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1. The InSight HP$^3$ Penetrator (Mole) on Mars: Soil Properties Derived From the Penetration Attempts and Related Activities

Author

Spohn, T., Hudson, T. L., Marteau, E., Golombek, M., Grott, M., Wippermann, T., Ali, K. S., Schmelzbach, C., Kedar, S., Hurst, K., Trebi-Ollennu, A., Ansan, V., Garvin, J., Knollenberg, J., Mueller, N., Piqeux, S., Lichtenheldt, R., Krause, C., Fantinati, C., Brinkman, N., Sollberger, D., Delage, P., Vrettos, C., Reershemius, S., Wisniewski, L., Grygorczuk, J., Robertsson, J., Edme, P., Andersson, F., Kroemer, O., Lognonne, P., Giardini, D., Smrekar, S. E., and Banerdt, W. B.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Physics - Geophysics
Abstract

The NASA InSight Lander on Mars includes the Heat Flow and Physical Properties Package HP$^3$ to measure the surface heat flow of the planet. The package uses temperature sensors that would have been brought to the target depth of 3--5 m by a small penetrator, nicknamed the mole. The mole requiring friction on its hull to balance remaining recoil from its hammer mechanism did not penetrate to the targeted depth. Instead, by precessing about a point midway along its hull, it carved a 7 cm deep and 5-6 cm wide pit and reached a depth of initially 31 cm. The root cause of the failure - as was determined through an extensive, almost two years long campaign - was a lack of friction in an unexpectedly thick cohesive duricrust. During the campaign -- described in detail in this paper -- the mole penetrated further aided by friction applied using the scoop at the end of the robotic Instrument Deployment Arm and by direct support by the latter. The mole finally reached a depth of 40 cm, bringing the mole body 1--2 cm below the surface. The penetration record of the mole and its thermal sensors were used to measure thermal and mechanical soil parameters such as the thermal conductivity and the penetration resistance of the duricrust and its cohesion. The hammerings of the mole were recorded by the seismometer SEIS and the signals could be used to derive a P-wave velocity and a S-wave velocity and elastic moduli representative of the topmost tens of cm of the regolith. The combined data were used to derive a model of the regolith that has an about 20 cm thick duricrust underneath a 1 cm thick unconsolidated layer of sand mixed with dust and above another 10 cm of unconsolidated sand. Underneath the latter, a layer more resistant to penetration and possibly consisting of debris from a small impact crater is inferred., Comment: 78 pages 22 figures, , submitted to Space Science Reviews

Published
2021
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2. The InSight HP3 Penetrator (Mole) on Mars: Soil Properties Derived from the Penetration Attempts and Related Activities

Author

Spohn, T., Hudson, T. L., Marteau, E., Golombek, M., Grott, M., Wippermann, T., Ali, K. S., Schmelzbach, C., Kedar, S., Hurst, K., Trebi-Ollennu, A., Ansan, V., Garvin, J., Knollenberg, J., Müller, N., Piqueux, S., Lichtenheldt, R., Krause, C., Fantinati, C., Brinkman, N., Sollberger, D., Delage, P., Vrettos, C., Reershemius, S., Wisniewski, L., Grygorczuk, J., Robertsson, J., Edme, P., Andersson, F., Krömer, O., Lognonné, P., Giardini, D., Smrekar, S. E., and Banerdt, W. B.

Published
2022
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3. Mars Soil Temperature and Thermal Properties From InSight HP3 ${\mathrm{H}\mathrm{P}}^{3}$ Data.

Author

Spohn, T., Müller, N., Knollenberg, J., Grott, M., Golombek, M. P., Plesa, A.‐C., Bickel, V. T., Morgan, P., Krause, C., Breuer, D., Smrekar, S. E., and Banerdt, W. B.

Subjects
CHEMICAL processes, SOIL temperature, THERMAL conductivity, THERMAL properties, SURFACE temperature, THERMAL diffusivity
Abstract

