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2. Surface waves and crustal structure on Mars

Author

Kim, D, Banerdt, WB, Ceylan, S, Giardini, D, Lekić, V, Lognonné, P, Beghein, C, Beucler, É, Carrasco, S, Charalambous, C, Clinton, J, Drilleau, M, Durán, C, Golombek, M, Joshi, R, Khan, A, Knapmeyer-Endrun, B, Li, J, Maguire, R, Pike, WT, Samuel, H, Schimmel, M, Schmerr, NC, Stähler, SC, Stutzmann, E, Wieczorek, M, Xu, Z, Batov, A, Bozdag, E, Dahmen, N, Davis, P, Gudkova, T, Horleston, A, Huang, Q, Kawamura, T, King, SD, McLennan, SM, Nimmo, F, Plasman, M, Plesa, AC, Stepanova, IE, Weidner, E, Zenhäusern, G, Daubar, IJ, Fernando, B, Garcia, RF, Posiolova, LV, and Panning, MP

Subjects
General Science & Technology
Abstract

We detected surface waves from two meteorite impacts on Mars. By measuring group velocity dispersion along the impact-lander path, we obtained a direct constraint on crustal structure away from the InSight lander. The crust north of the equatorial dichotomy had a shear wave velocity of approximately 3.2 kilometers per second in the 5- to 30-kilometer depth range, with little depth variation. This implies a higher crustal density than inferred beneath the lander, suggesting either compositional differences or reduced porosity in the volcanic areas traversed by the surface waves. The lower velocities and the crustal layering observed beneath the landing site down to a 10-kilometer depth are not a global feature. Structural variations revealed by surface waves hold implications for models of the formation and thickness of the martian crust.

Published
2022

4. SEIS: Insight’s Seismic Experiment for Internal Structure of Mars

Author

Lognonné, P, Banerdt, WB, Giardini, D, Pike, WT, Christensen, U, Laudet, P, de Raucourt, S, Zweifel, P, Calcutt, S, Bierwirth, M, Hurst, KJ, Ijpelaan, F, Umland, JW, Llorca-Cejudo, R, Larson, SA, Garcia, RF, Kedar, S, Knapmeyer-Endrun, B, Mimoun, D, Mocquet, A, Panning, MP, Weber, RC, Sylvestre-Baron, A, Pont, G, Verdier, N, Kerjean, L, Facto, LJ, Gharakanian, V, Feldman, JE, Hoffman, TL, Klein, DB, Klein, K, Onufer, NP, Paredes-Garcia, J, Petkov, MP, Willis, JR, Smrekar, SE, Drilleau, M, Gabsi, T, Nebut, T, Robert, O, Tillier, S, Moreau, C, Parise, M, Aveni, G, Ben Charef, S, Bennour, Y, Camus, T, Dandonneau, PA, Desfoux, C, Lecomte, B, Pot, O, Revuz, P, Mance, D, tenPierick, J, Bowles, NE, Charalambous, C, Delahunty, AK, Hurley, J, Irshad, R, Liu, Huafeng, Mukherjee, AG, Standley, IM, Stott, AE, Temple, J, Warren, T, Eberhardt, M, Kramer, A, Kühne, W, Miettinen, E-P, Monecke, M, Aicardi, C, André, M, Baroukh, J, Borrien, A, Bouisset, A, Boutte, P, Brethomé, K, Brysbaert, C, Carlier, T, Deleuze, M, Desmarres, JM, Dilhan, D, Doucet, C, Faye, D, Faye-Refalo, N, Gonzalez, R, Imbert, C, Larigauderie, C, Locatelli, E, Luno, L, Meyer, J-R, Mialhe, F, Mouret, JM, Nonon, M, Pahn, Y, Paillet, A, Pasquier, P, Perez, G, and Perez, R

Subjects
Behavioral and Social Science, Basic Behavioral and Social Science, Mars seismology, InSight, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

By the end of 2018, 42 years after the landing of the two Viking seismometers on Mars, InSight will deploy onto Mars' surface the SEIS (Seismic Experiment for Internal Structure) instrument; a six-axes seismometer equipped with both a long-period three-axes Very Broad Band (VBB) instrument and a three-axes short-period (SP) instrument. These six sensors will cover a broad range of the seismic bandwidth, from 0.01 Hz to 50 Hz, with possible extension to longer periods. Data will be transmitted in the form of three continuous VBB components at 2 sample per second (sps), an estimation of the short period energy content from the SP at 1 sps and a continuous compound VBB/SP vertical axis at 10 sps. The continuous streams will be augmented by requested event data with sample rates from 20 to 100 sps. SEIS will improve upon the existing resolution of Viking's Mars seismic monitoring by a factor of ∼2500 at 1 Hz and ∼200000 at 0.1 Hz. An additional major improvement is that, contrary to Viking, the seismometers will be deployed via a robotic arm directly onto Mars' surface and will be protected against temperature and wind by highly efficient thermal and wind shielding. Based on existing knowledge of Mars, it is reasonable to infer a moment magnitude detection threshold of Mw∼3 at 40∘ epicentral distance and a potential to detect several tens of quakes and about five impacts per year. In this paper, we first describe the science goals of the experiment and the rationale used to define its requirements. We then provide a detailed description of the hardware, from the sensors to the deployment system and associated performance, including transfer functions of the seismic sensors and temperature sensors. We conclude by describing the experiment ground segment, including data processing services, outreach and education networks and provide a description of the format to be used for future data distribution.Electronic supplementary materialThe online version of this article (10.1007/s11214-018-0574-6) contains supplementary material, which is available to authorized users.

Published
2019

6. Constraints on the shallow elastic and anelastic structure of Mars from InSight seismic data

Author

Lognonné, P., Banerdt, W. B., Pike, W. T., Giardini, D., Christensen, U., Garcia, R. F., Kawamura, T., Kedar, S., Knapmeyer-Endrun, B., Margerin, L., Nimmo, F., Panning, M., Tauzin, B., Scholz, J.-R., Antonangeli, D., Barkaoui, S., Beucler, E., Bissig, F., Brinkman, N., Calvet, M., Ceylan, S., Charalambous, C., Davis, P., van Driel, M., Drilleau, M., Fayon, L., Joshi, R., Kenda, B., Khan, A., Knapmeyer, M., Lekic, V., McClean, J., Mimoun, D., Murdoch, N., Pan, L., Perrin, C., Pinot, B., Pou, L., Menina, S., Rodriguez, S., Schmelzbach, C., Schmerr, N., Sollberger, D., Spiga, A., Stähler, S., Stott, A., Stutzmann, E., Tharimena, S., Widmer-Schnidrig, R., Andersson, F., Ansan, V., Beghein, C., Böse, M., Bozdag, E., Clinton, J., Daubar, I., Delage, P., Fuji, N., Golombek, M., Grott, M., Horleston, A., Hurst, K., Irving, J., Jacob, A., Knollenberg, J., Krasner, S., Krause, C., Lorenz, R., Michaut, C., Myhill, R., Nissen-Meyer, T., ten Pierick, J., Plesa, A.-C., Quantin-Nataf, C., Robertsson, J., Rochas, L., Schimmel, M., Smrekar, S., Spohn, T., Teanby, N., Tromp, J., Vallade, J., Verdier, N., Vrettos, C., Weber, R., Banfield, D., Barrett, E., Bierwirth, M., Calcutt, S., Compaire, N., Johnson, C.L., Mance, D., Euchner, F., Kerjean, L., Mainsant, G., Mocquet, A., Rodriguez Manfredi, J. A, Pont, G., Laudet, P., Nebut, T., de Raucourt, S., Robert, O., Russell, C. T., Sylvestre-Baron, A., Tillier, S., Warren, T., Wieczorek, M., Yana, C., and Zweifel, P.

Published
2020
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7. The seismicity of Mars

Author

Giardini, D., Lognonné, P., Banerdt, W. B., Pike, W. T., Christensen, U., Ceylan, S., Clinton, J. F., van Driel, M., Stähler, S. C., Böse, M., Garcia, R. F., Khan, A., Panning, M., Perrin, C., Banfield, D., Beucler, E., Charalambous, C., Euchner, F., Horleston, A., Jacob, A., Kawamura, T., Kedar, S., Mainsant, G., Scholz, J.-R., Smrekar, S. E., Spiga, A., Agard, C., Antonangeli, D., Barkaoui, S., Barrett, E., Combes, P., Conejero, V., Daubar, I., Drilleau, M., Ferrier, C., Gabsi, T., Gudkova, T., Hurst, K., Karakostas, F., King, S., Knapmeyer, M., Knapmeyer-Endrun, B., Llorca-Cejudo, R., Lucas, A., Luno, L., Margerin, L., McClean, J. B., Mimoun, D., Murdoch, N., Nimmo, F., Nonon, M., Pardo, C., Rivoldini, A., Manfredi, J. A. Rodriguez, Samuel, H., Schimmel, M., Stott, A. E., Stutzmann, E., Teanby, N., Warren, T., Weber, R. C., Wieczorek, M., and Yana, C.

