Measuring Fundamental and Higher Mode Surface Wave Dispersion on Mars From Seismic Waveforms

Autor: Mélanie Drilleau, B. Kenda, Naomi Murdoch, M. van Driel, Fabian Euchner, Maren Böse, P. H. Lognonné, Nienke Brinkman, Caroline Beghein, Domenico Giardini, John Clinton, Haotian Xu, Taichi Kawamura, Mark P. Panning, Savas Ceylan, Simon Stähler, Anna Horleston
Přispěvatelé: Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
Jazyk: angličtina
Rok vydání: 2021
Předmět:
Zdroj: Earth and Space Science
Earth and Space Science, 2021, 8 (2), pp.0. ⟨10.1029/2020EA001263⟩
Earth and Space Science, 8 (2)
Earth and Space Science, Vol 8, Iss 2, Pp n/a-n/a (2021)
Xu, H, Beghein, C, Panning, M, Drilleau, M, Lognonné, P, van Driel, M, Ceylan, S, Böse, M, Brinkman, N, Clinton, J, Euchner, F, Giardini, D, Horleston, A C, Kawamura, T, Kenda, B, Murdoch, N & Stähler, S C 2021, ' Measuring fundamental and higher mode surface wave dispersion on Mars from seismic waveforms ', Earth and Space Science, vol. 8, no. 2, e2020EA001263 . https://doi.org/10.1029/2020EA001263
ISSN: 2333-5084
Popis: International audience; One of the goals of the Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission is to constrain the interior structure of Mars. We present a hierarchical transdimensional Bayesian approach to extract phase velocity dispersion and interior shear‐wave velocity (VS) models from a single seismogram. This method was adapted to Mars from a technique recently developed for Earth (Xu & Beghein, 2019, https://doi.org/10.1093/gji/ggz133). Monte Carlo Markov Chains seek an ensemble of one dimensional (1‐D) VS models between a source and a receiver that can explain the observed waveform. The models obtained are used to calculate the phase velocities of fundamental and higher modes at selected periods, and a subsequent analysis is performed to assess which modes were reliably measured. An advantage of our approach is that it can also fit unknown data noise, which reduces the risk of overfitting the data. In addition, uncertainties in the source parameters can be propagated, yielding more accurate model parameter uncertainties. In this study, we first present our technique and discuss the challenges stemming from using a single station to characterize both structure and the source and from the absence of a Mars reference model. We then demonstrate the method feasibility using the Mars Structure Service blind test data and our own synthetic data, which included realistic noise levels based on the noise recorded by InSight.
Databáze: OpenAIRE
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