Can Mars Seismic Events Be Successfully Modeled as Flow Induced Seismicity?
Session: InSight Seismology on Mars: Results From the First (Earth) Year of Data and Prospects for the Future [Poster]
Type: Poster
Date: 4/28/2020
Time: 08:00 AM
Room: Ballroom
Description:
The InSight mission, which landed on November 26, 2018, placed the first Very Broad Band Seismometer on the Martian surface. Several high signal to noise quakes with clear P and S arrivals and direction appear to originate in the general area of Cerberus Fossae, a young geologic area due east (~1500 km or ~30 degrees) of the InSight landing site at Elysium Planetia, characterized by fissures that cut the youngest lava flows on the surface of Mars.
A fraction of the seismic events are emergent, near monochromatic, last 10-15 minutes and so bear some resemblance to seismicity observed in volcanic regions on Earth.
The study aims to answer two questions: 1. Can some of the observed Martian seismicity be fluid-induced?; 2. If so, what is the physical parameter space that would permit it?
We explore the model space using the Markov Chain Monte Carlo (MCMC) approach, in which a source located at Cerberus Fossea is modeled by a buried channel through which fluid is transported [Julian, 1994]. Under certain conditions the channel walls begin to oscillate, and the oscillations are subsequently propagated through a numerical wave model to match the observations.
We find that it is possible to successfully model the main Martian seismic events (Amplitude, Frequency Content and coda) using a buried oscillating channel at Cerberus Fossae, and that the allowable physical parameter space is depth dependent and is limited to low-viscosity and high flow rate fluid. The model predicts a large magma flux (~103 m3/s) in general agreement of the inferred properties of Martian lava flows and some terrestrial volcanic regions, possibly pointing to an episodic rather than a continuous process.
Presenting Author: Sharon Kedar
Authors
Sharon Kedar sharon.kedar@jpl.nasa.gov Jet Propulsion Laboratory, Caltech, West Hills, California, United States Presenting Author
Corresponding Author
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Mark P Panning mark.p.panning@jpl.nasa.gov Jet Propulsion Laboratory, Caltech, Pasadena, California, United States |
Suzanne E Smrekar suzanne.e.smrekar@jpl.nasa.gov Jet Propulsion Laboratory, Caltech, Pasadena, California, United States |
Scott D King king07@vt.edu Virginia Tech, Blacksburg, Virginia, United States |
Matthew P Golombek matthew.p.golombek@jpl.nasa.gov Jet Propulsion Laboratory, Caltech, Pasadena, California, United States |
Michael Manga manga@seismo.berkeley.edu University of California, Berkeley, Berkeley, California, United States |
Bruce R Julian bruce.r.julian@gmail.com Durham University, Durham, , United Kingdom |
Brian R Shiro bshiro@usgs.gov U.S. Geological Survey, Hilo, Hawaii, United States |
Clément Perrin perrin@ipgp.fr Institut de Physique du Globe de Paris, Paris, , France |
Chloe Michaut chloe.michaut@ens-lyon.fr ENS de Lyon, Lyon, , France |
Philippe Lognonné lognonne@ipgp.fr Institut de Physique du Globe de Paris, Paris, , France |
William B Banerdt william.b.banerdt@jpl.nasa.gov Jet Propulsion Laboratory, Caltech, Pasadena, California, United States |
Can Mars Seismic Events Be Successfully Modeled as Flow Induced Seismicity?
Category
Insight Seismology on Mars: Results From the First (Earth) Year of Data and Prospects for the Future