Computer Science
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..10e..12d&link_type=abstract
Progress in Planetary Exploration Missions, 26th meeting of the IAU, Joint Discussion 10, 21-22 August 2006, Prague, Czech Repub
Computer Science
Scientific paper
Three years after the end of the Galileo mission, analyses of the data obtained have led to a deeper understanding of volcanism on Io. A re-appraisal of previous analyses of imaging data shows that the presence of high-temperature ultramafic magmas is no longer needed to explain observations, although the presence of these exotic magmas are not ruled out [1]. Lower magma temperatures (reduced from >1800 K to ~1400-1500 K) removes the need for a global `mushy' magma ocean (required to produce the high degree of mantle melting needed to yield ultramafic magma). Study of time-series data coupled with process modelling of effusive and explosive activity at individual locations has allowed mechanisms of eruption and resurfacing to be constrained and quantified. Loki Patera, Io's most powerful volcano, is revealed as a magma sea, which for many years was periodically resurfaced [2, 3]. Prometheus undergoes episodic activity in a manner similar to that seen at Kilauea, on Earth [4]. At Pillan where over 55 km^3 of lava was erupted in ~100 days in 1997, new estimates of peak effusion rates are up to 4 x 10^4 m^3 s^-1, possibly the largest outpouring of lava ever witnessed [5] with implications for the emplacement of large, voluminous lava flows on Earth and Mars. Although Io's volcanoes are the main mechanism of removing heat from Io's interior to the surface (heat transport by conduction is suppressed by the rate at which Io is being resurfaced), the main mechanism of resurfacing during the Galileo epoch is by deposition from volcanic plumes [6]. After Galileo, many questions remain, and new ones are raised regarding the relationship between hot spots, paterae, and mountains; paterae formation; magma composition; and the relationship between observed heat flow and tidal heating. Acknowledgements: This work was carried out at the Jet Propulsion Laboratory-California Institute of Technology, under contract to NASA. References: [1] Keszthelyi et al., 2006, LPSC37 abstract 2216. [2] Rathbun et al., 2002, GRL, 29, 84 1-4. [3] Matson et al., 2006, JGR, in press. [4] Davies et al., 2006, Icarus, in press. [5] Davies et al., LPSC 37 abstract 1155. [6] Geissler et al., 2004, Icarus, 169, 29-64.
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