Abstract
We measure the wavelength of aeolian bedforms on the surface of martian volcanoes, spanning a 23km range in elevation, or nearly an order of magnitude in atmospheric pressure and density. We find that the bedform wavelength (∼1–5m) varies as the reciprocal of density. The observed wavelengths and wavelength dependence are compared with three recent models of bedform spacing. The results are consistent with the expected increase in threshold friction speed and saturation drag length with elevation. The observations lend support to the expectation that such bedforms on Venus or Titan are too small to be observed in present data.
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