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Cassini Encounters Enceladus: Background and the Discovery of a South Polar Hot Spot
Cassini's Composite Infrared Spectrometer (CIRS) detected 3 to 7 gigawatts of thermal emission from the south polar troughs at temperatures up to 145 kelvin or higher, making Enceladus only the third known solid planetary body—after Earth and Io—that is sufficiently geologically active for its internal heat to be detected by remote sensing. Expand
Hydrocarbon lakes on Titan: Distribution and interaction with a porous regolith
from <10 to more than 100,000 km 2 . The size and location of lakes provide constraints on parameters associated with subsurface transport. Using porous media properties inferred from Huygens probeExpand
Correlations between Cassini VIMS spectra and RADAR SAR images: Implications for Titan's surface composition and the character of the Huygens Probe Landing Site
Titan's vast equatorial fields of RADAR-dark longitudinal dunes seen in Cassini RADAR synthetic aperture images correlate with one of two dark surface units discriminated as “brown” and “blue” inExpand
Titan's inventory of organic surface materials
[1] Cassini RADAR observations now permit an initial assessment of the inventory of two classes, presumed to be organic, of Titan surface materials: polar lake liquids and equatorial dune sands.Expand
Modeling volcanic processes : the physics and mathematics of volcanism
List of contributors 1. Introduction Sarah Fagents, Tracy Gregg and Rosaly Lopes 2. Magma chamber dynamics and thermodynamics Josef Dufek, Chris Huber and Leif Karlstrom 3. The dynamics of dikeExpand
Dunes on Titan observed by Cassini Radar
Thousands of longitudinal dunes have recently been discovered by the Titan Radar Mapper on the surface of Titan. These are found mainly within ±30° of the equator in optically-, near-infrared-, andExpand
Rapid and Extensive Surface Changes Near Titan’s Equator: Evidence of April Showers
The detection by Cassini's Imaging Science Subsystem of a large low-latitude cloud system early in Titan’s northern spring and extensive surface changes in the wake of this storm are reported, which suggests that the dry channels observed at Titan's low latitudes are carved by seasonal precipitation. Expand
General patterns of flow field growth: Aa and blocky lavas
Lava flow fields consist of one or more flows. Four ideal emplacement regimes are recognized: (a) that for single flows and (b) that for flow fields dominated by (1) widening, (2) thickening, or (3)Expand
Io Volcanism Seen by New Horizons: A Major Eruption of the Tvashtar Volcano
The Tvashtar volcanic plume's morphology and dynamics support nonballistic models of large Io plumes and also suggest that most visible plume particles condensed within the plume rather than being ejected from the source. Expand
Fluvial channels on Titan: Initial Cassini RADAR observations
Abstract Cassini radar images show a variety of fluvial channels on Titan's surface, often several hundreds of kilometers in length. Some (predominantly at low- and mid-latitude) are radar-bright andExpand