The Polarization of Ambient Noise on Mars

Stutzmann, É.; Schimmel, Martin; Lognonné, Philippe; Horleston, Anna; Ceylan, Savas; Driel, Martin van; Stähler, Simon C.; Banerdt, B.; Calvet, Marie; Charalambous, Constantinos; Clinton, John; Drilleau, M.; Fayon, Lucile; Garcia, Raphaël; Giardini, Domenico; Hurst, K.; Jacob, A. W. B.; Kawamura, Taïchi; Kenda, B.; Margerin, Ludovic; Murdoch, Naomi; Panning, M. P.; Pike, Tom; Scholz, J. R.; Spiga, Aymeric

doi:10.1029/2020je006545

Cited by 36 publications

(52 citation statements)

References 71 publications

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“…Conversely, bumps 2–6 are systematically attenuated in the 30% and 3% data sets. These data sets consist mostly of seismic recordings during the local evening hours (Figure ) which is when there are less wind and less air pressure perturbations (e.g., Lognonne et al., 2020; Stutzmann et al., 2021). Bumps 2 to 6 correspond to resonances that are related to different lander modes which are mostly excited by turbulent winds above a threshold speed of about 3 m/s (Dahmen et al., 2021).…”

Section: Determination Of P‐wave Reflection Response At Seismentioning

confidence: 99%

“…SEIS has been deployed on the ground of the Homestead hollow, 1.81 m south of the closest lander foot (Stutzmann et al., 2021). Homestead hollow is a degraded impact crater of about 27 m diameter in Elysium Planitia with a smooth sandy, granule‐ and pebble‐rich surface with few rocks (Golombek et al., 2020).…”

Section: Introductionmentioning

confidence: 99%

“…In spite of these harsh conditions, 174 mostly small marsquakes (Giardini et al., 2020) have been identified until 30 September 2019 thanks to the sensitivity of SEIS and its careful deployment on the Martian surface. Nevertheless, due to the unfavorable deployment conditions different aseismic signals are being recorded together with events of the seismic origin (Ceylan et al., 2021; Lognonne et al., 2020; Scholz et al., 2020; Stutzmann et al., 2021). That is, the seismic recordings contain a wealth of features caused by operational activities at the lander, noise induced by the lander due to atmospheric perturbations as laminar and turbulent winds, and artifacts caused by the response of the instruments to the variability of the severe climatic factors as pressure and temperature.…”

Section: Introductionmentioning

confidence: 99%

“…So far, no unambiguous surface waves have been detected in the SEIS data (Clinton et al., 2020; Giardini et al., 2020; Stutzmann et al., 2021). The very shallow structure down to 20 m depth at the InSight landing site has been probed using the travel time of multiple hammer strokes of the HP 3 (Heat Flow and Physical Properties Package) instrument and compliance observations (Kenda et al., 2020; Lognonne et al., 2020).…”

Section: Introductionmentioning

confidence: 99%

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Seismic Noise Autocorrelations on Mars

Schimmel¹,

Stutzmann

Lognonné

et al. 2021

Earth and Space Science

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Mars is the first extraterrestrial planet with seismometers (Seismic Experiment for Interior Structure, SEIS) deployed directly on its surface in the framework of the Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission. The lack of strong Marsquakes, however, strengthens the need of seismic noise studies to additionally constrain the Martian structure. Seismic noise autocorrelations of single‐station recordings permit the determination of the zero‐offset reflection response underneath SEIS. We present a new autocorrelation study which employs state‐of‐the‐art approaches to determine a robust reflection response by avoiding bias from aseismic signals which are recorded together with seismic waves due to unfavorable deployment and environmental conditions. Data selection and segmentation is performed in a data‐adaptive manner which takes the data root‐mean‐square amplitude variability into account. We further use the amplitude‐unbiased phase cross‐correlation and work in the 1.2–8.9 Hz frequency band. The main target are crustal scale reflections, their robustness and convergence. The strongest signal appears at 10.6 s, and, if interpreted as a P‐wave reflection, would correspond to a discontinuity at about 21 km depth. This signal is a likely candidate for a reflection from the base of the Martian crust due to its strength, polarity, and stability. Additionally we identify, among the stable signals, a signal at about 6.15 s that can be interpreted as the P‐wave reflection from the mid‐crust at about 9.5 km depth.

