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High resolution camera for mapping Titan Surface

Show simple item record Reinhardt, Bianca 2012-09-17T23:14:39Z 2012-09-17T23:14:39Z 2011-05
dc.identifier.citation NASA Undergraduate Student Research Program (USRP), Pasadena, California, May 2011 en_US
dc.identifier.clearanceno 11-4362
dc.description.abstract Titan, Saturn’s largest moon, has a dense atmosphere and is the only object besides Earth to have stable liquids at its surface. The Cassini/Huygens mission has revealed the extraordinary breadth of geological processes shaping its surface. Further study requires high resolution imaging of the surface, which is restrained by light absorption by methane and scattering from aerosols. The Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini spacecraft has demonstrated that Titan’s surface can be observed within several windows in the near infrared, allowing us to process several regions in order to create a geological map and to determine the morphology. Specular reflections monitored on the lakes of the North Pole show little scattering at 5 microns, which, combined with the present study of Titan’s northern pole area, refutes the paradigm that only radar can achieve high resolution mapping of the surface. The present data allowed us to monitor the evolution of lakes, to identify additional lakes at the Northern Pole, to examine Titan’s hypothesis of non-synchronous rotation and to analyze the albedo of the North Pole surface. Future missions to Titan could carry a camera with 5 micron detectors and a carbon fiber radiator for weight reduction. en_US
dc.description.sponsorship NASA/JPL en_US
dc.language.iso en_US en_US
dc.publisher Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2011. en_US
dc.subject Cassini en_US
dc.subject Titan en_US
dc.subject mapping en_US
dc.title High resolution camera for mapping Titan Surface en_US
dc.type Student Report en_US
dc.subject.NASATaxonomy Lunar and Planetary Science and Exploration en_US

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