Mathematics – Logic
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusm.p33a..07c&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #P33A-07
Mathematics
Logic
3619 Magma Genesis And Partial Melting (1037), 5430 Interiors (8147), 5460 Physical Properties Of Materials, 6280 Saturnian Satellites, 8429 Lava Rheology And Morphology
Scientific paper
We discuss tidal dissipation in molten basaltic magma and the results from model application to Io and Enceladus. Magma is a non-newtonian liquid with a complex rheology dependent on interactions between different phases: liquid, crystals and bubbles, resulting in a slurry with each component responding differently to temperature and stress. This study is based on results obtained for terrestrial basalts. For example, the evolution of crystal content as a function of temperature has been described for basalts [e.g., 1]. The behavior of cyclically stressed basalt has been observed in laboratory for frequencies corresponding to seismic waves between 1 and 200 sec. [e.g., 2-5]. While this frequency range is outside the range of dynamical frequencies considered in planetary sciences, these results show variations of the response as a function of the wavelength of the structure involved in the response. From the trend observed at low frequencies we extrapolate these data to tidal frequencies encountered at Io and Enceladus. We apply this result to a silicate magma chamber deep in Enceladus's core. Such a magma body has been proposed by Matson et al. [6, 7] as a heat source for keeping Enceladus warm over geological time and ultimately powering the observed volcanism [8]. We also apply the model to the 'magma sea' at Loki Patera [9] the source of 10-20% of Io's heat flow. In both cases we evaluate how much tidal dissipation can be produced. Our objectives are to chart the development and long-term evolution of magma chambers on bodies heavily influenced by tidal dissipation. From consideration of the relevant processes taking place over appropriate timescales, results show that self- regulation mechanisms are in place, such that crystal content and heat production remain in equilibrium over geological time. Our preliminary results support long-term preservation of a magma chamber in Enceladus' core. Coupled thermal-orbital modeling also indicates consistency between this model and Enceladus' present dynamical state. The conditions for tidal dissipation to explain thermal observations at Loki Patera are a function of the volume of material involved in the process. In this framework it can be possible to infer constraints on the volume, i.e., depth of this magma sea. This work was carried out at the Jet Propulsion Laboratory-California Institute of Technology, under contract to NASA. References: [1] McBirney and Murase (1984) Ann. Rev. Earth Planet Sci., 12, 337-357. [2] Bagdassarov N. S. and D. B. Dingwell (1993) JGR, 98, 6477-6487. [3] Bagdassarov et al. (1994) PEPI, 83, 83-99. [4] Webb S. (1997) Rev. Geoph., 35, 191-218. [5] James M.R. et al. (2004) JVGR, 132, 99-113. [6] Matson et al. (2005) AGU Fall meeting, #P32-A05. [7] Matson D. L. et al. (2006) LPS, 37, 2219. [8] Spencer et al., 2006, LPS, 37, 2252. [9] Matson et al. (2006) JGR, submitted.
Castillo Julie C.
Davies Andrew G.
Johnson Torrence V.
Matson Dennis L.
Veeder Glenn J. Jr.
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