Diurnal and seasonal variations in soil and surface temperature measured with the HP3 ${\mathrm{H}\mathrm{P}}^{3}$ thermal probe and radiometer of NASA's InSight Mars mission are reported. At a representative depth of 10–20 cm, an average temperature of 217.5 K was found, varying by 5.3–6.7 K during a sol and by 13.3 K during the seasons. From the damping of the temperature variation with depth and the phase shift, a thermal diffusivity of (3.93 ± $\pm $ 0.39) × 10−8 ${10}^{-8}$m2 ${\mathrm{m}}^{2}$/s was derived for the upper ∼ ${\sim} $10 cm from the diurnal temperature variation and of (3.63 ± $\pm $ 0.53) × 10−8 ${10}^{-8}$m2 ${\mathrm{m}}^{2}$/s for the ∼ ${\sim} $40 cm depth range of the mole from the annual temperature variation. Using published thermal conductivity and inertia values together with the diffusivities, soil densities of 1,470 and 1,730 kg/m3 ${m}^{3}$ were derived for these depths. The temperatures allow the deliquescence of thin films of brine, the efflorescence of which may explain the cemented duricrust observed. Plain Language Summary: Temperature is an important factor in understanding the physical properties of Martian soil. It determines how quickly physical processes and chemical reactions occur, including the transport of heat and materials. Temperature is crucial to astrobiology because it affects the habitability of the soil and the potential for water or brine to support microbial life. We measured the temperature in the soil during several Martian days and over a Martian year using the NASA InSight Mars mission's Heat Flow and Physical Properties Package. The average temperature was −56°C (217.5 K) over the depth extent of the thermal probe, which was about 40 cm. The temperature varied by 5–7° during the day, which is only a tenth of the daily surface temperature variation. It varied by 13° during the seasons. The temperature is subfreezing for water, but it allows the formation of thin films of salty brine for 10 hr or more during a Martian day. The solidification of the brine is a likely explanation for the observed few tens of centimeters thick duricrust, a layer of consolidated, cohesive sand, which is thought to have hampered the penetration to greater depth of the mission's thermal probe. Key Points: We measured the temperature and its diurnal and annual variations in the top 40 cm of the Martian soil at the InSight landing siteThe soil thermal diffusivity was calculated from the diurnal and seasonal surface and soil temperature variationsThe soil temperature allows the formation of thin films of brine; their efflorescence may explain the formation of the observed duricrust [ABSTRACT FROM AUTHOR]

Published
2024
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4. 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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5. 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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6. Geology of the InSight landing site on Mars

Author

Golombek, M., Warner, N. H., Grant, J. A., Hauber, E., Ansan, V., Weitz, C. M., Williams, N., Charalambous, C., Wilson, S. A., DeMott, A., Kopp, M., Lethcoe-Wilson, H., Berger, L., Hausmann, R., Marteau, E., Vrettos, C., Trussell, A., Folkner, W., Le Maistre, S., Mueller, N., Grott, M., Spohn, T., Piqueux, S., Millour, E., Forget, F., Daubar, I., Murdoch, N., Lognonné, P., Perrin, C., Rodriguez, S., Pike, W. T., Parker, T., Maki, J., Abarca, H., Deen, R., Hall, J., Andres, P., Ruoff, N., Calef, F., Smrekar, S., Baker, M. M., Banks, M., Spiga, A., Banfield, D., Garvin, J., Newman, C. E., and Banerdt, W. B.

Published
2020
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7. Results From Insight’s First Full Martian Year

Author

Wieczorek, M, Weber, R, Warner, N, Tromp, J, Teanby, N, Stanley, S, Stahler, S, Spohn, T, Spiga, A, Siegler, M, Schmerr, N, Rodriguez-Manfredi, P.J.A, Plesa, A.-C, Pike, W.T, Nimmo, Francis, Newman, C, Nagihara, S, Müller, N, Morgan, P, Mittelholz, A, Mimoun, D, Michaut, C, McLennan, S, Margerin, L, Maki, J, Lorenz, R, Lognonné, P, Lemmon, M, Knapmeyer-Endrun, B, King, S, Khan, A, Kedar, S, Kawamura, Taichi, Kargl, G, Joshi, R, Johnson, C, Irving, J, Hudson, T, Grygorczuk, J, Grott, M, Grant, J, Golombek, M, Giardini, D, Garvin, J, Garcia, R, Folkner, W, Fillingim, M, Dehant, V, Daubar, I, Collins, G, Clinton, J, Christensen, U, Chi, P, Ceylan, S, Brinkman, N, Bozdag, Ebru, Bowles, Neil, Bissig, F, Beucler, E, Beghein, C, Banfield, D, Asmar, S, Antonangeli, D, Smrekar, S, Banerdt, W. B, and Panning, M.P

