Surface albedo changes with time on Titan’s possible
cryovolcanic sites: Cassini/VIMS processing and
geophysical implications
Rodriguez, S.
Stephan, K.
Bampasidis, G.
Moussas, X.
Jaumann, R.
Sotin, C.
Kyriakopoulos, K.
Coustenis, A.
Sohl, F.
Wagner, F. W.
Lopes, R.M.C.
Hirtzig, M.
Brown, R. H.
Drossart, P.
Le Mouélic, S.
Hussmann, H.
Solomonidou, A.
Bratsolis, E.
Seymour, K. St.
We present a study on Titan’s possibly cryovolcanic and varying regions as suggested from previous studies [e.g. 1;2;7]. These regions, which are potentially subject to change over time in brightness and are located close to the equator, are Tui Regio, Hotei Regio, and Sotra Patera. We apply two methods on Cassini/VIMS data in order to retrieve their surface properties and monitor any temporal variations. First, we apply a statistical method, the Principal Component Analysis (PCA) [3;4] where we manage to isolate regions of distinct and diverse chemical composition called ‘Region of interest – RoI’. Then, we focus on retrieving the spectral differences (with respect to the Huygens landing site albedo) among the RoIs by applying a radiative transfer code (RT) [5;3]. Hence, we are able to view the dynamical range and evaluate the differences in surface albedo within the RoIs of the three regions. In addition, using this double procedure, we study the temporal surface variations of the three regions witnessing albedo changes with time for Tui Regio from 2005-2009 (darkening) and Sotra Patera from 2005-2006 (brightening) at all wavelengths [3]. The surface albedo variations and the presence of volcanic-like features within the regions in addition to a recent study [6] that calculates Titan's tidal response are significant indications for the connection of the interior with the cryovolcanic candidate features with implications for the satellite’s astrobiological potential.