Published
2020
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8. Planetary Seismology: Nearly 3 years on Mars, and a return to the Moon

Author

Yana, Charles, Weber, Renee, Walsh, William, Standley, Ian, de Raucourt, Sebastien, Pont, Gabriel, Pike, W. Tom, Nunn, Ceri, Lognonné, Philippe, Kawamura, Taichi, Garcia, Raphael, Elliott, John, Cutler, James, Calcutt, Simon, Bugby, David, Bowles, Neil, Kedar, Sharon, Tharimena, S, Tauzin, B, Stutzmann, E, Schimmel, M, Schmelzbach, C, Nunn, C, Murdoch, N, Lekic, V, Brinkman, N, Kenda, B, Fayon, L, Spiga, A, Stott, A. E, Stähler, S, Orhand-Mainsant, G, Knapmeyer, M, Khan, A, Horleston, A, van Driel, M, Charalambous, C, Ceylan, S, Böse, M, Drilleau, M, Hurst, K, Weber, R, Teanby, N, Schmerr, N, Mimoun, D, Margerin, L, Knapmeyer-Endrun, B, Kedar, S, Kawamura, T, Irving, J, Garcia, R, Clinton, J, Bozdag, E, Lorenz, R, Giardini, D, Pike, W.T, Lognonné, P, Banerdt, W.B, and Panning, Mark

Published
2021

9. Planetary Seismology: Nearly 3 years on Mars, and a return to the Moon

Author

Panning, Mark, Banerdt, W.B, Lognonné, P, Pike, W.T, Giardini, D, Lorenz, R, Bozdag, E, Clinton, J, Garcia, R, Irving, J, Kawamura, T, Kedar, S, Knapmeyer-Endrun, B, Margerin, L, Mimoun, D, Schmerr, N, Teanby, N, Weber, R, Hurst, K, Drilleau, M, Böse, M, Ceylan, S, Charalambous, C, van Driel, M, Horleston, A, Khan, A, Knapmeyer, M, Orhand-Mainsant, G, Stähler, S, Stott, A. E, Spiga, A, Fayon, L, Kenda, B, Brinkman, N, Lekic, V, Murdoch, N, Nunn, C, Schmelzbach, C, Schimmel, M, Stutzmann, E, Tauzin, B, Tharimena, S, Kedar, Sharon, Bowles, Neil, Bugby, David, Calcutt, Simon, Cutler, James, Elliott, John, Garcia, Raphael, Kawamura, Taichi, Lognonné, Philippe, Nunn, Ceri, Pike, W. Tom, Pont, Gabriel, de Raucourt, Sebastien, Standley, Ian, Walsh, William, Weber, Renee, and Yana, Charles

Published
2021

11. Stratification of Heterogeneity in the Lithosphere of Mars From Envelope Modeling of Event S1222a and Near Impacts: Interpretation and Implications for Very‐High‐Frequency Events

Author

Menina, S., primary, Margerin, L., additional, Kawamura, T., additional, Heller, G., additional, Drilleau, M., additional, Xu, Z., additional, Calvet, M., additional, Garcia, R. F., additional, Knapmeyer‐Endrun, B., additional, Carrasco, S., additional, Onodera, K., additional, Lognonné, P., additional, Stott, A., additional, and Banerdt, W. B., additional

Published
2023
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12. First observations of core-transiting seismic phases on Mars

Author

Irving, J. C. E., Lekic, V., Durán, C., Drilleau, M., Kim, D., Rivoldini, A., Khan, A., Samuel, H., Antonangeli, D., Bruce Banerdt, W., Beghein, C., Bozdagk, E., Ceylan, S., Charalambous, C., Clinton, J., Davis, P., Garcia, R., Giardini, D., Catherine Horleston, A., Huang, Q., Hurst, K. J., Kawamura, T., King, Scott D., Knapmeyer, M., Li, J., Lognonné, P., Maguire, R., Panning, M. P., Plesa, A. C., Schimmel, M., Schmerr, N. C., Stählerc, S. C., Stutzmann, E., Xu, Z., Irving, J. C. E., Lekic, V., Durán, C., Drilleau, M., Kim, D., Rivoldini, A., Khan, A., Samuel, H., Antonangeli, D., Bruce Banerdt, W., Beghein, C., Bozdagk, E., Ceylan, S., Charalambous, C., Clinton, J., Davis, P., Garcia, R., Giardini, D., Catherine Horleston, A., Huang, Q., Hurst, K. J., Kawamura, T., King, Scott D., Knapmeyer, M., Li, J., Lognonné, P., Maguire, R., Panning, M. P., Plesa, A. C., Schimmel, M., Schmerr, N. C., Stählerc, S. C., Stutzmann, E., and Xu, Z.

Abstract

We present the first observations of seismic waves propagating through the core of Mars. These observations, made using seismic data collected by the InSight geophysical mission, have allowed us to construct the first seismically constrained models for the elastic properties of Mars core. We observe core-Transiting seismic phase SKS from two farside seismic events detected on Mars and measure the travel times of SKS relative to mantle traversing body waves. SKS travels through the core as a compressional wave, providing information about bulk modulus and density. We perform probabilistic inversions using the core-sensitive relative travel times together with gross geophysical data and travel times from other, more proximal, seismic events to seek the equation of state parameters that best describe the liquid iron-Alloy core. Our inversions provide constraints on the velocities in Mars core and are used to develop the first seismically based estimates of its composition. We show that models informed by our SKS data favor a somewhat smaller (median core radius = 1,780 to 1,810 km) and denser (core density = 6.2 to 6.3 g/cm3) core compared to previous estimates, with a P-wave velocity of 4.9 to 5.0 km/s at the core mantle boundary, with the composition and structure of the mantle as a dominant source of uncertainty. We infer from our models that Mars core contains a median of 20 to 22 wt% light alloying elements when we consider sulfur, oxygen, carbon, and hydrogen. These data can be used to inform models of planetary accretion, composition, and evolution.

Published
2023

13. Characterization of Martian Convective Vortices Using InSight's Seismic and Meteorological Data

Author

Onodera, K., Nishida, Kiwamu, Kawamura, T., Murdoch, N., Otsuka, R., Drilleau, M., Schimmel, Martin, Carrasco, S., Sainton, G., Horleston, A., Tanaka, S., Mitani, T., Perrin, C., Stutzmann, Eléonore, Rodriguez, S., Lorenz, R., Spiga, A., Lognonné, Philippe, Banerdt, William Bruce, Onodera, K., Nishida, Kiwamu, Kawamura, T., Murdoch, N., Otsuka, R., Drilleau, M., Schimmel, Martin, Carrasco, S., Sainton, G., Horleston, A., Tanaka, S., Mitani, T., Perrin, C., Stutzmann, Eléonore, Rodriguez, S., Lorenz, R., Spiga, A., Lognonné, Philippe, and Banerdt, William Bruce

Abstract

From Nov. 2018 to Dec. 2022, NASA's InSight (Interior Exploration using Seismic Investigations, Geodesy, and Heat Transport) was operated on Mars to conduct seismic and meteorological observations. InSight¿s long quasicontinuous and high-temporal sampling observations have significantly improved our understandings of the inner structure, seismicity, and meteorological phenomena of the red planet (e.g., [1]-[8]). Prominent among these are convective vortices or dust devils.

Published
2023

14. Description of Martian convective vortices observed by InSight and implications for vertical vortex structure and subsurface physical properties

Author

NASA Astrobiology Institute (US), Centre National de la Recherche Scientifique (France), Japan Society for the Promotion of Science, Onodera, K., Nishida, Kiwamu, Kawamura, Taichi, Murdoch, Naomi, Drilleau, M., Otsuka, Ryoji, Lorenz, Ralph, Horleston, Anna, Widmer-Schnidrig, Rudolf, Schimmel, Martin, Rodriguez, Sebastien, Carrasco, Sebastián, Tanaka, Satoshi, Perrin, Clément, Lognonné, Philippe, Spiga, Aymeric, Banfield, Don, Panning, Mark, Banerdt, William Bruce, NASA Astrobiology Institute (US), Centre National de la Recherche Scientifique (France), Japan Society for the Promotion of Science, Onodera, K., Nishida, Kiwamu, Kawamura, Taichi, Murdoch, Naomi, Drilleau, M., Otsuka, Ryoji, Lorenz, Ralph, Horleston, Anna, Widmer-Schnidrig, Rudolf, Schimmel, Martin, Rodriguez, Sebastien, Carrasco, Sebastián, Tanaka, Satoshi, Perrin, Clément, Lognonné, Philippe, Spiga, Aymeric, Banfield, Don, Panning, Mark, and Banerdt, William Bruce

Abstract

Convective vortices (whirlwinds) and dust devils (dust-loaded vortices) are one of the most common phenomena on Mars. They reflect the local thermodynamical structure of the atmosphere and are the driving force of the dust cycle. Additionally, they cause an elastic ground deformation, which is useful for retrieving the subsurface rigidity. Therefore, investigating convective vortices with the right instrumentation can lead to a better understanding of the Martian atmospheric structures as well as the subsurface physical properties. In this study, we quantitatively characterized the convective vortices detected by NASA's InSight (~13,000 events) using meteorological (e.g., pressure, wind speed, temperature) and seismic data. The evaluated parameters, such as the signal-to-noise ratio, event duration, asymmetricity of pressure drop profiles, and cross-correlation between seismic and pressure signals, are compiled as a catalog. Using these parameters, we investigated (a) the vortex structure and (b) the subsurface physical properties. Regarding the first topic, we tried to illustrate the vertical vortex structure and its link to the shape of the pressure profiles by combining the asymmetrical features seen in the observed pressure drops and the terrestrial observations of dust devils. Our results indicate that most of the vortices move with the wall tilted in the advection direction. Concerning the second topic, selecting the highly correlated events between pressure perturbation and ground response, we estimated the subsurface rigidity at the InSight landing site down to 100 m depth. Our results indicate that the subsurface structure can be modeled with two layers having a transition at 5¿15 m depth.

Published
2023

15. First observations of core-Transiting seismic phases on Mars

Author

Université Paris Cité, European Research Council, Irving, Jessica C. E., Lekic, Vedran, Duran, C., Drilleau, M., Kim, D., Rivoldini, A., Khan, A., Samuel, H., Antonangeli, D., Bruce Banerdt, W., Beghein, C., Bozdagk, E., Ceylan, S., Charalambous, C., Clinton, John, Davis, P., García, R., Giardini, Domenico, Catherine Horleston, A., Huang, Q., Hurst, Kenneth J., Kawamura, T., King, S. D., Knapmeyer, M., Li, J., Lognonné, Philippe, Maguire, R., Panning, M.P., Plesa, A.C., Schimmel, Martin, Schmerr, N. C., Stählerc, S. C., Stutzmann, Eléonore, Xu, Z., Université Paris Cité, European Research Council, Irving, Jessica C. E., Lekic, Vedran, Duran, C., Drilleau, M., Kim, D., Rivoldini, A., Khan, A., Samuel, H., Antonangeli, D., Bruce Banerdt, W., Beghein, C., Bozdagk, E., Ceylan, S., Charalambous, C., Clinton, John, Davis, P., García, R., Giardini, Domenico, Catherine Horleston, A., Huang, Q., Hurst, Kenneth J., Kawamura, T., King, S. D., Knapmeyer, M., Li, J., Lognonné, Philippe, Maguire, R., Panning, M.P., Plesa, A.C., Schimmel, Martin, Schmerr, N. C., Stählerc, S. C., Stutzmann, Eléonore, and Xu, Z.