Published
2021

8. Results From Insight’s First Full Martian Year

Author

Panning, M.P, Banerdt, W. B, Smrekar, S, Antonangeli, D, Asmar, S, Banfield, D, Beghein, C, Beucler, E, Bissig, F, Bowles, Neil, Bozdag, Ebru, Brinkman, N, Ceylan, S, Chi, P, Christensen, U, Clinton, J, Collins, G, Daubar, I, Dehant, V, Fillingim, M, Folkner, W, Garcia, R, Garvin, J, Giardini, D, Golombek, M, Grant, J, Grott, M, Grygorczuk, J, Hudson, T, Irving, J, Johnson, C, Joshi, R, Kargl, G, Kawamura, Taichi, Kedar, S, Khan, A, King, S, Knapmeyer-Endrun, B, Lemmon, M, Lognonné, P, Lorenz, R, Maki, J, Margerin, L, McLennan, S, Michaut, C, Mimoun, D, Mittelholz, A, Morgan, P, Müller, N, Nagihara, S, Newman, C, Nimmo, Francis, Pike, W.T, Plesa, A.-C, Rodriguez-Manfredi, P.J.A, Schmerr, N, Siegler, M, Spiga, A, Spohn, T, Stahler, S, Stanley, S, Teanby, N, Tromp, J, Warner, N, Weber, R, and Wieczorek, M

Published
2021

9. InSight and SEIS on Mars: First results after 200 sols

Author

Weber, Renee, Lognonné, P, Banerdt, W. B, Smrekar, S, Banfield, D, Russel, C, Folkner, B, Maki, J, Pike, W. T, Giardini, D, and Christensen, U

Subjects
Lunar And Planetary Science And Exploration
Published
2020

11. Seasonal Variations of Soil Thermal Conductivity at the InSight Landing Site

Author

Grott, M., primary, Piqueux, S., additional, Spohn, T., additional, Knollenberg, J., additional, Krause, C., additional, Marteau, E., additional, Hudson, T. L., additional, Forget, F., additional, Lange, L., additional, Müller, N., additional, Golombek, M., additional, Nagihara, S., additional, Morgan, P., additional, Murphy, J. P., additional, Siegler, M., additional, King, S. D., additional, Banfield, D., additional, Smrekar, S. E., additional, and Banerdt, W. B., additional

Published
2023
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12. Seasonal Variations of Soil Thermal Conductivity at the InSight Landing Site

Author

Grott, M., Piqueux, S., Spohn, T., Knollenberg, J., Krause, C., Marteau, E., Hudson, T. L., Forget, F., Lange, L., Mueller, N., Golombek, M., Nagihara, S., Morgan, P., Murphy, J. P., Siegler, M., King, Scott D., Banfield, D., Smrekar, S. E., Banerdt, W. B., Grott, M., Piqueux, S., Spohn, T., Knollenberg, J., Krause, C., Marteau, E., Hudson, T. L., Forget, F., Lange, L., Mueller, N., Golombek, M., Nagihara, S., Morgan, P., Murphy, J. P., Siegler, M., King, Scott D., Banfield, D., Smrekar, S. E., and Banerdt, W. B.

Abstract

The heat flow and physical properties package measured soil thermal conductivity at the landing site in the 0.03-0.37 m depth range. Six measurements spanning solar longitudes from 8.0 degrees to 210.0 degrees were made and atmospheric pressure at the site was simultaneously measured using InSight's Pressure Sensor. We find that soil thermal conductivity strongly correlates with atmospheric pressure. This trend is compatible with predictions of the pressure dependence of thermal conductivity for unconsolidated soils under martian atmospheric conditions, indicating that heat transport through the pore filling gas is a major contributor to the total heat transport. Therefore, any cementation or induration of the soil sampled by the experiments must be minimal and soil surrounding the mole at depths below the duricrust is likely unconsolidated. Thermal conductivity data presented here are the first direct evidence that the atmosphere interacts with the top most meter of material on Mars.

