to traverse a hot spot. Considerably longer lifetimes would, however, be required to sample a sizable portion of the planet. Knowledge of the locations of the balloons with respect to gross atmospheric features will be required.
A Scientific Rationale for Mobility in Planetary Environments (Compass Series) by National Research Council Staff