Abstract

We present the first observations of seismic waves propagating through the core of Mars. These observations, made using seismic data collected by the InSight geophysical mission, have allowed us to construct the first seismically constrained models for the elastic properties of Mars core. We observe core-Transiting seismic phase SKS from two farside seismic events detected on Mars and measure the travel times of SKS relative to mantle traversing body waves. SKS travels through the core as a compressional wave, providing information about bulk modulus and density. We perform probabilistic inversions using the core-sensitive relative travel times together with gross geophysical data and travel times from other, more proximal, seismic events to seek the equation of state parameters that best describe the liquid iron-Alloy core. Our inversions provide constraints on the velocities in Mars core and are used to develop the first seismically based estimates of its composition. We show that models informed by our SKS data favor a somewhat smaller (median core radius = 1,780 to 1,810 km) and denser (core density = 6.2 to 6.3 g/cm3) core compared to previous estimates, with a P-wave velocity of 4.9 to 5.0 km/s at the core mantle boundary, with the composition and structure of the mantle as a dominant source of uncertainty. We infer from our models that Mars core contains a median of 20 to 22 wt% light alloying elements when we consider sulfur, oxygen, carbon, and hydrogen. These data can be used to inform models of planetary accretion, composition, and evolution.

Published
2023

16. Detection of Mars Normal Modes From S1222a Event and Seismic Hum

Author

Agence Nationale de la Recherche (France), Lognonné, Philippe, Schimmel, Martin, Stutzmann, Eleonore, Davis, P., Drilleau, M., Sainton, G., Kawamura, T., Panning, M.P., Banerdt, W. B., Agence Nationale de la Recherche (France), Lognonné, Philippe, Schimmel, Martin, Stutzmann, Eleonore, Davis, P., Drilleau, M., Sainton, G., Kawamura, T., Panning, M.P., and Banerdt, W. B.

Abstract

We present the first detection of normal modes on Mars using the vertical records from InSight's broad-band seismometer following the marsquake that occurred on sol 1222. The proposed catalog lists 60 potential eigenfrequencies between 3 and 12 mHz. Due to their low signal-to-noise ratio, these normal modes were detected using the phasor walkout approach. The normal modes amplitudes are consistent with the upper limit of the S1222a magnitude and with high quality factors. Additionally, we provide the first detection of a Martian hum before the quake for several of these frequencies. The proposed frequencies are at about 1-sigma of those predicted by published models based on body wave travel time inversions. Our detection of normal modes is the first made on a terrestrial planet other than Earth and opens the way for future interior models that incorporate both normal modes frequencies, surface waves velocities and body wave travel times.

Published
2023

17. The Marsquake Service: Securing Daily Analysis of SEIS Data and Building the Martian Seismicity Catalogue for InSight

Author

Clinton, J., Giardini, D., Böse, M., Ceylan, S., van Driel, M., Euchner, F., Garcia, R. F., Kedar, S., Khan, A., Stähler, S. C., Banerdt, B., Lognonne, P., Beucler, E., Daubar, I., Drilleau, M., Golombek, M., Kawamura, T., Knapmeyer, M., Knapmeyer-Endrun, B., Mimoun, D., Mocquet, A., Panning, M., Perrin, C., and Teanby, N. A.

Published
2018
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18. New discoveries about the cores of Mars and the Earth

Author

Irving, J., Lekic, V., Duran, C., Drilleau, M., Kim, D., Rivoldini, A., Khan, A., Samuel, H., Cottaar, S., Horleston, A., Russell, S., Wu, W., and InSight Science Team, I.

Abstract

More than one hundred years of seismological, mineralogical and geophysical research have shed light on the properties and evolution of Earth’s core. A liquid outer core, hosting the geodynamo, and a solid inner core, growing slowly at the expense of the outer core, together span roughly half of Earth’s diameter. The presence of a light-element enriched layer at the core-mantle interface, along with layering and lateral variation deeper in the core remain areas of active investigation.In contrast, the first confirmed marsquakes, detected by the InSight mission, were recorded only in 2019. Thus we have enjoyed only a few years of in-situ seismic observations of waves propagating through Mars’ interior. With well over a thousand seismic events detected in InSight’s operational life, seismic waves have been detected from marsquakes and impacts at large and small epicentral distances. Two seismic events have permitted the detection of core-transiting seismic (SKS) waves. These observations have enabled the estimation of the elastic properties of Mars’ liquid core and allowed inferences to be made about its composition, which is enriched in light elements when compared to Earth. This presentation will highlight new discoveries about Mars’ core and put them into context by comparing them with known and unknown features of Earth’s core., The 28th IUGG General Assembly (IUGG2023) (Berlin 2023)

Published
2023
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22. Largest recent impact craters on Mars: Orbital imaging and surface seismic co-investigation

Author

Posiolova, L. V., primary, Lognonné, P., additional, Banerdt, W. B., additional, Clinton, J., additional, Collins, G. S., additional, Kawamura, T., additional, Ceylan, S., additional, Daubar, I. J., additional, Fernando, B., additional, Froment, M., additional, Giardini, D., additional, Malin, M. C., additional, Miljković, K., additional, Stähler, S. C., additional, Xu, Z., additional, Banks, M. E., additional, Beucler, É., additional, Cantor, B. A., additional, Charalambous, C., additional, Dahmen, N., additional, Davis, P., additional, Drilleau, M., additional, Dundas, C. M., additional, Durán, C., additional, Euchner, F., additional, Garcia, R. F., additional, Golombek, M., additional, Horleston, A., additional, Keegan, C., additional, Khan, A., additional, Kim, D., additional, Larmat, C., additional, Lorenz, R., additional, Margerin, L., additional, Menina, S., additional, Panning, M., additional, Pardo, C., additional, Perrin, C., additional, Pike, W. T., additional, Plasman, M., additional, Rajšić, A., additional, Rolland, L., additional, Rougier, E., additional, Speth, G., additional, Spiga, A., additional, Stott, A., additional, Susko, D., additional, Teanby, N. A., additional, Valeh, A., additional, Werynski, A., additional, Wójcicka, N., additional, and Zenhäusern, G., additional

Published
2022
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23. Surface waves and crustal structure on Mars

Author

Kim, D., primary, Banerdt, W. B., additional, Ceylan, S., additional, Giardini, D., additional, Lekić, V., additional, Lognonné, P., additional, Beghein, C., additional, Beucler, É., additional, Carrasco, S., additional, Charalambous, C., additional, Clinton, J., additional, Drilleau, M., additional, Durán, C., additional, Golombek, M., additional, Joshi, R., additional, Khan, A., additional, Knapmeyer-Endrun, B., additional, Li, J., additional, Maguire, R., additional, Pike, W. T., additional, Samuel, H., additional, Schimmel, M., additional, Schmerr, N. C., additional, Stähler, S. C., additional, Stutzmann, E., additional, Wieczorek, M., additional, Xu, Z., additional, Batov, A., additional, Bozdag, E., additional, Dahmen, N., additional, Davis, P., additional, Gudkova, T., additional, Horleston, A., additional, Huang, Q., additional, Kawamura, T., additional, King, S. D., additional, McLennan, S. M., additional, Nimmo, F., additional, Plasman, M., additional, Plesa, A. C., additional, Stepanova, I. E., additional, Weidner, E., additional, Zenhäusern, G., additional, Daubar, I. J., additional, Fernando, B., additional, Garcia, R. F., additional, Posiolova, L. V., additional, and Panning, M. P., additional

Published
2022
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28. MSS/1: Single-Station and Single-Event Marsquake Inversion

Author

Drilleau, M, Drilleau, M, Beucler, É, Lognonné, P, Panning, MP, Knapmeyer-Endrun, B, Banerdt, WB, Beghein, C, Ceylan, S, van Driel, M, Joshi, R, Kawamura, T, Khan, A, Menina, S, Rivoldini, A, Samuel, H, Stähler, S, Xu, H, Bonnin, M, Clinton, J, Giardini, D, Kenda, B, Lekic, V, Mocquet, A, Murdoch, N, Schimmel, M, Smrekar, SE, Stutzmann, É, Tauzin, B, Tharimena, S, Drilleau, M, Drilleau, M, Beucler, É, Lognonné, P, Panning, MP, Knapmeyer-Endrun, B, Banerdt, WB, Beghein, C, Ceylan, S, van Driel, M, Joshi, R, Kawamura, T, Khan, A, Menina, S, Rivoldini, A, Samuel, H, Stähler, S, Xu, H, Bonnin, M, Clinton, J, Giardini, D, Kenda, B, Lekic, V, Mocquet, A, Murdoch, N, Schimmel, M, Smrekar, SE, Stutzmann, É, Tauzin, B, and Tharimena, S

Abstract

SEIS, the seismometer of the InSight mission, which landed on Mars on 26 November 2018, is monitoring the seismic activity of the planet. The goal of the Mars Structure Service (MSS) is to provide, as a mission product, the first average 1-D velocity model of Mars from the recorded InSight data. Prior to the mission, methodologies have been developed and tested to allow the location of the seismic events and estimation of the radial structure, using surface waves and body waves arrival times, and receiver functions. The paper describes these validation tests and compares the performance of the different algorithms to constrain the velocity model below the InSight station and estimate the 1-D average model over the great circle path between source and receiver. These tests were performed in the frame of a blind test, during which synthetic data were inverted. In order to propagate the data uncertainties on the output model distribution, Bayesian inversion techniques are mainly used. The limitations and strengths of the methods are assessed. The results show the potential of the MSS approach to retrieve the structure of the crust and underlying mantle. However, at this time, large quakes with clear surface waves have not yet been recorded by SEIS, which makes the estimation of the 1-D average seismic velocity model challenging. Additional locatable events, especially at large epicentral distances, and development of new techniques to fully investigate the data, will ultimately provide more constraints on the crust and mantle of Mars.

