Mathematics – Logic
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm...p21a11w&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #P21A-11 INVITED
Mathematics
Logic
5430 Interiors (8147), 6250 Moon (1221), 8434 Magma Migration, 8450 Planetary Volcanism (5480)
Scientific paper
The ability of a body of magma to ascend from the mantle of a planet depends on several factors: the density structure of the lithosphere; the density of the magma (which may change as it ascends if it contains exsolvable volatiles); the depth of origin of the magma; and the stress regime and rheology of the lithosphere (both of which will vary, with depth and over geologic time). We review these factors and discuss how the locations of density traps and rheological traps will have changed during lunar history. We then demonstrate that, early in lunar history, a diapiric magma body generated by magma segregation after pressure release melting in the head of a mantle plume may have reached a density trap at the base of the crust before reaching a rheological trap, whereas the reverse is almost certainly true later in lunar history. The order in which these events occur strongly influences the size of the magma body which can detach from the diapir and propagate into the crust. If the rheological trap is below, but sufficiently close to, the density trap, giant dikes can be created which penetrate the entire lithosphere. These are almost certainly the feeders required to explain the large volume mare lava flows and lava ponds, and are probably the intrusions inferred to be the cause of many linear rilles. If the rheological trap is too far below the density trap, the volumes of individual melt bodies able to reach the surface are less by several orders of magnitude, no matter how great the buoyancy of the magma. Indeed, over a wide range of conditions, increasing the buoyancy decreases the volume of magma delivered in each pulse.
Head James W.
Wilson Leslie
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