Fluvial Channels On Titan
| dc.contributor.advisor | Brown, Robert H. | en_US |
| dc.contributor.author | Baugh, Nicole Faith | |
| dc.creator | Baugh, Nicole Faith | en_US |
| dc.date.accessioned | 2011-12-05T14:15:14Z | |
| dc.date.available | 2011-12-05T14:15:14Z | |
| dc.date.issued | 2008 | en_US |
| dc.identifier.uri | http://hdl.handle.net/10150/193368 | |
| dc.description.abstract | We present channel length and stream order for possible fluvial channels present in Cassini Synthetic Aperture Radar (SAR) data from Ta to T19. These features are present at most latitudes observed, with the bulk of the channels located in near-equatorial latitudes. Many of them are also organized into four branching channel networks, three of third order and one of fourth order, similar to river systems on Earth and Mars. These networks appear well integrated, with few streams that are not incorporated into the higher order branches. The median channel length for all channels on Titan is 29 km, with the longest channels all being incorporated into the channel networks. Estimates of channel width and depth of 1 km and 100m respectively result in a channel volume of 1012 m3 which, when extrapolated to the entire surface of Titan results in 1013 m3 of sediment. | |
| dc.language.iso | EN | en_US |
| dc.publisher | The University of Arizona. | en_US |
| dc.rights | Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. | en_US |
| dc.subject | Titan | en_US |
| dc.subject | Planetary Surfaces | en_US |
| dc.subject | Fluvial Erosion | en_US |
| dc.title | Fluvial Channels On Titan | en_US |
| dc.type | text | en_US |
| dc.type | Electronic Thesis | en_US |
| dc.contributor.chair | Brown, Robert H. | en_US |
| dc.identifier.oclc | 659749783 | en_US |
| thesis.degree.grantor | University of Arizona | en_US |
| thesis.degree.level | masters | en_US |
| dc.identifier.proquest | 2751 | en_US |
| thesis.degree.discipline | Planetary Sciences | en_US |
| thesis.degree.discipline | Graduate College | en_US |
| thesis.degree.name | MS | en_US |
| refterms.dateFOA | 2018-06-30T21:16:56Z | |
| html.description.abstract | We present channel length and stream order for possible fluvial channels present in Cassini Synthetic Aperture Radar (SAR) data from Ta to T19. These features are present at most latitudes observed, with the bulk of the channels located in near-equatorial latitudes. Many of them are also organized into four branching channel networks, three of third order and one of fourth order, similar to river systems on Earth and Mars. These networks appear well integrated, with few streams that are not incorporated into the higher order branches. The median channel length for all channels on Titan is 29 km, with the longest channels all being incorporated into the channel networks. Estimates of channel width and depth of 1 km and 100m respectively result in a channel volume of 1012 m3 which, when extrapolated to the entire surface of Titan results in 1013 m3 of sediment. |
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