Debris flows or lava flows on Mars? Shapes of terrestrial counterparts may help identify flows imaged in upcoming mission

Details Debris flows or lava flows on Mars? Shapes of terrestrial counterparts may help identify flows imaged in upcoming mission Debris flows or lava flows on Mars? Shapes of terrestrial counterparts may help identify flows imaged in upcoming mission

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28..949m&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 949.

Statistics

Methodology

Debris, Lava, Mars Surface, Satellite Imagery, Morphology, Methodology

Scientific paper

If Martian flows are similar to terrestrial flows they may have been undetected in Viking Orbiter images, but may be detected in upcoming missions. We are developing an understanding of morphological characteristics of terrestrial debris flows from air photos of the lahars of Mount St. Helens, Washington; Mount Augustine, Alaska; and Klyuchevskii, Kamchatka, and the debris flows in Owens Valley, California, as well as from descriptive accounts of these and other debris flow deposits. Our research focuses on a quantitative analysis of the margins of terrestrial flow deposits, including rhyodacite, andesite and basalt lavas, debris flows, pyroclastic flows and debris avalanches. To analyze these flows, we use an algorithm to generate curvature spectra, a measure of the abundance of all orders of radius of curvature within a margin. The results are somewhat analogous to Fourier spectra but can be adapted to highly irregular, digitate margins. The spectra are then examined for consistent differences between different types of flows, and variations within one type. Variation is expected among debris flows due to differences in grain size and the size distribution of debris, bulk sediment, clay and water concentration, and underlying topography.

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