MODELLING OF VOLCANIC ERUPTIONS ON TITAN

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Publiée : Jan 1, 2010
DOI : https://doi.org/10.12681/bgsg.11679
A. Solomonidou
A.D. Fortes
K. Kyriakopoulos
Résumé

Observations by the Visual Infrared Spectrometer instrument (VIMS) aboard the Cassini mission have
indicated the possible presence of CO2 ice on the surface on Titan, in areas which exhibit high
reflectance in specific spectral windows (McCord et al., 2008). Two of the bright spots of significance
are located within the Xanadu region – Tui Regio (located at 20°S, 130°W) and Hotei Regio (located
at 26°S, 78°W), and there is a further spot situated in proximity to Omacatl Macula (Hayne et al.,
2008). Explosive volcanic eruptions of a cryomagma containing H2O and CO2 are modelled for
several potential scenarios regarding entrained CO2 clathrates. The model yielded a range of values
corresponding to the fragmentation pressure in the lava conduit, the velocity of the exploding
cryomagma, the height of the associated lava fountain and the potential distance covered by ejecta.
The results show that a single vent source does not possess the force required to cover an area
resembling Hotei Regio or Tui Regio. Therefore, we consider alternative origins: the area may have
been resurfaced by small CO2 grains resulting from multiple explosive eruptions emanating from a
zone of weakness (Hayne et al., 2008); the characteristics of the area are consequential of an eruption
of cryomagma with CO2 and NH3 components (McCord et al., 2008); or finally, long term seasonal
winds transferred small CO2 grains and distributed them within the limits of Tui Regio area.

Article Details
  • Rubrique
  • Petrology and Mineralogy
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