Determining characteristic morphological wavelengths for Venus using
Baltis Vallis.
Abstract
One of Venus’ most enigmatic landforms is Baltis Vallis, the longest
observed channel on the surface (~7000 km long).
Topographic conformity analysis shows that Baltis Vallis was modified
over most of its observed wavelengths. Since the source location of
Baltis Vallis is not well constrained, we analyze in both flow
directions. For the commonly used northern source, topography across all
wavelengths appears to be created after Baltis Vallis. However, for the
southern source, topographic components with wavelengths longer than
~1900 km might have previously existed. Fourier analysis
reveals three characteristic wavelengths, ~110-235 km,
~640±25 km and ~3500±1200 km. The
shortest corresponds to deformation belts that cross Venus’ low plains,
while the medium currently lacks an explanation. The longest is
plausibly associated with the wavelength of dynamic uplift of the crust
by mantle plumes. Higher resolution observations provided by the VERITAS
mission can help resolve the source location of Baltis Vallis.