Simulations of Seismic Wave Propagation on Mars

Bozdağ, Ebru; Ruan, Youyi; Metthez, Nathan; Khan, Amir; Leng, Kuangdai; van Driel, Martin; Wieczorek, Mark; Rivoldini, Attilio; Larmat, Carène S.; Giardini, Domenico; Tromp, Jeroen; Lognonné, Philippe; Banerdt, Bruce W.

doi:10.1007/s11214-017-0350-z

Simulations of Seismic Wave Propagation on Mars

Journal Article · Thu Mar 23 00:00:00 EDT 2017 · Space Science Reviews

DOI:https://doi.org/10.1007/s11214-017-0350-z· OSTI ID:1369205

Bozdağ, Ebru ^[1]; Ruan, Youyi ^[2]; Metthez, Nathan ^[3]; Khan, Amir ^[3]; Leng, Kuangdai ^[4]; van Driel, Martin ^[3]; Wieczorek, Mark ^[5]; Rivoldini, Attilio ^[6]; Larmat, Carène S. ^[7]; Giardini, Domenico ^[3]; Tromp, Jeroen ^[2]; Lognonné, Philippe ^[8]; Banerdt, Bruce W. ^[9]

Univ. of Nice Sophia Antipolis, Nice (France). CNRS-OCA-IRD-Geoazur
Princeton Univ., NJ (United States)
Federal Inst. of Technology (ETH), Zurich (Switzerland)
Univ. of Oxford (United Kingdom)
Univ. of Cote d'Azur, Nice (France). Lab. Lagrange. CNRS. Observatory of Cote d'Azur
Royal Observatory of Belgium, Brussels (Belgium)
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Paris Diderot Univ. (France). Inst. of Physics of the Globe of Paris-Sorbonne Paris City
California Inst. of Technology (CalTech), Pasadena, CA (United States). Jet Propulsion Lab.

In this paper, we present global and regional synthetic seismograms computed for 1D and 3D Mars models based on the spectral-element method. For global simulations, we implemented a radially-symmetric Mars model with a 110 km thick crust. For this 1D model, we successfully benchmarked the 3D seismic wave propagation solver SPECFEM3D_GLOBE against the 2D axisymmetric wave propagation solver AxiSEM at periods down to 10 s. We also present higher-resolution body-wave simulations with AxiSEM down to 1 s in a model with a more complex 1D crust, revealing wave propagation effects that would have been difficult to interpret based on ray theory. For 3D global simulations based on SPECFEM3D_GLOBE, we superimposed 3D crustal thickness variations capturing the distinct crustal dichotomy between Mars’ northern and southern hemispheres, as well as topography, ellipticity, gravity, and rotation. The global simulations clearly indicate that the 3D crust speeds up body waves compared to the reference 1D model, whereas it significantly changes surface waveforms and their dispersive character depending on its thickness. We also perform regional simulations with the solver SES3D based on 3D crustal models derived from surface composition, thereby addressing the effects of various distinct crustal features down to 2 s. The regional simulations confirm the strong effects of crustal variations on waveforms. Finally, we conclude that the numerical tools are ready for examining more scenarios, including various other seismic models and sources.

View Accepted Manuscript (DOE)

Research Organization:: Los Alamos National Lab. (LANL), Los Alamos, NM (United States)

Sponsoring Organization:: USDOE; Swiss National Science Foundation (Switzerland)

Contributing Organization:: Princeton Univ., NJ (United States); Univ. of Oxford (United Kingdom); Univ. of Cote d'Azur, Nice (France); Royal Observatory of Belgium, Brussels (Belgium); Paris Diderot Univ. (France); California Inst. of Technology (CalTech), Pasadena, CA (United States)

Grant/Contract Number:: AC52-06NA25396

OSTI ID:: 1369205

Report Number(s):: LA-UR--17-22631

Journal Information:: Space Science Reviews, Journal Name: Space Science Reviews Journal Issue: 1-4 Vol. 211; ISSN 0038-6308

Publisher:: SpringerCopyright Statement

Country of Publication:: United States

Language:: English

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58 GEOSCIENCES
Mars
Planetary Sciences
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normal modes
numerical methods
seismic
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Simulations of Seismic Wave Propagation on Mars

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