Published
2020

29. Surface waves and crustal structure on Mars

Author

Kim, D., Banerdt, W. B., Ceylan, S., Giardini, D., Lekic, V., Lognonne, P., Beghein, C., Beucler, E., Carrasco, S., Charalambous, C., Clinton, J., Drilleau, M., Duran, C., Golombek, M., Joshi, R., Khan, A., Knapmeyer-Endrun, B., Li, J., Maguire, R., Pike, W. T., Samuel, H., Schimmel, M., Schmerr, N. C., Stahler, S. C., Stutzmann, E., Wieczorek, M., Xu, Z., Batov, A., Bozdag, E., Dahmen, N., Davis, P., Gudkova, T., Horleston, A., Huang, Q., Kawamura, T., King, Scott D., McLennan, S. M., Nimmo, F., Plasman, M., Plesa, A. C., Stepanova, I. E., Weidner, E., Zenhausern, G., Daubar, I. J., Fernando, B., Garcia, R. F., Posiolova, L., Panning, M. P., Kim, D., Banerdt, W. B., Ceylan, S., Giardini, D., Lekic, V., Lognonne, P., Beghein, C., Beucler, E., Carrasco, S., Charalambous, C., Clinton, J., Drilleau, M., Duran, C., Golombek, M., Joshi, R., Khan, A., Knapmeyer-Endrun, B., Li, J., Maguire, R., Pike, W. T., Samuel, H., Schimmel, M., Schmerr, N. C., Stahler, S. C., Stutzmann, E., Wieczorek, M., Xu, Z., Batov, A., Bozdag, E., Dahmen, N., Davis, P., Gudkova, T., Horleston, A., Huang, Q., Kawamura, T., King, Scott D., McLennan, S. M., Nimmo, F., Plasman, M., Plesa, A. C., Stepanova, I. E., Weidner, E., Zenhausern, G., Daubar, I. J., Fernando, B., Garcia, R. F., Posiolova, L., and Panning, M. P.

Abstract

We detected surface waves from two meteorite impacts on Mars. By measuring group velocity dispersion along the impact-lander path, we obtained a direct constraint on crustal structure away from the InSight lander. The crust north of the equatorial dichotomy had a shear wave velocity of approximately 3.2 kilometers per second in the 5- to 30-kilometer depth range, with little depth variation. This implies a higher crustal density than inferred beneath the lander, suggesting either compositional differences or reduced porosity in the volcanic areas traversed by the surface waves. The lower velocities and the crustal layering observed beneath the landing site down to a 10-kilometer depth are not a global feature. Structural variations revealed by surface waves hold implications for models of the formation and thickness of the martian crust.

Published
2022

30. Surface waves and crustal structure on Mars

Author

ETH Zurich, NASA Astrobiology Institute (US), Agence Nationale de la Recherche (France), UK Space Agency, California Institute of Technology, National Aeronautics and Space Administration (US), Kim, D., Banerdt, W. B., Ceylan, S., Giardini, Domenico, Lekic, Vedran, Lognonné, P., Beghein, C., Beucler, E., Carrasco, Sebastián, Charalambous, C., Clinton, John F., Drilleau, M., Duran, C., Golombek, M. P., Joshi, R., Khan, A., Knapmeyer‐Endrun, Brigitte, Li, J., Maguire, R., Pike, William T., Samuel, H., Schimmel, Martin, Schmerr, Nicholas C., Stähler, S. C., Stutzmann, E., Wieczorek, M., Xu, Z. D., Batov, A., Bozdag, E., Dahmen, N., Davis, P., Gudkova, T., Horleston, A., Huang, Quancheng, Kawamura, T., King, S., McLennan, S M, Nimmo, F., Plasman, M., Plesa, A. C., Stepanova, I. E., Weidner, E., Zenhäusern, Geraldine, Daubar, I., Fernando, B., García, R. F., Posiolova, L. V., Panning, Mark P., ETH Zurich, NASA Astrobiology Institute (US), Agence Nationale de la Recherche (France), UK Space Agency, California Institute of Technology, National Aeronautics and Space Administration (US), Kim, D., Banerdt, W. B., Ceylan, S., Giardini, Domenico, Lekic, Vedran, Lognonné, P., Beghein, C., Beucler, E., Carrasco, Sebastián, Charalambous, C., Clinton, John F., Drilleau, M., Duran, C., Golombek, M. P., Joshi, R., Khan, A., Knapmeyer‐Endrun, Brigitte, Li, J., Maguire, R., Pike, William T., Samuel, H., Schimmel, Martin, Schmerr, Nicholas C., Stähler, S. C., Stutzmann, E., Wieczorek, M., Xu, Z. D., Batov, A., Bozdag, E., Dahmen, N., Davis, P., Gudkova, T., Horleston, A., Huang, Quancheng, Kawamura, T., King, S., McLennan, S M, Nimmo, F., Plasman, M., Plesa, A. C., Stepanova, I. E., Weidner, E., Zenhäusern, Geraldine, Daubar, I., Fernando, B., García, R. F., Posiolova, L. V., and Panning, Mark P.

Abstract

We detected surface waves from two meteorite impacts on Mars. By measuring group velocity dispersion along the impact-lander path, we obtained a direct constraint on crustal structure away from the InSight lander. The crust north of the equatorial dichotomy had a shear wave velocity of approximately 3.2 kilometers per second in the 5- to 30-kilometer depth range, with little depth variation. This implies a higher crustal density than inferred beneath the lander, suggesting either compositional differences or reduced porosity in the volcanic areas traversed by the surface waves. The lower velocities and the crustal layering observed beneath the landing site down to a 10-kilometer depth are not a global feature. Structural variations revealed by surface waves hold implications for models of the formation and thickness of the martian crust.

Published
2022

31. Largest recent impact craters on Mars: Orbital imaging and surface seismic co-investigation

Author

Posiolova, L.V., Lognonné, P., Banerdt, W.B., Clinton, J., Collins, G.S., Kawamura, T., Ceylan, S., Daubar, I.J., Fernando, B., Froment, M., Giardini, D., Malin, M.C., Miljković, Katarina, Stähler, S.C., Xu, Z., Banks, M.E., Beucler, Cantor, B.A., Charalambous, C., Dahmen, N., Davis, P., Drilleau, M., Dundas, C.M., Durán, C., Euchner, F., Garcia, R.F., Golombek, M., Horleston, A., Keegan, C., Khan, A., Kim, D., Larmat, C., Lorenz, R., Margerin, L., Menina, S., Panning, M., Pardo, C., Perrin, C., Pike, W.T., Plasman, M., Rajšić, Andrea, Rolland, L., Rougier, E., Speth, G., Spiga, A., Stott, A., Susko, D., Teanby, N.A., Valeh, A., Werynski, A., Wójcicka, N., Zenhäusern, G., Posiolova, L.V., Lognonné, P., Banerdt, W.B., Clinton, J., Collins, G.S., Kawamura, T., Ceylan, S., Daubar, I.J., Fernando, B., Froment, M., Giardini, D., Malin, M.C., Miljković, Katarina, Stähler, S.C., Xu, Z., Banks, M.E., Beucler, Cantor, B.A., Charalambous, C., Dahmen, N., Davis, P., Drilleau, M., Dundas, C.M., Durán, C., Euchner, F., Garcia, R.F., Golombek, M., Horleston, A., Keegan, C., Khan, A., Kim, D., Larmat, C., Lorenz, R., Margerin, L., Menina, S., Panning, M., Pardo, C., Perrin, C., Pike, W.T., Plasman, M., Rajšić, Andrea, Rolland, L., Rougier, E., Speth, G., Spiga, A., Stott, A., Susko, D., Teanby, N.A., Valeh, A., Werynski, A., Wójcicka, N., and Zenhäusern, G.

Abstract

Two >130-meter-diameter impact craters formed on Mars during the later half of 2021. These are the two largest fresh impact craters discovered by the Mars Reconnaissance Orbiter since operations started 16 years ago. The impacts created two of the largest seismic events (magnitudes greater than 4) recorded by InSight during its 3-year mission. The combination of orbital imagery and seismic ground motion enables the investigation of subsurface and atmospheric energy partitioning of the impact process on a planet with a thin atmosphere and the first direct test of martian deep-interior seismic models with known event distances. The impact at 35°N excavated blocks of water ice, which is the lowest latitude at which ice has been directly observed on Mars.

Published
2022

32. An autonomous lunar geophysical experiment package (ALGEP) for future space missions: In response to Call for White Papers for the Voyage 2050 long-term plan in the ESA Science Program

Author

Kawamura, T., Grott, M., Garcia, R., Wieczorek, M., de Raucourt, S., Lognonné, P., Bernauer, F., Breuer, D., Clinton, J., Delage, P., Drilleau, M., Ferraioli, L., Fuji, N., Horleston, A., Kletetschka, G., Knapmeyer, M., Knapmeyer-Endrun, B., Padovan, S., Plesa, A.C., Rivoldini, A., Robertsson, J., Rodriguez, S., Stähler, S.C., Stutzmann, E., Teanby, N.A., Tosi, N., Vrettos, C., Banerdt, B., Fa, W., Huang, Q., Irving, J., Ishihara, Y., Miljković, Katarina, Mittelholz, A., Nagihara, S., Neal, C., Qu, S., Schmerr, N., Tsuji, T., Kawamura, T., Grott, M., Garcia, R., Wieczorek, M., de Raucourt, S., Lognonné, P., Bernauer, F., Breuer, D., Clinton, J., Delage, P., Drilleau, M., Ferraioli, L., Fuji, N., Horleston, A., Kletetschka, G., Knapmeyer, M., Knapmeyer-Endrun, B., Padovan, S., Plesa, A.C., Rivoldini, A., Robertsson, J., Rodriguez, S., Stähler, S.C., Stutzmann, E., Teanby, N.A., Tosi, N., Vrettos, C., Banerdt, B., Fa, W., Huang, Q., Irving, J., Ishihara, Y., Miljković, Katarina, Mittelholz, A., Nagihara, S., Neal, C., Qu, S., Schmerr, N., and Tsuji, T.