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Section: Determination Of P‐wave Reflection Response At Seismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Seismic Noise Autocorrelations on Mars

Schimmel¹,

Stutzmann

Lognonné

et al. 2021

Earth and Space Science

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“…The azimuth with respect to North in the N, E of the horizontal components of the elliptical polarized motion is the linear component will be   N . All components for Z downward are the opposite for N z and Z.Data Availability StatementData corresponding to this article are inStutzmann et al (2020). Seis raw data are in "InSight Mars SEIS Data Service together with IPGP, JPL, CNES, ETHZ, ICL, MPS, ISAE-Supaero, LPG, MFSC" (2019) with doi:https://doi.org/10.18715/SEIS.INSIGHT.XB_2016.STUTZMANN ET AL.…”

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confidence: 99%

The Polarization of Ambient Noise on Mars 

Stutzmann¹,

Schimmel²,

Lognonné³

et al. 2021

Preprint

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Seismic noise recorded at the surface of Mars has been monitored since February 2019, using the InSight seismometers.This noise can reach -200 dB and is 500 times lower than on Earth at night and it increases of 30 dB during the day. We analyze its polarization as a function of time and frequency in the band 0.03-1Hz. We use the degree of polarization&#160; to extract signals with stable polarization independent of their amplitude and type of polarization. We detect polarized signals at all frequencies and all times. Glitches correspond to linear polarized signals which are more abundant during the night. For signals with elliptical polarization, the ellipse is in the horizontal plane below 0.3 Hz (LF). Above 0.3 Hz (HF) and except in the evening, the ellipse is in the vertical plane and the major axis is tilted. While polarization azimuths are different in the two frequency bands, they both vary as a function of local hour and season.&#160; They are also correlated with wind direction, particularly during the daytime.We investigate possible aseismic and seismic origins of the polarized signals. Lander or tether noise can be discarded. Pressure fluctuations transported by wind may explain part of the HF polarization but not the tilt of the ellipse. This tilt can be obtained if the source is an acoustic emission coming from high altitude at critical angle. Finally, in the evening when the wind is low, the polarized signals may correspond to the seismic wavefield of the Mars background noise.

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The marsquake catalogue from InSight, sols 0–1011

Ceylan

Clinton

Giardini

et al. 2022

Preprint

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The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission began collecting high quality seismic data on Mars in February 2019. This manuscript documents the seismicity observed by SEIS, InSight's seismometer, from this time until the end of March 2020. Within the InSight project, the Marsquake Service (MQS) is responsible for prompt review of all seismic data collected by InSight, detection of events that are likely to be of seismic origin, and curation and release of seismic catalogues. In the first year of data collection, MQS have identified 465 seismic events that we interpret to be from regional and teleseismic marsquakes. Seismic events are grouped into 2 different event families: the low frequency family is dominated by energy at long period below 1 s, and the high frequency family primarily include energy at and above 2.4 Hz. Event magnitudes, from Mars-specific scales, range from 1.3 to 3.7. A third class of events with very short duration but high frequency bursts have been observed 712 times. These are likely associated with a local source driven by thermal stresses. This paper describes the data collected so far in the mission and the procedures under which MQS operates; summarises the content of the current MQS seismic catalogue; and presents the key features of the events we have observed so far, using the largest events as examples.

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The Polarization of Ambient Noise on Mars

Cited by 36 publications

References 71 publications

Seismic Noise Autocorrelations on Mars

Seismic Noise Autocorrelations on Mars

The Polarization of Ambient Noise on Mars

The marsquake catalogue from InSight, sols 0–1011

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The Polarization of Ambient Noise on Mars

Cited by 36 publications

References 71 publications

Seismic Noise Autocorrelations on Mars

Seismic Noise Autocorrelations on Mars

The Polarization of Ambient Noise on Mars&#160;

The marsquake catalogue from InSight, sols 0–1011

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The Polarization of Ambient Noise on Mars