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A combined spectrophotometric and morphometric study of the lunar mare dome fields near Cauchy, Arago, Hortensius, and Milichius |
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| Authors: | Christian Wöhler Raffaello Lena Jim Phillips Zac Pujic Geologic Lunar Research Group |
| Institution: | a DaimlerChrysler Research and Technology, Machine Perception, P.O. Box 2360, 89013 Ulm, Germany b Via Cartesio 144, sc. D, 00137 Rome, Italy c Via Pernice 71, 54100 Massa (MS), Italy d 101 Bull Street, Charleston, SC 29401, USA e RR#3 Perth, Ontario, K7H 3C5, Canada f Queensland Brain Institute, The University of Queensland, Queensland 4072, Australia |
| Abstract: | In this study we examine the spectral and morphometric properties of the four important lunar mare dome fields near Cauchy, Arago, Hortensius, and Milichius. We utilize Clementine UV-vis multispectral data to examine the soil composition of the mare domes while employing telescopic CCD imagery to compute digital elevation maps in order to determine their morphometric properties, especially flank slope, height, and edifice volume. After reviewing previous attempts to determine topographic data for lunar domes, we propose an image-based 3D reconstruction approach which is based on a combination of photoclinometry and shape from shading. Accordingly, we devise a classification scheme for lunar mare domes which is based on a principal component analysis of the determined spectral and morphometric features. For the effusive mare domes of the examined fields we establish four classes, two of which are further divided into two subclasses, respectively, where each class represents distinct combinations of spectral and morphometric dome properties. As a general trend, shallow and steep domes formed out of low-TiO2 basalts are observed in the Hortensius and Milichius dome fields, while the domes near Cauchy and Arago that consist of high-TiO2 basalts are all very shallow. The intrusive domes of our data set cover a wide continuous range of spectral and morphometric quantities, generally characterized by larger diameters and shallower flank slopes than effusive domes. A comparison to effusive and intrusive mare domes in other lunar regions, highland domes, and lunar cones has shown that the examined four mare dome fields display such a richness in spectral properties and 3D dome shape that the established representation remains valid in a more global context. Furthermore, we estimate the physical parameters of dome formation for the examined domes based on a rheologic model. Each class of effusive domes defined in terms of spectral and morphometric properties is characterized by its specific range of values for lava viscosity, effusion rate, and duration of the effusion process. For our data set we report lava viscosities between about 102 and  , effusion rates between 25 and  , and durations of the effusion process between three weeks and 18 years. Lava viscosity decreases with increasing R415/R750 spectral ratio and thus TiO2 content; however, the correlation is not strong, implying an important influence of further parameters like effusion temperature on lava viscosity. |
| Keywords: | Moon Volcanism Image processing Spectrophotometry Geological processes |
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