Discrete Element Simulations of Density-Driven Volcanic Deformation: Applications to Martian Caldera Complexes

Details Discrete Element Simulations of Density-Driven Volcanic Deformation: Applications to Martian Caldera Complexes Discrete Element Simulations of Density-Driven Volcanic Deformation: Applications to Martian Caldera Complexes

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.v23e2157z&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #V23E-2157

Physics

[5480] Planetary Sciences: Solid Surface Planets / Volcanism, [8148] Tectonophysics / Planetary Volcanism, [8450] Volcanology / Planetary Volcanism

Scientific paper

We have carried out 2-D numerical simulations using the discrete element method (DEM) to investigate density-driven deformation in Martian volcanic edifices. Our initial simulations demonstrated that gravitationally-driven settling of a dense, ductile cumulate body within a volcano causes enhanced lateral spreading of the edifice flanks, influencing the overall volcano morphology and generating pronounced summit subsidence. Here, we explore the effects of cumulate bodies and their geometries on the generation of summit calderas, to gain insight into the origin of Martian caldera complexes, in particular the Olympus Mons and Arsia Mons calderas. The Olympus Mons caldera, roughly 80 km in diameter, is composed of several small over-lapping craters with steep walls, thought to be produced by episodic collapse events of multiple shallow magma chambers. The Arsia Mons caldera spans ~130 km across and displays one prominent crater with gently sloping margins, possibly reflecting the collapse of a single magma chamber. Although the depth of the magma chamber is debated, its lateral width is thought to approximate the diameter of the caldera. Our models indicate that cumulate bodies located at shallow depths of <10 km below the edifice surface produce caldera complexes on the order of 80-100 km in width, with increasing cumulate widths producing widening calderas. Narrow cumulate bodies with densities near 4000 kg/m3 produce the deepest calderas (up to ~8 km deep). We conclude that the generation of large Arsia-type calderas may be adequately modeled by the presence of a wide cumulate body found at shallow depths beneath the summit. Although we do not model the multiple magma chamber systems thought to exist beneath the Olympus Mons summit, the closely spaced craters and the small size of the caldera relative to the size of the volcano (~13% of the edifice) suggests that the cumulate body would be narrow; our simulations of a single narrow cumulate body are capable of generating summit subsidence that is similar in dimension to the Olympus Mons caldera. Our findings suggest that cumulate spreading may play a primary role in the long-term development of caldera geometry, although the collapse of magma reservoirs (not modeled here) may cause important short-term changes in caldera structure.

Affiliated with

Also associated with

No associations

Rating

Discrete Element Simulations of Density-Driven Volcanic Deformation: Applications to Martian Caldera Complexes does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Discrete Element Simulations of Density-Driven Volcanic Deformation: Applications to Martian Caldera Complexes, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Discrete Element Simulations of Density-Driven Volcanic Deformation: Applications to Martian Caldera Complexes will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1776283