Published
2023

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

Author

Lognonné, P., Banerdt, W. B., Giardini, D., Pike, W. T., Christensen, U., Laudet, P., de Raucourt, S., Zweifel, P., Calcutt, S., Bierwirth, M., Hurst, K. J., Ijpelaan, F., Umland, J. W., Llorca-Cejudo, R., Larson, S. A., Garcia, R. F., Kedar, S., Knapmeyer-Endrun, B., Mimoun, D., Mocquet, A., Panning, M. P., Weber, R. C., Sylvestre-Baron, A., Pont, G., Verdier, N., Kerjean, L., Facto, L. J., Gharakanian, V., Feldman, J. E., Hoffman, T. L., Klein, D. B., Klein, K., Onufer, N. P., Paredes-Garcia, J., Petkov, M. P., Willis, J. R., Smrekar, S. E., Drilleau, M., Gabsi, T., Nebut, T., Robert, O., Tillier, S., Moreau, C., Parise, M., Aveni, G., Ben Charef, S., Bennour, Y., Camus, T., Dandonneau, P. A., Desfoux, C., Lecomte, B., Pot, O., Revuz, P., Mance, D., tenPierick, J., Bowles, N. E., Charalambous, C., Delahunty, A. K., Hurley, J., Irshad, R., Liu, Huafeng, Mukherjee, A. G., Standley, I. M., Stott, A. E., 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, J. M., 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, J. M., Nonon, M., Pahn, Y., Paillet, A., Pasquier, P., Perez, G., Perez, R., Perrin, L., Pouilloux, B., Rosak, A., Savin de Larclause, I., Sicre, J., Sodki, M., Toulemont, N., Vella, B., Yana, C., Alibay, F., Avalos, O. M., Balzer, M. A., Bhandari, P., Blanco, E., Bone, B. D., Bousman, J. C., Bruneau, P., Calef, F. J., Calvet, R. J., D’Agostino, S. A., de los Santos, G., Deen, R. G., Denise, R. W., Ervin, J., Ferraro, N. W., Gengl, H. E., Grinblat, F., Hernandez, D., Hetzel, M., Johnson, M. E., Khachikyan, L., Lin, J. Y., Madzunkov, S. M., Marshall, S. L., Mikellides, I. G., Miller, E. A., Raff, W., Singer, J. E., Sunday, C. M., Villalvazo, J. F., Wallace, M. C., Banfield, D., Rodriguez-Manfredi, J. A., Russell, C. T., Trebi-Ollennu, A., Maki, J. N., Beucler, E., Böse, M., Bonjour, C., Berenguer, J. L., Ceylan, S., Clinton, J., Conejero, V., Daubar, I., Dehant, V., Delage, P., Euchner, F., Estève, I., Fayon, L., Ferraioli, L., Johnson, C. L., Gagnepain-Beyneix, J., Golombek, M., Khan, A., Kawamura, T., Kenda, B., Labrot, P., Murdoch, N., Pardo, C., Perrin, C., Pou, L., Sauron, A., Savoie, D., Stähler, S., Stutzmann, E., Teanby, N. A., Tromp, J., van Driel, M., Wieczorek, M., Widmer-Schnidrig, R., and Wookey, J.

Published
2019
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14. InSight Auxiliary Payload Sensor Suite (APSS)

Author

Banfield, D., Rodriguez-Manfredi, J. A., Russell, C. T., Rowe, K. M., Leneman, D., Lai, H. R., Cruce, P. R., Means, J. D., Johnson, C. L., Mittelholz, A., Joy, S. P., Chi, P. J., Mikellides, I. G., Carpenter, S., Navarro, S., Sebastian, E., Gomez-Elvira, J., Torres, J., Mora, L., Peinado, V., Lepinette, A., The TWINS Team, Hurst, K., Lognonné, P., Smrekar, S. E., and Banerdt, W. B.

Published
2018
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15. Thermal and mechanical properties of the Martian soil from InSight HP3 data

Author

Spohn, T., Grott, M., Mueller, N., Hudson, T., Marteau, E., Piqueux, S., Golombek, M., and Smrekar, S.

Abstract

The NASA InSight Lander on Mars includes the Heat Flow and Physical Properties Package HP3[1] toin-situmeasure the surface heat flow. Temperature sensors were to be installed at a target depth of 3–5m by a small penetrator, nicknamed the mole. A radiometer to measure the surface temperature complements the package. The mole, requiring friction on its hull to balance remaining recoil from its hammer mechanism, did not penetrate to the targeted depth. Instead, it reached a depth of 40cm, bringing the mole back-end 2–3cm below the surface. Lessons learned from the penetration failure have been discussed by [2]. The root cause of the failure - as was determined through an almost two years long campaign - was a lack of friction in an unexpectedly thick cohesive near-surface duricrust. The mole was used as a penetrometer and a thermal probe [3,4] instead and the hammering signals were recorded by the InSight seismometer [5]. Accordingly, the soil is highly porous and layered with a density of 1200kg/m3, thermal conductivity of 39mW/m K, cohesion between 4 and 25kPa, and s and p wave velocities of around 115 and 60m/s, respectively.The thermal conductivity varies with the season and the atmospheric pressure by +/-5% showing that gas in the pores contributes significantly to the heat transport.[1]Spohn et al. (2018) doi:10.1007/s11214-018-0531-4 [2]Spohn et al. (2022) doi:10.1016/j.asr.2022.02.009[3] Spohn et al. (2022) doi:10.1007/s11214-022-00941-z[4] Grott et al. (2021) doi:10.1029/2019EA000670[5] Brinkmann et al.(2022) doi:10.1029/2022JE007229, The 28th IUGG General Assembly (IUGG2023) (Berlin 2023)