Abstract

Geophysical observations will provide key information about the inner structure of the planets and satellites and understanding the internal structure is a strong constraint on the bulk composition and thermal evolution of these bodies. Thus, geophysical observations are a key to uncovering the origin and evolution of the Moon. In this article, we propose the development of an autonomous lunar geophysical experiment package, composed of a suite of instruments and a central station with standardized interface, which can be installed on various future lunar missions. By fixing the interface between instruments and the central station, it would be possible to easily configure an appropriate experiment package for different missions. We describe here a series of geophysical instruments that may be included as part of the geophysical package: a seismometer, a magnetometer, a heat flow probe, and a laser reflector. These instruments will provide mechanical, thermal, and geodetic parameters of the Moon that are strongly related to the internal structure. We discuss the functionality required for future geophysical observations of the Moon, including the development of the central station that will be used commonly by different payloads.

Published
2022

33. First observations of seismic waves travelling through the Martian core

Author

Irving, J. C. E., Antonangeli, D., Banerdt, B., Beghein, C., Bozdag, E., Ceylan, S., Clinton, J., Drilleau, M., Duran, C., Garcia, Raphaël F., Giardini, D., Horleston, A., Huang, Quancheng, Hurst, K., Kawamura, T., Khan, A., Kim, D., King, S., Knapmeyer, Martin, Lekic, V., Li, J., Lognonne, P., Maguire, R., Panning, M., Plesa, Ana-Catalina, Rivoldini, A., Schimmel, M., Schmerr, N., Samuel, Henri, Stähler, S., Stutzmann, Éléonore, and Xu, Z.

Subjects
Seismic waves, Martian core, Mars, InSight
Published
2022

34. SEIS achievement for Mars Seismology after 1000 sols of seismic monitoring

Author

Lognonne, P., Banerdt, William B., Giardini, D., Panning, M.P., Pike, W.T., Barakoui, S., Böse, Maren, Brinkman, Nienke, Charalambous, C., Compaire, Nicolas, Dahmen, N., Drilleau, M., Fernando, B., Garcia, R., Hobiger, M., Huang, Q., Hurst, K., Jacob, A., Karakostas, F., Kawamura, T., Kedar, S., Khan, A., Kim, D., Knapmeyer‐Endrun, Brigitte, Knapmeyer, Martin, Li, Jiaqi, Menina, S., Murdoch, N., Onodera, K, Perrin, C, Pou, L., Rajsic, A., Samuel, H., Savoie, D., Schimmel, M., Sollberger, D., Stähler, S., Stott, A., Gyalay, S, Van Driel, M., Wojcicka, N., Zweifel, P., Beghein, C., Beucler, E., Antonangeli, D., Banfield, D., Bowles, Neil, Bozdag, E., Christensen, Ulrich, Clinton, J., Collins, G., Daubar, I., Irving, J. C. E., Lorenz, R. D., Margerin, L., Michaut, Chloe, Mimoun, D., Nimmo, Francis, Plesa, Ana-Catalina, Schmerr, N., Smrekar, S., Spiga, A., Teanby, N., Tromp, J., Weber, R., Wieczorek, M., Agard, C., Barrett, Elizabeth, Berenguer, J.L., Ceylan, S., Conejero, V., Duran, C., Froment, M., Horleston, A., Ferrier, C., Fuji, N., Gabsi, T., Gaudin, E., Jaillant, B., Jullien, A., Meunier, F., Pardo, C., ten Pierick, J., Plasman, M., Rochas, L., Sainton, G., Stutzmann, Éléonore, Xu, Z., Yana, Charles, Zenhäusern, Geraldine, and InSight/SEIS, Science Team

Subjects
Mars InSight SEIS
Published
2022

35. Crustal structure of Mars from the first observation of surface waves

Author

Kim, D., Banerdt, W.B., Ceylan, S., Giardini, D., Lekic, V., Lognonne, P., Beghein, C., Beucler, E., Carrasco, S., Charalambous, C., Clinton, J., Drilleau, M., Duran, C., Golombek, M., Joshi, Rakshit, Khan, A., Knapmeyer-Endrun, B., Li, J., Maguire, R., Pike, W.T., Samuel, H., Schimmel, M., Schmerr, N., Stähler, S., Stutzmann, Éléonore, Wieczorek, M., Xu, Z., Batov, A., Bozdag, E., Dahmen, N., Davis, P., Gudkova, T., Horleston, A., Huang, Quancheng, Kawamura, T., King, S., McLennan, S M, Nimmo, F., Plasman, M., Plesa, Ana-Catalina, Stepanova, I., Weidner, E., Zenhäusern, Geraldine, Daubar, I., Fernando, B., Garcia, R., Posiolova, L., and Panning, M.

Subjects
Mars, Crustal structure, Surface waves, InSight
Published
2022

37. The Polarization of Ambient Noise on Mars

Author

Stutzmann, E., Schimmel, Martin, Lognonne, P., Horleston, Anna, Ceylan, S., van Driel, M., Stahler, Simon, Banerdt, B., Calvet, Marie, Charalambous, C., Clinton, John, Drilleau, M., Fayon, Lucile, Garcia, Raphael, Jacob, A., Kawamura, T., Kenda, B., Margerin, Ludovic, Murdoch, N., and Panning, Mark

Subjects
Mars, Seismology, Physics::Geophysics
Abstract

vEGU21: Gather Online | 19–30 April 2021, 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 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. 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.

Published
2021

38. One Martian Year of Seismic Monitoring of Mars by InSight: SEIS Results and Perspectives for the Extended Mission

Author

Lognonne, P., Banerdt, B., Giardini, D., Panning, M., Pike, T., Antonangeli, D., Ballestra, J., Banfield, D., Beghein, C., Beucler, E., Bowles, Neil, Bozdag, E., Ceylan, S., Charalambous, C., Christensen, U., Clinton, J., Compaire, Nicolas, Collins, G., Dahmen, N., Daubar, I., van Driel, M, Drilleau, M., Fernando, B., Froment, M., Garcia, R., Irving, J., Khan, A., Kawamura, T., Kedar, S., Kenda, B., Knapmeyer-Endrun, B., Lorenz, R. D., Margerin, L., Martire, L., Michaut, C., Mimoun, D., Murdoch, N., Nimmo, F., Perrin, C, Plesa, Ana-Catalina, Schmerr, N., Scholz, J.-R., Smrekar, S., Sollberger, D., Spiga, A., Stähler, S., Stutzmann, Éléonore, Teanby, N., Tromp, J., Weber, R., Wieczorek, M., Wojcicka, N., Xu, H., Agard, C., Barrett, Elizabeth, Berenguer, J.L., Böse, Maren, Conejero, V., Horleston, A., Hurst, K., Ferrier, C., Fuji, N., Gabsi, T., Gaudin, E., Jaillant, B., Jullien, A., Karakostas, F., Labrot, P., Meunier, F., Pardo, C., ten Pierick, J., Plasman, Matthieu, Rochas, L., Sauron, A., Sainton, G., Xu, Z., Yana, Charles, and InSight/SEIS, Science Team

Subjects
Mars, SEIS, InSight
Published
2021

39. Seismic detection of the martian core by InSight

Author

Stähler, S., Ceylan, S., Duran, Andrea Cecilia, Garcia, Raphaël F., Giardini, D., Huang, Quancheng, Khan, Amir, Kim, Doyeon, Lognonne, P., Maguire, R., Marusiak, A, Plesa, Ana-Catalina, Samuel, H., Schmerr, N., Schimmel, M., Sollberger, D., Stutzmann, Éléonore, Antonangeli, D., Clinton, J., van Driel, M, Drilleau, M., Gudkova, T., Horleston, A., Irving, J., Kawamura, T., Lekic, V., Myhill, R., Nimmo, F., Panning, M., Rivoldini, A., Schmelzbach, C., Stanley, S., Weber, Renee, Xu, Zongbo, Zenhäusern, Geraldine, and Banerdt, B.

Subjects
Core detection, Mars, Seismic measurements, InSight
Abstract

A plethora of geophysical, geo- chemical, and geodynamical observations indicate that the terrestrial planets have differentiated into silicate crusts and mantles that surround a dense core. The latter consists primarily of Fe and some lighter alloying elements (e.g., S, Si, C, O, and H) [1]¿. The Martian meteorites show evidence of chalcophile element depletion, suggesting that the otherwise Fe-Ni- rich core likely contains a sulfide component, which influences physical state.

