Autocorrelation of the Ground Vibrations Recorded by the SEIS‐InSight Seismometer on Mars

Compaire, Nicolas; Margerin, Ludovic; Garcia, Raphaël; Pinot, Baptiste; Calvet, Marie; Orhand-Mainsant, G.; Kim, Doyeon; Lekić, V.; Tauzin, Benoît; Schimmel, Martin; Stutzmann, E.; Knapmeyer‐Endrun, Brigitte; Lognonné, Philippe; Pike, W. T.; Schmerr, Nicholas; Gizon, Laurent; Banerdt, W. B.

doi:10.1029/2020je006498

Cited by 40 publications

(48 citation statements)

References 47 publications

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“…Indeed, the 10.6 s signal is a likely candidate for a reflection from the base of the crust owing to its two-way travel time, negative polarity, strengths and robustness. En--19-manuscript submitted to ESS ergy at similar lag time has also been reported by Deng and Levander (2020) and Compaire et al (2021) and interpreted as P-wave Moho reflection. The 10.6 s signal seems to be consistent with models obtained for receiver functions from marsquake data (Lognonne et al, 2020;Knapmeyer-Endrun et al, 2021) This is based on the assumption that the crust-mantle boundary is stronger than a midcrust discontinuity.…”

Section: Discussionsupporting

confidence: 70%

“…All in all, they use data recorded during the evening hours for which autocorrelations have the highest signalto-noise ratio (SNR) and find a signal at 10.6 s and at 21 s which they interpret as reflections from crustal layers. They also show that glitches can not interfere with these reflections as they are separated by more than 30 s. The repeat time of donks, however, can be much smaller with maximum at about 10 s around 17-18 h LMST (Compaire et al, 2021). The authors argue that the observed stability of the 10.6 s signal with time -20-manuscript submitted to ESS is not correlated with the overall distribution of donks which finally makes a donk origin of these reflections unlikely.…”

Section: Discussionmentioning

confidence: 95%

“…The tick noise is caused by electro-magnetic coupling during the SEIS temperature acquisition at 1 sps with a recorded waveform which does not resemble an impulsive sig--12-manuscript submitted to ESS nal (Compaire et al, 2021). On vertical components and within the here considered frequency band, most of its energy is at 4, 7, and 2 Hz (Fig.…”

Section: Attenuation Of Tick Noise Lander and Shallow Structure Resonancesmentioning

confidence: 93%

“…Deng and Levander (2020) High-frequency autocorrelations (5-7 Hz) have been presented by Suemoto et al (2020) who showed robust signals which indicate the presence of two shallow reflectors in the first hundreds of meters. Noise and Marsquake autocorrelations have been also presented by Compaire et al (2021), who find stable autocorrelations with signals related to crustal structure only during low-noise periods around 2.4 Hz In this study we use the VBB SEIS data to further analyze noise autocorrelations through independent approaches. Special care is given to avoid imprints of aseismic signals and artifacts on the autocorrelation results.…”

Section: Introductionmentioning

confidence: 91%

“…Indeed, the 10.6 s signal is quite robust and a likely candidate for a P-wave reflection from the crust-mantle boundary. Note thatCompaire et al (2021) also report a signal at 10.6 s using a different approach. The 10.6 s signal is discernible in linear and tf-PWSs of the three data sets as shown in Fig.…”

mentioning

confidence: 99%

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Seismic Noise Autocorrelations on Mars

Schimmel¹,

Stutzmann

Lognonné

et al. 2021

Preprint

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Section: Discussionsupporting

confidence: 70%

Section: Discussionmentioning

confidence: 95%

Section: Attenuation Of Tick Noise Lander and Shallow Structure Resonancesmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 91%

mentioning

confidence: 99%

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Seismic Noise Autocorrelations on Mars

Schimmel¹,

Stutzmann

Lognonné

et al. 2021

Preprint

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Joint Inversion of receiver functions and apparent incidence angles to determine the crustal structure of Mars

Joshi

Knapmeyer‐Endrun²,

Mosegaard

et al. 2022

Preprint

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Recent estimates of the crustal thickness of Mars show a bimodal result of either 20 km or 40 km beneath the InSight lander.We propose an approach based on random matrix theory applied to receiver functions to further constrain the subsurface structure. Assuming a spiked covariance model for our data, we first use the phase transition properties of the singular value spectrum of random matrices to detect coherent arrivals in the waveforms. Examples from terrestrial data show how the method works in different scenarios. We identify three new converted arrivals in the InSight data, including the second multiply reflected phase from a deeper third interface. We then use this information to jointly invert receiver functions with the absolute S-wave velocity information in the polarization of body waves. Results show a crustal thickness of 43±5 km beneath the lander with two mid-crustal interfaces at depths of 8.5±1.5 km and 22±3 km.

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Crustal Structure Constraints from the Detection of the SsPp Phase on Mars

Beghein

Davis

et al. 2022

Preprint

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The shallowest intracrustal layer (extending to 8 ± 2 km depth) beneath the Mars InSight Lander site exhibits low seismic wave velocity, which are likely related to a combination of high porosity and other lithological factors. The SsPp phase, an SV-to P-wave reflection on the receiver side, is naturally suited for constraining the seismic structure of this top crustal layer since its prominent signal makes it observable with a single station without the need for stacking. We have analyzed eight broadband and low-frequency seismic events recorded on Mars and made the first coherent detection of the SsPp phase on the red planet. The timing and amplitude of SsPp confirm the existence of the ~8 km interface in the crust and the large wave speed (or impedance) contrast across it. With our new constraints from the SsPp phase, we determined that the P-wave speed in the top crustal layer is between 2.5 km/s and 3.3 km/s, which is a more precise and robust estimate than the previous range of 2.0-3.5 km/s obtained by receiver function analysis. The porosity in Layer 1 is estimated to be as much as 21-31% (assuming an aspect ratio of 0.1 for the pore space), but could be lower if some pores are filled by low-density cements or other secondary 1 mineral phases. These porosities and P-wave speeds are compatible with our current understanding of the upper crustal stratigraphy beneath the InSight Lander site.

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Autocorrelation of the Ground Vibrations Recorded by the SEIS‐InSight Seismometer on Mars

Cited by 40 publications

References 47 publications

Seismic Noise Autocorrelations on Mars

Seismic Noise Autocorrelations on Mars

Joint Inversion of receiver functions and apparent incidence angles to determine the crustal structure of Mars

Crustal Structure Constraints from the Detection of the SsPp Phase on Mars

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