Published
2023
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16. Finding Marsquakes: InSight's Marsquake Service and the Mars Seismic Catalogue

Author

Horleston, A., Clinton, J., Ceylan, S., Kawamura, T., Stähler, S., Charalambous, C., Dahmen, N., Duran, C. A., Kim, D., Plasman, M., Zenhäusern, Geraldine, Euchner, F., Knapmeyer, Martin, Giardini, D., Lognonne, A.P., Pike, W.T., Panning, M., Smrekar, S., and Banerdt, B.

Subjects
Mars InSight Marsquake Service
Published
2023

17. Insight and SEIS on Mars: First Results After 200 Sols

Author

Weber, Renee, Lognonné, P, Banerdt, W. B, Smrekar, S, Banfield, D, Russel, C, Folkner, B, Maki, J, Pike, W. T, Giardini, D, and Christensen, U

Subjects
Lunar And Planetary Science And Exploration
Abstract

Slightly less than 50 years after the deployment of Apollo 11 seismometer, and slightly more than 41 years after the operational end of the combined Apollo seismic network, seismology is back to operations in planetary science. InSight, or Interior Exploration using Seismic Investigations, Geodesy and Heat Transport, is a mission dedicated to understand the formation and evolution of terrestrial planets through the investigation of the interior structure and processes of Mars. This presentation will outline early mission results, focusing primarily on SEIS, the Seismic Experiment for Interior Structure.

Published
2019

20. Selection of the InSight Landing Site

Author

Golombek, M., Kipp, D., Warner, N., Daubar, I. J., Fergason, R., Kirk, R. L., Beyer, R., Huertas, A., Piqueux, S., Putzig, N. E., Campbell, B. A., Morgan, G. A., Charalambous, C., Pike, W. T., Gwinner, K., Calef, F., Kass, D., Mischna, M., Ashley, J., Bloom, C., Wigton, N., Hare, T., Schwartz, C., Gengl, H., Redmond, L., Trautman, M., Sweeney, J., Grima, C., Smith, I. B., Sklyanskiy, E., Lisano, M., Benardini, J., Smrekar, S., Lognonné, P., and Banerdt, W. B.

Published
2016
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23. Geology and Physical Properties Investigations by the InSight Lander

Author

Golombek, M., Grott, M., Kargl, G., Andrade, J., Marshall, J., Warner, N., Teanby, N. A., Ansan, V., Hauber, E., Voigt, J., Lichtenheldt, R., Knapmeyer-Endrun, B., Daubar, I. J., Kipp, D., Muller, N., Lognonné, P., Schmelzbach, C., Banfield, D., Trebi-Ollennu, A., Maki, J., Kedar, S., Mimoun, D., Murdoch, N., Piqueux, S., Delage, P., Pike, W. T., Charalambous, C., Lorenz, R., Fayon, L., Lucas, A., Rodriguez, S., Morgan, P., Spiga, A., Panning, M., Spohn, T., Smrekar, S., Gudkova, T., Garcia, R., Giardini, D., Christensen, U., Nicollier, T., Sollberger, D., Robertsson, J., Ali, K., Kenda, B., and Banerdt, W. B.

Published
2018
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25. The seismicity on Mars as recorded by InSight Marsquake Service

Author

Kawamura, T., Clinton, J., Horleston, A., Ceylan, S., Stähler, S., Plasman, M., Dahmen, N., Zenhäusern, Geraldine, Duran, C., Euchner, F, Kim, D., Charalambous, C., Knapmeyer, Martin, Giardini, D., Lognonne, P., Pike, W.T., Panning, M., Smrekar, S., and Banerdt, William B.

Subjects
Mars seismische Aktivität
Published
2022

26. 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

27. The Seismicity of Mars as Recorded by InSight Marsquake Service after 1100 Sols

Author

Kawamura, T., Clinton, J., Horleston, A., Ceylan, S., Stähler, S., Plasman, M., Dahmen, N., Zenhäusern, Geraldine, Duran, C., Euchner, F, Kim, D., Charalambous, C., Knapmeyer, Martin, Giardini, D., Lognonne, P., Pike, W.T., Panning, M., Smrekar, S., and Banerdt, William B.