Published
2021

40. The interior of Mars as seen by InSight (Invited)

Author

Staehler, Simon C., Khan, A., Knapmeyer‐Endrun, Brigitte, Panning, Mark P., Banerdt, William B., Lognonné, P., Giardini, Domenico, Antonangeli, D., Beucler, E., Bissig, F., Bozdag, E., Brinkmann, N., Ceylan, S., Charalambous, C., Clinton, John F., Compaire, Nicolas, Dahmen, N. L., Davis, P., van Driel, M., Drilleau, M., Garcia, Raphael F., Huang, Quancheng, Joshi, Rakshit, Gudkova, T., Irving, Jessica C. E., Johnson, C., Kawamura, T., Kim, Doyeon, Knapmeyer, Martin, Maguire, R., Lekic, Vedran, Margerin, L., Marusiak, A, McLennan, S M, Mittelholz, A., Michaut, Chloe, Plasman, M., Pan, L., Duran, C., Perrin, C., Pike, T., Plesa, Ana-Catalina, Pinot, Baptiste, Rivoldini, A., Scholz, J.-R., Schimmel, Martin, Schmerr, N., Stutzmann, Éléonore, Samuel, H., Smrekar, S., Spohn, Tilman, Tauzin, B., Tharimena, S., Widmer-Schnidrig, R, Wieczorek, M., Xu, Zongbo, Zenhäusern, Geraldine, Karakostas, F., and InSight, Science Team

Abstract

InSight is the first planetary mission dedicated to exploring the whole interior of a planet using geophysical methods, specifically seismology and geodesy. To this end, we observed seismic waves of distant marsquakes and inverted for interior models using differential travel times of phases reflected at the surface (PP, SS...) or the core mantle-boundary (ScS), as well as those converted at crustal interfaces. Compared to previous orbital observations1-3, the seismic data added decisive new insights with consequences for the formation of Mars: The global average crustal thickness of 24-75 km is at the low end of pre-mission estimates5. Together with the the thick lithosphere of 450-600 km5, this requires an enrichment of heat-producing elements in the crust by a factor of 13-20, compared to the primitive mantle. The iron-rich liquid core is 1790-1870 km in radius6, which rules out the existence of an insulating bridgmanite-dominated lower mantle on Mars. The large, and therefore low-density core needs a high amount of light elements. Given the geochemical boundary conditions, Sulfur alone cannot explain the estimated density of ~6 g/cm3 and volatile elements, such as oxygen, carbon or hydrogen are needed in significant amounts. This observation is difficult to reconcile with classical models of late formation from the same material as Earth. We also give an overview of open questions after three years of InSight operation on the surface of Mars, such as the potential existence of an inner core or compositional layers above the CMB

Published
2021

41. Seismic detection of the martian core by InSight

Author

Schimmel, Martin, Stähler, S. C., Savas, Ceylan, Duran, A. C., García, Raphael, Giardini, Domenico, Huang, Quancheng, Khan, A., Kim, Doyeon, Lognonné, P., Maguire, Ross, Marusiak, A. G., Plesa, A. C., Samuel, Henri, Schmerr, Nicholas C., Sollberger, David, Stutzmann, E., Antonangeli, D., Clinton, John F., van Driel, M., Drilleau, M., Gudkova, T., Horleston, Anna, Irving, J., Kawamura, T., Lekic, Vedran, Myhill, Robert, Nimmo, F., Panning, Mark, Rivoldini, A., Schmelzbach, C., Stanley, S., Weber, R., Xu, Zongbo, Zenhäusern, G., Banerdt, W. B., Schimmel, Martin, Stähler, S. C., Savas, Ceylan, Duran, A. C., García, Raphael, Giardini, Domenico, Huang, Quancheng, Khan, A., Kim, Doyeon, Lognonné, P., Maguire, Ross, Marusiak, A. G., Plesa, A. C., Samuel, Henri, Schmerr, Nicholas C., Sollberger, David, Stutzmann, E., Antonangeli, D., Clinton, John F., van Driel, M., Drilleau, M., Gudkova, T., Horleston, Anna, Irving, J., Kawamura, T., Lekic, Vedran, Myhill, Robert, Nimmo, F., Panning, Mark, Rivoldini, A., Schmelzbach, C., Stanley, S., Weber, R., Xu, Zongbo, Zenhäusern, G., and Banerdt, W. B.

Abstract

A plethora of geophysical, geo- chemical, and geodynamical observations indicate that the terrestrial planets have differentiated into silicate crusts and mantles that surround a dense core. The latter consists primarily of Fe and some lighter alloying elements (e.g., S, Si, C, O, and H) [1]¿. The Martian meteorites show evidence of chalcophile element depletion, suggesting that the otherwise Fe-Ni- rich core likely contains a sulfide component, which influences physical state.

Published
2021

42. The Polarization of Ambient Noise on Mars

Author

Agence Nationale de la Recherche (France), UK Space Agency, Ministerio de Ciencia, Innovación y Universidades (España), Schimmel, Martin [0000-0003-2601-4462], Stutzmann, E., Schimmel, Martin, Lognonné, P., Horleston, A., Ceylan, S., van Driel, M., Stähler, S., Banerdt, B., Calvet, M., Charalambous, C., Clinton, John F., Drilleau, M., Fayon, L., Garcia, R. F., Giardini, Domenico, Hurst, K., Jacob, A., Kawamura, T., Kenda, B., Margerin, L., Murdoch, N., Panning, M., Pike, T., Scholz, J. R., Spiga, A., Agence Nationale de la Recherche (France), UK Space Agency, Ministerio de Ciencia, Innovación y Universidades (España), Schimmel, Martin [0000-0003-2601-4462], Stutzmann, E., Schimmel, Martin, Lognonné, P., Horleston, A., Ceylan, S., van Driel, M., Stähler, S., Banerdt, B., Calvet, M., Charalambous, C., Clinton, John F., Drilleau, M., Fayon, L., Garcia, R. F., Giardini, Domenico, Hurst, K., Jacob, A., Kawamura, T., Kenda, B., Margerin, L., Murdoch, N., Panning, M., Pike, T., Scholz, J. R., and Spiga, A.

Abstract

Seismic noise recorded at the surface of Mars has been monitored since February 2019, using the InSight seismometers. This noise can reach -200 dB. It 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 0.03-1 Hz. We use the degree of polarization 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. In the 0.3-1Hz high frequency band (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. 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 measured polarized signals may correspond to the seismic wavefield of the Mars background noise. Plain Language Summary Seismic noise at the surface of Mars was unknown until the first measurements by the seismometers from the InSight mission in January 2019. On Earth, the microseismic noise (0.05-1 Hz) is composed dominantly of surface waves generated by the numerous sources related to ocean wave activities. On Mars, because there is no ocean, seismic noise is down to 500 times lower than on Earth reaching -200 dB in acceleration at night. In order to deter

Published
2021

43. Seismic Noise Autocorrelations on Mars

Author

Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Centre National de la Recherche Scientifique (France), Schimmel, Martin [0000-0003-2601-4462], Schimmel, Martin, Stutzmann, E., Lognonné, P., Compaire, Nicolas, Davis, Paul, Drilleau, M., García, Raphael, Kim, Doyeon, Knapmeyer‐Endrun, Brigitte, Lekic, Vedran, Margerin, Ludovic, Panning, M., Schmerr, N., Scholz, J. R., Spiga, A., Tauzin, Benoit, Banerdt, B., Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Centre National de la Recherche Scientifique (France), Schimmel, Martin [0000-0003-2601-4462], Schimmel, Martin, Stutzmann, E., Lognonné, P., Compaire, Nicolas, Davis, Paul, Drilleau, M., García, Raphael, Kim, Doyeon, Knapmeyer‐Endrun, Brigitte, Lekic, Vedran, Margerin, Ludovic, Panning, M., Schmerr, N., Scholz, J. R., Spiga, A., Tauzin, Benoit, and Banerdt, B.

Abstract

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.

Published
2021

44. Seismic detection of the martian core

Author

NASA Jet Propulsion Laboratory, European Commission, Agence Nationale de la Recherche (France), Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia, Innovación y Universidades (España), UK Space Agency, Stahler, S. C., Khan, A., Banerdt, W. B., Lognonné, P., Giardini, Domenico, Ceylan, S., Drilleau, M., Duran, A. C., Garcia, R. F., Huang, Q. C., Kim, D., Lekic, Vedran, Samuel, H., Schimmel, Martin, Schmerr, N., Sollberger, D., Stutzmann, E., Xu, Z. D., Antonangeli, D., Charalambous, C., Davis, P. M., Irving, Jessica C. E., Kawamura, T., Knapmeyer, M., Maguire, R., Marusiak, A. G., Panning, M.P., Perrin , C., Plesa, A. C., Rivoldini, A., Schmelzbach, C., Zenhausern, G., Beucler, E., Clinton, John F., Dahmen, N., van Driel, M., Gudkova, T., Horleston, A., Pike, William T., Plasman, M., Smrekar, S. E., NASA Jet Propulsion Laboratory, European Commission, Agence Nationale de la Recherche (France), Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia, Innovación y Universidades (España), UK Space Agency, Stahler, S. C., Khan, A., Banerdt, W. B., Lognonné, P., Giardini, Domenico, Ceylan, S., Drilleau, M., Duran, A. C., Garcia, R. F., Huang, Q. C., Kim, D., Lekic, Vedran, Samuel, H., Schimmel, Martin, Schmerr, N., Sollberger, D., Stutzmann, E., Xu, Z. D., Antonangeli, D., Charalambous, C., Davis, P. M., Irving, Jessica C. E., Kawamura, T., Knapmeyer, M., Maguire, R., Marusiak, A. G., Panning, M.P., Perrin , C., Plesa, A. C., Rivoldini, A., Schmelzbach, C., Zenhausern, G., Beucler, E., Clinton, John F., Dahmen, N., van Driel, M., Gudkova, T., Horleston, A., Pike, William T., Plasman, M., and Smrekar, S. E.

Abstract

Clues to a planet's geologic history are contained in its interior structure, particularly its core. We detected reflections of seismic waves from the core-mantle boundary of Mars using InSight seismic data and inverted these together with geodetic data to constrain the radius of the liquid metal core to 1830 +/- 40 kilometers. The large core implies a martian mantle mineralogically similar to the terrestrial upper mantle and transition zone but differing from Earth by not having a bridgmanite-dominated lower mantle. We inferred a mean core density of 5.7 to 6.3 grams per cubic centimeter, which requires a substantial complement of light elements dissolved in the iron-nickel core. The seismic core shadow as seen from InSight's location covers half the surface of Mars, including the majority of potentially active regions-e.g., Tharsis-possibly limiting the number of detectable marsquakes.

