Temporal changes of mid-latitude surface regions on Titan
Abstract
The Cassini-Huygens instruments revealed that Titan, Saturn’s largest moon, has a complex, dynamic and Earth-like surface. Understanding the distribution and interplay of geologic processes on Titan is important for constraining models of its interior, surface-atmospheric interactions, and climate evolution. Data from the remote sensing instruments have shown the presence of diverse terrains, suggesting exogenic and endogenic processes. However, interpretations of surface features need a precise knowledge of the contribution by the dense intervening atmosphere, especially the troposphere. Cassini’s Visual and Infrared Mapping Spectrometer (VIMS) collects spectro-images within the so-called “methane windows” where the methane atmospheric absorption is weak, but non-negligible, permitting however a good perception of the surface. In order to make a good evaluation of the atmosphere and extract surface information we follow a method using a statistical tool and a Radiative transfer code with which we analyze regions of interest (i.e. regions of unknown origin), in order to monitor if their spectral behavior changes with time. These are cryovolcanic candidates and for comparison undifferentiated plains. We find that the cryovolcanic candidates Tui Regio and Sotra Patera change with time becoming darker and brighter respectively in terms of surface albedo while the plains do not present any significant change. The surface brightening of Sotra supports a possible cryovolcanic rather than an exogenic origin. The unchanged surface behavior of the plains supports a sedimentary origin rather than cryovolcanic. Such a variety of geologic processes and their relationship to the methane cycle make Titan particularly significant in Solar System studies.
- Publication:
-
AAS/Division for Planetary Sciences Meeting Abstracts #46
- Pub Date:
- November 2014
- Bibcode:
- 2014DPS....4621110S