Joint Inversion of High-Frequency Receiver Functions and Surface-Wave Dispersion: Case Study in the Parnaíba Basin of Northeast Brazil

Victor, T. S. D. C.; Julià, Jordi; White, Nicholas J.; Rodríguez‐Tribaldos, Verónica

doi:10.1785/0120190203

Cited by 5 publications

(3 citation statements)

References 42 publications

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“…We conduct P‐wave RF analysis of this event because the RF method is very sensitive to velocity discontinuities. On Earth, RFs have been routinely applied to study structures from near‐surface sedimentary layering (e.g., Cunningham & Lekic, 2020; Licciardi & Agostinetti, 2014; Victor et al., 2020) to the structure of the mantle transition zone (e.g., Xu et al., 2018). On Mars and the Moon, RFs mostly focus on the crustal scale so far (Durán et al., 2022; Knapmeyer‐Endrun et al., 2021; Vinnik et al., 2001).…”

Section: Introductionmentioning

confidence: 99%

High‐Frequency Receiver Functions With Event S1222a Reveal a Discontinuity in the Martian Shallow Crust

Shi

Plasman

Knapmeyer‐Endrun

et al. 2023

Geophysical Research Letters

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The Interior Exploration using Seismic Investigations, Geodesy, and Heat Transport (InSight) mission of NASA successfully landed on the western Elysium Planitia of Mars on 26 November 2018 (Banerdt et al., 2020), and a few weeks later, deployed the SEIS seismometer for continuous seismic monitoring of Mars (Lognonné et al., 2019). One of InSight's main tasks is to investigate the Martian crust to shed light on the evolution of terrestrial planets (Lognonné et al., 2019;Smrekar et al., 2019) because the crust of Mars has preserved not only the products of early mantle differentiation and magmatism but also information about the sedimentary history and meteorite impacts.To carry out this task, different approaches have been employed. The seismic studies have revealed that the uppermost 100-200 m beneath the landing site are composed of two low-velocity zones (∼0-20 m and ∼30-80 m) and two high-velocity zones (∼20-30 m, and ∼80-200 m) (Carrasco et al., 2022;Hobiger et al., 2021;Kenda et al., 2020). The low-velocity zones are interpreted as brecciated regolith and sediments, while the high-velocity zones represent basaltic layer based on in situ geological investigations (Warner et al., 2022). For structures of the deeper crust, the P-wave receiver functions (RFs) computed from several marsquakes indicate three crus-

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Section: Introductionmentioning

confidence: 99%

High‐Frequency Receiver Functions With Event S1222a Reveal a Discontinuity in the Martian Shallow Crust

Shi

Plasman

Knapmeyer‐Endrun

et al. 2023

Geophysical Research Letters

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“…Consequently, the Moho‐multiples are often not used in the joint inversion with RF waveforms (e.g., Shen & Ritzwoller, 2016; Shen, Ritzwoller, & Schulte‐Pelkum, 2013), leaving crustal Vp/Vs poorly constrained. Thus, crustal Vp/Vs can only be presumed during the inversion (e.g., Victor et al., 2020; Yang et al., 2020; Zhang & Yao, 2017) except for a few regional studies (e.g., Berg et al., 2021). Additionally, making inaccurate assumptions in crustal Vp/Vs while it trades off with other parameters results in insufficient constraints on all parameters of interest in the continent‐scale studies (Shen & Ritzwoller, 2016).…”

Section: Introductionmentioning

confidence: 99%

Incorporating H‐κ Stacking With Monte Carlo Joint Inversion of Multiple Seismic Observables: A Case Study for the Northwestern US

Wu,

Sui,

Shen

2024

JGR Solid Earth

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Accurately determining the seismic structure of the continental deep crust is crucial for understanding its geological evolution and continental dynamics in general. However, traditional tools such as surface waves often face challenges in solving the trade‐offs between elastic parameters and discontinuities. In this work, we present a new approach that combines two established inversion techniques, receiver function H‐κ stacking and joint inversion of surface wave dispersion and receiver function waveforms, within a Bayesian Monte Carlo (MC) framework to address these challenges. Demonstrated by synthetic tests, the new method greatly reduces trade‐offs between critical parameters, such as the deep crustal Vs, Moho depth, and crustal Vp/Vs ratio. This eliminates the need for assumptions regarding crustal Vp/Vs ratios in joint inversion, leading to a more accurate outcome. Furthermore, it improves the precision of the upper mantle velocity structure by reducing its trade‐off with Moho depth. Additional notes on the sources of bias in the results are also included. Application of the new approach to USArray stations in the Northwestern US reveals consistency with previous studies and identifies new features. Notably, we find elevated Vp/Vs ratios in the crystalline crust of regions such as coastal Oregon, suggesting potential mafic composition or fluid presence. Shallower Moho depth in the Basin and Range indicates reduced crustal support to the elevation. The uppermost mantle Vs, averaging 5 km below Moho, aligns well with the Pn‐derived Moho temperature variations, offering the potential of using Vs as an additional constraint to Moho temperature and crustal thermal properties.

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“…(b) The scattered waves in the scattering medium vary in different time windows, but it is unclear whether the PRFs are stable when calculated using different time windows. (c) The PRF method is widely used to study seismic structures of various scales on Earth (e.g., Victor et al, 2020;Xu et al, 2018;Zhu & Kanamori, 2000) and has also been successfully applied to Mars (Durán et al, 2022;Knapmeyer-Endrun et al, 2021;Lognonné et al, 2020;Shi et al, 2023a). However, for the Moon, only S-wave receiver functions beneath Apollo 12 (Lognonné et al, 2003;Vinnik et al, 2001) and no other RFs have been retrieved.…”

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confidence: 99%

Differences in Scattering Properties of the Shallow Crusts of Earth, Mars, and the Moon Revealed by P‐Wave Receiver Functions

et al. 2023

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The scattering properties of terrestrial planetary bodies can provide valuable insights into their shallow seismic structure, meteoritic impact history, and geological activity. Scattering properties of the shallow crusts of Earth, Mars, and the Moon are investigated by constructing P‐wave receiver functions (PRFs) from teleseismic waveforms with high signal‐to‐noise ratios. The authors’ analysis reveals that strong coda waves lead to significant variations in the PRF waveforms calculated using different time windows, and the stability of the PRF is primarily influenced by the fractional velocity fluctuation. Synthetic PRFs for various scattering media confirm these observations. Comparing the observed and synthetic PRFs, it is found that the fractional velocity fluctuation in the shallow crust is greater than ∼0.2 for the Moon but less than ∼0.2 for Earth and Mars. The authors further discuss possible mechanisms that could have affected the fractional velocity fluctuation and suggest that the distinct fractional velocity fluctuation between the Moon and Earth/Mars is mainly due to differences in the water content of the crustal rocks of the three planetary bodies.

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Joint Inversion of High-Frequency Receiver Functions and Surface-Wave Dispersion: Case Study in the Parnaíba Basin of Northeast Brazil

Cited by 5 publications

References 42 publications

High‐Frequency Receiver Functions With Event S1222a Reveal a Discontinuity in the Martian Shallow Crust

High‐Frequency Receiver Functions With Event S1222a Reveal a Discontinuity in the Martian Shallow Crust

Incorporating H‐κ Stacking With Monte Carlo Joint Inversion of Multiple Seismic Observables: A Case Study for the Northwestern US

Differences in Scattering Properties of the Shallow Crusts of Earth, Mars, and the Moon Revealed by P‐Wave Receiver Functions

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