Curtain eruptions from Enceladus’ south-polar terrain

  title={Curtain eruptions from Enceladus’ south-polar terrain},
  author={Joseph Nicholas Spitale and Terry Anthony Hurford and Alyssa Rose Rhoden and Emily E. Berkson and Symeon S. Platts},
Observations of the south pole of the Saturnian moon Enceladus revealed large rifts in the south-polar terrain, informally called ‘tiger stripes’, named Alexandria, Baghdad, Cairo and Damascus Sulci. These fractures have been shown to be the sources of the observed jets of water vapour and icy particles and to exhibit higher temperatures than the surrounding terrain. Subsequent observations have focused on obtaining close-up imaging of this region to better characterize these emissions. Recent… 
Sustained eruptions on Enceladus explained by turbulent dissipation in tiger stripes
  • E. Kite, A. Rubin
  • Geology
    Proceedings of the National Academy of Sciences
  • 2016
A model of the tiger stripes as tidally flexed slots that puncture the ice shell can simultaneously explain the persistence of the eruptions through the tidal cycle, the phase lag, and the total power output, while suggesting that eruptions are maintained over geological timescales.
We apply histogram analysis, photogeological methods, and tidal stress modeling to Porco et al.'s survey of 101 Enceladus South Polar Basin geysers and their three-dimensional orientations to test if
Enceladus Plume Structure and Time Variability: Comparison of Cassini Observations
The authors' results confirm a mixture of both low and high Mach gas emission from Enceladus' surface tiger stripes, with gas accelerated as fast as Mach 10 before escaping the surface.
Enceladus Plume Structure and Time Variability: Comparison of Cassini Observations.
Abstract During three low-altitude (99, 66, 66 km) flybys through the Enceladus plume in 2010 and 2011, Cassini's ion neutral mass spectrometer (INMS) made its first high spatial resolution
Geodynamic modeling of the ice-ocean system on Enceladus
The Saturnian moon Enceladus is one of the most geologically active bodies in the solar system. Ridged terrains dominated by intense tectonism are observed on both hemispheres while plume jets
Modeling insights into the locations of density enhancements from the Enceladus water vapor jets
Monte Carlo modeling of the vapor erupting from Enceladus' south polar region is presented to demonstrate the influence of physical characteristics of the emitted vapor on the distribution of


Association of the jets of Enceladus with the warmest regions on its south-polar fractures
Cassini images taken from a variety of viewing directions are used to triangulate the source locations for the most prominent jets, and compare these with the infrared hotspot locations and the predictions from a recent model of tidally induced shear heating within the fractures.
We present the first comprehensive examination of the geysering, tidal stresses, and anomalous thermal emission across the south pole of Enceladus and discuss the implications for the moon's thermal
Cassini Observes the Active South Pole of Enceladus
The shape of Enceladus suggests a possible intense heating epoch in the past by capture into a 1:4 secondary spin/orbit resonance.
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.
Water vapour jets inside the plume of gas leaving Enceladus
Observations of an occultation of a star by the Enceladus plume on 24 October 2007 revealed four high-density gas jets superimposed on the background plume, which supports the hypothesis that the source of the plume is liquid water, with gas accelerated to supersonic velocity in nozzle-like channels.
High heat flow from Enceladus' south polar region measured using 10–600 cm−1 Cassini/CIRS data
[1] Analysis of 2008 Cassini Composite Infrared Spectrometer (CIRS) 10 to 600 cm−1 thermal emission spectra of Encleadus shows that for reasonable assumptions about the spatial distribution of the
Cartographic Mapping of the Icy Satellites Using ISS and VIMS Data
The sizes and shapes of six icy Saturnian satellites have been measured from Cassini Imaging Science Subsystem (ISS) data, employing limb coordinates and stereogram-metric control points. Mimas,
Enceladus' Water Vapor Plume
The Cassini spacecraft flew close to Saturn's small moon Enceladus three times in 2005 and observed stellar occultations on two flybys and confirmed the existence, composition, and regionally confined nature of a water vapor plume in the south polar region of Ence Gladus.
Cassini Imaging Science: Instrument Characteristics And Anticipated Scientific Investigations At Saturn
The Cassini Imaging Science Subsystem (ISS) is the highest-resolution two-dimensional imaging device on the Cassini Orbiter and has been designed for investigations of the bodies and phenomena found
Saturn from Cassini-Huygens
This book comprehensively reviews our current knowledge of Saturn featuring the latest results obtained by the Cassini-Huygens mission.