The Biggest Eruption Ever Witnessed: The Effusion Profile Of The Pillan (Io) 1997 Eruption, And The Implications For Massive Basaltic Flow Emplacement On Earth And Mars.

Details The Biggest Eruption Ever Witnessed: The Effusion Profile Of The Pillan (Io) 1997 Eruption, And The Implications For Massive Basaltic Flow Emplacement On Earth And Mars. The Biggest Eruption Ever Witnessed: The Effusion Profile Of The Pillan (Io) 1997 Eruption, And The Implications For Massive Basaltic Flow Emplacement On Earth And Mars.

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.3003d&link_type=abstract

American Astronomical Society, DPS meeting #38, #30.03; Bulletin of the American Astronomical Society, Vol. 38, p.538

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The 1997 eruption of Pillan Patera, on Io, was the largest effusive eruption ever witnessed. At least 31 km3 of lava were erupted in 100 days, with an additional 25 km3 erupted shortly thereafter, yielding a total of 56 km3 [1]. This eruption is important as it sheds light on the emplacement of very large, voluminous flows that were emplaced millions of years ago on Earth and Mars. Temporal and areal constraints allow application of models of varying effusion rate [2] to determine peak effusion rate and also the varying rate of surface coverage. From this information, thermal emission profiles have been constructed that show that the thermal emission measured by Galileo [e.g., 3] can be produced by insulated flows, implying that turbulent flow emplacement may not have been the dominant emplacement regime. Peak effusion rates at Pillan exceeded 104 m3 s-1. NIMS thermal emission measurements can be modelled with a basaltic magma composition. The resulting insulating crust, with a small crack fraction, appears to be similar to that on terrestrial flood basalts that formed inflated pahoehoe sheet flows with a 'rubbly' surface [4]. Our new results from Pillan lend additional quantitative support to the idea that terrestrial rubbly pahoehoe flows and Martian "platy-ridged" flows are diagnostic of similar high eruption rates [4]. Further modelling requires consideration of flow advance rate, which is yet to be adequately constrained for Pillan. This work was carried out at the Jet Propulsion Laboratory-California Institute of Technology, under contract to NASA. AGD is supported by a grant from the NASA PG&G Program. References: [1] Davies, A. G. et al. (2006) LPSC 37, abstract 1155. [2] Wadge, G. (1981) J. Volc. Geotherm. Res., 11, 139-168. [3] Davies, A. G. et al., (2001) JGR, 106, E12, 33079-33104. [4] Keszthelyi, L. et al. (2004) G3, 5, 2004GC000758.

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