Applications to Lunar Remote Sensing - 3D Computer Vision: Efficient Methods and Applications - page 328

Fig. 8.16 ( a ) Pixel-synchronous pair of images of the central part of Rupes Cauchy, acquired at
local sunrise ( top ) and at local sunset ( bottom ). Image credit: P. Lazzarotti. ( b ) Perspective view
of the DEM obtained based on combined shadow and shading analysis according to Sect. 5.2 .The
vertical axis is 10 times exaggerated. The curvature of the lunar surface has been subtracted

(cf. Fig. 8.15 b) provides the required shadow information. The height of the re-
constructed part of Rupes Recta ranges from 200 m to about 400 m, which is well
consistent with the shadow length in Fig. 8.15 b. The albedo map ρ uv shows bright
spots in the lower part and especially in the upper right part of the image. The linear
structures in the albedo map along Rupes Recta are artefacts; presumably, ρ uv is not
very accurate at places where the surface strongly bends and the residual intensity
error e i according to ( 3.50 ) is comparably large due to the regularisation constraints.

A three-dimensional reconstruction of the central part of the lunar tectonic fault
Rupes Cauchy obtained by Wöhler et al. ( 2006a ) based on a combined shadow and
shading analysis according to Sect. 5.2 isshowninFig. 8.16 . The upper image in
Fig. 8.16 a acquired at local sunrise was used for extracting shadow information.
The resulting DEM reveals that the elevation of the fault is not constant, obtaining
values of more than 350 m in its highest parts. In the southern part of the DEM small
structures appear on the slope of the fault, reaching a height of about 100 m relative
to the surface level to the west.

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8.4 Three-Dimensional Reconstruction of Lunar Domes

8.4.1 General Overview of Lunar Domes

This section provides a short description of the characteristics of lunar volcanic
domes. According to Head and Gifford ( 1980 ), lunar mare domes are low elevations
of mostly circular shape located in the mare plains. They have smooth surfaces and
low flank slopes of typically less than a few degrees. Presumably, most of them were
formed by the effusion of basaltic lava (Wilhelms, 1987 ). The highest frequencies of
lunar domes are observed in several parts of Oceanus Procellarum, especially in the
Marius region and between the craters Hortensius, Milichius, and Tobias Mayer, and
in Mare Tranquillitatis. Other mare regions on the lunar nearside display individual
domes (Head and Gifford, 1980 ).