Published
2021

45. Constraints on the shallow elastic and anelastic structure of Mars from InSight seismic data

Author

Lognonné, P.; Banerdt, W.B.; Pike, W.T.; Giardini, D.; Christensen, U.; Garcia, R.F.; Kawamura, T.; Kedar, S.; Knapmeyer-Endrun, B.; Margerin, L.; Nimmo, F.; Panning, M.; Tauzin, B.; Scholz, J.R.; Antonangeli, D.; Barkaoui, S.; Beucler, E.; Bissig, F.; Brinkman, N.; Calvet, M.; Ceylan, S.; Charalambous, C.; Davis, P.; van Driel, M.; Drilleau, M.; Fayon, L.; Joshi, R.; Kenda, B.; Khan, A.; Knapmeyer, M.; Lekic, V.; McClean, J.; Mimoun, D.; Murdoch, N.; Pan, L.; Perrin, C.; Pinot, B.; Pou, L.; Menina, S.; Rodriguez, S.; Schmelzbach, C.; Schmerr, N.; Sollberger, D.; Spiga, A.; Stähler, S.; Stott, A.; Stutzmann, E.; Tharimena, S.; Widmer-Schnidrig, R.; Schimmel, M.; Rodriguez Manfredi, J.A. and Lognonné, P.; Banerdt, W.B.; Pike, W.T.; Giardini, D.; Christensen, U.; Garcia, R.F.; Kawamura, T.; Kedar, S.; Knapmeyer-Endrun, B.; Margerin, L.; Nimmo, F.; Panning, M.; Tauzin, B.; Scholz, J.R.; Antonangeli, D.; Barkaoui, S.; Beucler, E.; Bissig, F.; Brinkman, N.; Calvet, M.; Ceylan, S.; Charalambous, C.; Davis, P.; van Driel, M.; Drilleau, M.; Fayon, L.; Joshi, R.; Kenda, B.; Khan, A.; Knapmeyer, M.; Lekic, V.; McClean, J.; Mimoun, D.; Murdoch, N.; Pan, L.; Perrin, C.; Pinot, B.; Pou, L.; Menina, S.; Rodriguez, S.; Schmelzbach, C.; Schmerr, N.; Sollberger, D.; Spiga, A.; Stähler, S.; Stott, A.; Stutzmann, E.; Tharimena, S.; Widmer-Schnidrig, R.; Schimmel, M.; Rodriguez Manfredi, J.A.

Abstract

Mars’s seismic activity and noise have been monitored since January 2019 by the seismometer of the InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) lander. At night, Mars is extremely quiet; seismic noise is about 500 times lower than Earth’s microseismic noise at periods between 4 s and 30 s. The recorded seismic noise increases during the day due to ground deformations induced by convective atmospheric vortices and ground-transferred wind-generated lander noise. Here we constrain properties of the crust beneath InSight, using signals from atmospheric vortices and from the hammering of InSight’s Heat Flow and Physical Properties (HP) instrument, as well as the three largest Marsquakes detected as of September 2019. From receiver function analysis, we infer that the uppermost 8–11 km of the crust is highly altered and/or fractured. We measure the crustal diffusivity and intrinsic attenuation using multiscattering analysis and find that seismic attenuation is about three times larger than on the Moon, which suggests that the crust contains small amounts of volatiles.

Published
2020

46. MSS/1: Single-Station and Single-Event Marsquake Inversion

Author

California Institute of Technology, National Aeronautics and Space Administration (US), National Supercomputing Center of Tianjin, Swiss National Science Foundation, NASA Jet Propulsion Laboratory, Schimmel, Martin [0000-0003-2601-4462], Drilleau, M., Beucler, E., Lognonné, P., Panning, M.P., Knapmeyer‐Endrun, Brigitte, Banerdt, W. B., Beghein, C., Ceylan, S., van Driel, M., Joshi, R., Kawamura, T., Khan, A., Menina, S., Rivoldini, A., Samuel, H., Stähler, S., Xu, H., Bonnin, Mickaël, Clinton, John F., Giardini, Domenico, Kenda, B., Lekic, Vedran, Mocquet, A., Murdoch, N., Schimmel, Martin, Smrekar, S. E., Stutzmann, E., Tauzin, B., Tharimena, S., California Institute of Technology, National Aeronautics and Space Administration (US), National Supercomputing Center of Tianjin, Swiss National Science Foundation, NASA Jet Propulsion Laboratory, Schimmel, Martin [0000-0003-2601-4462], Drilleau, M., Beucler, E., Lognonné, P., Panning, M.P., Knapmeyer‐Endrun, Brigitte, Banerdt, W. B., Beghein, C., Ceylan, S., van Driel, M., Joshi, R., Kawamura, T., Khan, A., Menina, S., Rivoldini, A., Samuel, H., Stähler, S., Xu, H., Bonnin, Mickaël, Clinton, John F., Giardini, Domenico, Kenda, B., Lekic, Vedran, Mocquet, A., Murdoch, N., Schimmel, Martin, Smrekar, S. E., Stutzmann, E., Tauzin, B., and Tharimena, S.

Abstract

SEIS, the seismometer of the InSight mission, which landed on Mars on 26 November 2018, is monitoring the seismic activity of the planet. The goal of the Mars Structure Service (MSS) is to provide, as a mission product, the first average 1-D velocity model of Mars from the recorded InSight data. Prior to the mission, methodologies have been developed and tested to allow the location of the seismic events and estimation of the radial structure, using surface waves and body waves arrival times, and receiver functions. The paper describes these validation tests and compares the performance of the different algorithms to constrain the velocity model below the InSight station and estimate the 1-D average model over the great circle path between source and receiver. These tests were performed in the frame of a blind test, during which synthetic data were inverted. In order to propagate the data uncertainties on the output model distribution, Bayesian inversion techniques are mainly used. The limitations and strengths of the methods are assessed. The results show the potential of the MSS approach to retrieve the structure of the crust and underlying mantle. However, at this time, large quakes with clear surface waves have not yet been recorded by SEIS, which makes the estimation of the 1-D average seismic velocity model challenging. Additional locatable events, especially at large epicentral distances, and development of new techniques to fully investigate the data, will ultimately provide more constraints on the crust and mantle of Mars. ©2020 The Authors.

Published
2020

47. Constraints on the shallow elastic and anelastic structure of Mars from InSight seismic data

Author

Centre National D'Etudes Spatiales (France), California Institute of Technology, NASA Astrobiology Institute (US), Swiss National Science Foundation, European Commission, Schimmel, Martin [0000-0003-2601-4462], Lognonné, P., Banerdt, W. B., Pike, William T., Giardini, Domenico, Christensen, U., Garcia, R. F., Kawamura, T., Kedar, S., Knapmeyer‐Endrun, Brigitte, Margerin, L., Nimmo, F., Daubar, I., Delage, P., Fuji, N., Golombek, M., Grott, M., Horleston, A., Hurst, K., Irving, J., Jacob, A., Knollenberg, J., Krasner, S., Krause, C., Lorenz, R., Michaut, C., Myhill, Robert, Nissen-Meyer, T., ten Pierick, J., Plesa, A. C., Quantin-Nataf, C., Robertsson, J., Rochas, L., Schimmel, Martin, Smrekar, S., Spohn, T., Teanby, N., Tromp, J., Vallade, J., Verdier, N., Vrettos, C., Weber, R., Banfield, D., Barrett, E., Bierwirth, M., Calcutt, S., Compaire, N., Johnson, C. L., Mance, D., Euchner, F., Kerjean, L., Mainsant, G., Mocquet, A., Rodriguez Manfredi, J. A., Pont, G., Laudet, P., Nebut, T., de Raucourt, S., Robert, O., Russell, C. T., Sylvestre-Baron, A., Tillier, S., Warren, T., Wieczorek, M., Yana, C., Zweifel, P., Panning, M., Tauzin, B., Scholz, J. R., Antonangeli, D., Barkaoui, S., Beucler, E., Bissig, F., Brinkman, N., Calvet, M., Ceylan, S., Charalambous, C., Davis, P., van Driel, M., Drilleau, M., Fayon, L., Joshi, R., Kenda, B., Khan, A., Knapmeyer, M., Lekic, Vedran, McClean, J., Mimoun, D., Murdoch, N., Pan, L., Perrin , C., Pinot, B, Pou, L., Menina, S., Rodríguez, S., Schmelzbach, C., Schmerr, N., Sollberger, D., Spiga, A., Stähler, S., Stott, A., Stutzmann, E., Tharimena, S., Widmer-Schnidrig, R., Andersson, F., Ansan, V., Beghein, C., Böse, M., Bozdag, E., Clinton, John F., Centre National D'Etudes Spatiales (France), California Institute of Technology, NASA Astrobiology Institute (US), Swiss National Science Foundation, European Commission, Schimmel, Martin [0000-0003-2601-4462], Lognonné, P., Banerdt, W. B., Pike, William T., Giardini, Domenico, Christensen, U., Garcia, R. F., Kawamura, T., Kedar, S., Knapmeyer‐Endrun, Brigitte, Margerin, L., Nimmo, F., Daubar, I., Delage, P., Fuji, N., Golombek, M., Grott, M., Horleston, A., Hurst, K., Irving, J., Jacob, A., Knollenberg, J., Krasner, S., Krause, C., Lorenz, R., Michaut, C., Myhill, Robert, Nissen-Meyer, T., ten Pierick, J., Plesa, A. C., Quantin-Nataf, C., Robertsson, J., Rochas, L., Schimmel, Martin, Smrekar, S., Spohn, T., Teanby, N., Tromp, J., Vallade, J., Verdier, N., Vrettos, C., Weber, R., Banfield, D., Barrett, E., Bierwirth, M., Calcutt, S., Compaire, N., Johnson, C. L., Mance, D., Euchner, F., Kerjean, L., Mainsant, G., Mocquet, A., Rodriguez Manfredi, J. A., Pont, G., Laudet, P., Nebut, T., de Raucourt, S., Robert, O., Russell, C. T., Sylvestre-Baron, A., Tillier, S., Warren, T., Wieczorek, M., Yana, C., Zweifel, P., Panning, M., Tauzin, B., Scholz, J. R., Antonangeli, D., Barkaoui, S., Beucler, E., Bissig, F., Brinkman, N., Calvet, M., Ceylan, S., Charalambous, C., Davis, P., van Driel, M., Drilleau, M., Fayon, L., Joshi, R., Kenda, B., Khan, A., Knapmeyer, M., Lekic, Vedran, McClean, J., Mimoun, D., Murdoch, N., Pan, L., Perrin , C., Pinot, B, Pou, L., Menina, S., Rodríguez, S., Schmelzbach, C., Schmerr, N., Sollberger, D., Spiga, A., Stähler, S., Stott, A., Stutzmann, E., Tharimena, S., Widmer-Schnidrig, R., Andersson, F., Ansan, V., Beghein, C., Böse, M., Bozdag, E., and Clinton, John F.

Abstract

Mars’s seismic activity and noise have been monitored since January 2019 by the seismometer of the InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) lander. At night, Mars is extremely quiet; seismic noise is about 500 times lower than Earth’s microseismic noise at periods between 4 s and 30 s. The recorded seismic noise increases during the day due to ground deformations induced by convective atmospheric vortices and ground-transferred wind-generated lander noise. Here we constrain properties of the crust beneath InSight, using signals from atmospheric vortices and from the hammering of InSight’s Heat Flow and Physical Properties (HP3) instrument, as well as the three largest Marsquakes detected as of September 2019. From receiver function analysis, we infer that the uppermost 8–11 km of the crust is highly altered and/or fractured. We measure the crustal diffusivity and intrinsic attenuation using multiscattering analysis and find that seismic attenuation is about three times larger than on the Moon, which suggests that the crust contains small amounts of volatiles.

Published
2020

48. The seismicity of Mars

Author

Swiss National Supercomputing Centre, Swiss National Science Foundation, Agence Nationale de la Recherche (France), State Secretariat for Education, Research and Innovation (Switzerland), UK Space Agency, California Institute of Technology, German Centre for Air and Space Travel, Schimmel, Martin [0000-0003-2601-4462], Giardini, Domenico, Lognonné, P., Banerdt, W. B., Pike, William T., Christensen, U., Ceylan, S., Clinton, John F., van Driel, M., Stähler, S. C., Böse, M., Garcia, R. F., Khan, A., Panning, M., Perrin, C., Banfield, D., Beucler, E., Charalambous, C., Euchner, F., Horleston, A., Jacob, A., Kawamura, T., Kedar, S., Mainsant, G., Scholz, J. R., Smrekar, S. E., Spiga, A., Agard, C., Antonangeli, D., Barkaoui, S., Barrett, E., Combes, P., Conejero, Vicente, Daubar, I., Drilleau, M., Ferrier, C., Gabsi, T., Gudkova, T., Hurst, K., Karakostas, F., King, S., Knapmeyer, M., Knapmeyer‐Endrun, Brigitte, Llorca-Cejudo, R., Lucas, A., Luno, L., Margerin, L., McClean, J. B., Mimoun, D., Murdoch, N., Nimmo, F., Nonon, M., Pardo, C., Rivoldini, A., Manfredi, J. A. R., Samuel, H., Schimmel, Martin, Stott, A. E., Stutzmann, E., Teanby, N., Warren, T., Weber, R. C., Wieczorek, M., Yana, C., Swiss National Supercomputing Centre, Swiss National Science Foundation, Agence Nationale de la Recherche (France), State Secretariat for Education, Research and Innovation (Switzerland), UK Space Agency, California Institute of Technology, German Centre for Air and Space Travel, Schimmel, Martin [0000-0003-2601-4462], Giardini, Domenico, Lognonné, P., Banerdt, W. B., Pike, William T., Christensen, U., Ceylan, S., Clinton, John F., van Driel, M., Stähler, S. C., Böse, M., Garcia, R. F., Khan, A., Panning, M., Perrin, C., Banfield, D., Beucler, E., Charalambous, C., Euchner, F., Horleston, A., Jacob, A., Kawamura, T., Kedar, S., Mainsant, G., Scholz, J. R., Smrekar, S. E., Spiga, A., Agard, C., Antonangeli, D., Barkaoui, S., Barrett, E., Combes, P., Conejero, Vicente, Daubar, I., Drilleau, M., Ferrier, C., Gabsi, T., Gudkova, T., Hurst, K., Karakostas, F., King, S., Knapmeyer, M., Knapmeyer‐Endrun, Brigitte, Llorca-Cejudo, R., Lucas, A., Luno, L., Margerin, L., McClean, J. B., Mimoun, D., Murdoch, N., Nimmo, F., Nonon, M., Pardo, C., Rivoldini, A., Manfredi, J. A. R., Samuel, H., Schimmel, Martin, Stott, A. E., Stutzmann, E., Teanby, N., Warren, T., Weber, R. C., Wieczorek, M., and Yana, C.

Abstract

The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed in Elysium Planitia on Mars on 26 November 2018 and fully deployed its seismometer by the end of February 2019. The mission aims to detect, characterize and locate seismic activity on Mars, and to further constrain the internal structure, composition and dynamics of the planet. Here, we present seismometer data recorded until 30 September 2019, which reveal that Mars is seismically active. We identify 174 marsquakes, comprising two distinct populations: 150 small-magnitude, high-frequency events with waves propagating at crustal depths and 24 low-frequency, subcrustal events of magnitude Mw 3–4 with waves propagating at various depths in the mantle. These marsquakes have spectral characteristics similar to the seismicity observed on the Earth and Moon. We determine that two of the largest detected marsquakes were located near the Cerberus Fossae fracture system. From the recorded seismicity, we constrain attenuation in the crust and mantle, and find indications of a potential low-S-wave-velocity layer in the upper mantle. © 2020, The Author(s), under exclusive licence to Springer Nature Limited.

Published
2020

49. The Mars Structure Service for InSight:Single-Station Marsquake Inversions for Structure

Author

Drilleau, M., Lognonné, P., Panning, Mark P., Beucler, E., Khan, A., van Driel, M., Beghein, Caroline, Staehler, Simon C., Knapmeyer‐Endrun, Brigitte, Ceylan, S., Barkaoui, Salma, Clinton, John F., Giardini, Domenico, Joshi, R., Kenda, B., Lekic, Vedran, Menina, Sabrina, Murdoch, N., Rivoldini, A., Samuel, H., Schimmel, Martin, Smrekar, Suzanne, Stutzmann, Martin, Tauzin, Benoit, Tharimena, S., and Xu, Haotian

Abstract

AGU Fall Meeting in San Francisco, 9-13 December 2019, The SEIS seismometer package was successfully deployed on Mars by February 2019. Routine operations are split into two services: the Mars Structure Service (MSS) and the Marsquake Service (MQS), which are responsible for defining interior structure models and seismicity catalogs, respectively. Initial model delivery from MSS is based on a limited dataset of two Marsquakes with a clear P and S arrivals. Different inversion algorithms were developed by the MSS team in order to retrieve the first 1D averaged model of Mars. Two complementary approaches are considered. One set of models (called M1) is parameterized in seismic velocity and density as a function of depth. A second set of models (called M2) is obtained by parameterizing with geodynamical constraints like temperature and composition. We use Bayesian inversion techniques to obtain robust probability density functions of seismic velocity profiles. Different types of data are considered for these inversions including body waves, surface waves and receiver functions. To characterize what we could learn about Mars¿ interior structure with only one station and with the first seismic event, we performed inversions of synthetic data following a blind test process, where the interior model and the Marsquake parameters (location, depth, origin time, and moment tensor) were unknown to all team members carrying out data analysis and inversion. In this presentation we will discuss the results of this blind test in terms of structure and compare different methods developed by the MSS. We will then show results from investigations of the first, real seismic data due to quakes on Mars recorded by SEIS in terms of the structure and quake locations. We will especially focus our investigation on joint inversions made not only with the arrival time, but also with secondary seismic data extracted from the detected events, including apparent attenuation rate and with receiver functions. Of course, much more detailed analysis will be made if Mars seismicity provide us in the near future larger quakes with body wave phases and first orbit surface wave dispersion, and/or one event large enough to record multiple orbit surface waves, and will augment future interiors models of Mars.

Published
2019

50. Unsupervised representation learning for clustering SEIS data in continuous records with deep scattering network

Author

Barkaoui, Salma, Lognonné, P., Dehoop, Maarten, Drilleau, M., Kawamura, T., Stutzmann, E., van Driel, M., Kenda, B., Sainton, G., Seydoux, Leonard, Clinton, John F., Schimmel, Martin, and Murdoch, N.

Abstract

AGU Fall Meeting 2019 in San Francisco, 9-13 December 2019, Exploring the internal structure and the dynamics of our solar system is mandatory to understand the behavior of our universe and its origin. One of the tools chosen by NASA is seismology particularly in order to constrain the parameters of the deep interior structure of the red planet via the Insight (Interior Exploration using Seismic Investigations, Geodesy, and Heat Transport) mission. InSight was successfully landed on November 26th, 2018 in Elysium Planitia with geophysical instruments a short-period seismometer and a broadband seismometer (SEIS, Seismic Experiment for Interior Structure). Both seismometers are now installed directly on Mars surface and enable to analyze the continuous seismic signal.But, before making the structure inversion, we need to extract the features from SEIS data. However, those features may nevertheless be hidden into noise, or may escape from analysis due to the limitations imposed by the current methodologies.Therefore, the aim of this study is to overcome this problem by well extracting, recognizing and classifying the instrument signals using Machine Learning and Deep Learning new strategies inspired from the Deep scattering network.This is very promising for the SIES data as, we¿re going to be able not only to detect the familiar signals, but the exciting part is the unseen or the unknown ones. This technique is used to clean the data from the glitches. In fact, this tool has recently proved to be powerful in signal processing, data automatic feature extraction and may even be helpful to detect new types of signals. Those new signals can reveal unknown processes and lead to new discoveries about Mars physical processes.The method used in this study is divided into three fundamental steps. The first one, to make an automatic feature extraction using the Deep scattering transform which is a convolution neural network that computes a cascade of wavelets calculations and filtering operations to get a stable waveform representation stable to local deformations and overlapping at multiple times and frequencies.. The second step is to use those features for signal classification using Machine Learning classifier Gaussian Mixture Network. Finally, we update the wavelet mother bank depending on the results of the classification error minimization using Adam stochastic gradient descent.

Published
2019

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