Subjects
Mars InSight seismische Aktivität
Published
2022

30. The InSight HP$^3$ Penetrator (Mole) on Mars: Soil Properties Derived From the Penetration Attempts and Related Activities

Author

Spohn, Tilman, Hudson, T.L., Marteau, E., Golombek, M., Grott, Matthias, Wippermann, Torben, Ali, K., Schmelzbach, C., Kedar, S., Hurst, K., Trebi-Ollennu, A., Ansan, V., Garvin, J., Knollenberg, Jörg, Müller, Nils, Piqueux, S., Lichtenheldt, Roy, Krause, Christian, Fantinati, C., Brinkman, Nienke, Sollberger, D., Delage, P., Vrettos, C., Reershemius, Siebo, Wisniewski, Lukasz, Grygorczuk, J., Robertsson, J., Edme, P., Andersson, F., Krömer, Olaf, Lognonne, A.P., Giardini, D., Smrekar, S., and Banerdt, B.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics - Geophysics, InSight Mars Heat Flow Geophysics Soil Mechanics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Geophysics (physics.geo-ph), Astrophysics - Earth and Planetary Astrophysics
Abstract

The NASA InSight Lander on Mars includes the Heat Flow and Physical Properties Package HP$^3$ to measure the surface heat flow of the planet. The package uses temperature sensors that would have been brought to the target depth of 3--5 m by a small penetrator, nicknamed the mole. The mole requiring friction on its hull to balance remaining recoil from its hammer mechanism did not penetrate to the targeted depth. Instead, by precessing about a point midway along its hull, it carved a 7 cm deep and 5-6 cm wide pit and reached a depth of initially 31 cm. The root cause of the failure - as was determined through an extensive, almost two years long campaign - was a lack of friction in an unexpectedly thick cohesive duricrust. During the campaign -- described in detail in this paper -- the mole penetrated further aided by friction applied using the scoop at the end of the robotic Instrument Deployment Arm and by direct support by the latter. The mole finally reached a depth of 40 cm, bringing the mole body 1--2 cm below the surface. The penetration record of the mole and its thermal sensors were used to measure thermal and mechanical soil parameters such as the thermal conductivity and the penetration resistance of the duricrust and its cohesion. The hammerings of the mole were recorded by the seismometer SEIS and the signals could be used to derive a P-wave velocity and a S-wave velocity and elastic moduli representative of the topmost tens of cm of the regolith. The combined data were used to derive a model of the regolith that has an about 20 cm thick duricrust underneath a 1 cm thick unconsolidated layer of sand mixed with dust and above another 10 cm of unconsolidated sand. Underneath the latter, a layer more resistant to penetration and possibly consisting of debris from a small impact crater is inferred., 78 pages 22 figures, , submitted to Space Science Reviews

Published
2021

31. The Seismicity on Mars as recorded by InSight's Marsquake Service

Author

Ceylan, S., Horleston, A., Clinton, J., Giardini, D., Kawamura, T., Stähler, S., Banerdt, B., Charalambous, C., Dahmen, N., Duran, C. A., Euchner, F, Knapmeyer, Martin, Lognonne, A.P., Panning, M.P., Pike, W.T., Plasman, M., Smrekar, S., and Zenhäusern, Geraldine

Subjects
Mars, Marsbeben, InSight
Published
2021

32. Space Weather Observations With InSight

Author

Mittelholz, A., primary, Johnson, C. L., additional, Fillingim, M., additional, Joy, S. P., additional, Espley, J., additional, Halekas, J., additional, Smrekar, S., additional, and Banerdt, W. B., additional

Published
2021
Full Text
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35. 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

36. Global Character of the Martian Crust as Revealed by InSight Seismic Data

Author

Wieczorek, M., Knapmeyer-Endrun, B., Panning, M., Plesa, Ana-Catalina, McLennan, S M, Nimmo, F., Gyalay, S, Michaut, C., Broquet, A., Samuel, H., Rivoldini, A., Smrekar, S., Banerdt, B., and InSight, Science Team

Subjects
Crustal thickness, Crustal density, Mars, InSight
Published
2021

37. Near Surface Properties of Martian Regolith Derived From InSight HP3‐RAD Temperature Observations During Phobos Transits

Author

Mueller, N., primary, Piqueux, S., additional, Lemmon, M., additional, Maki, J., additional, Lorenz, R. D., additional, Grott, M., additional, Spohn, T., additional, Smrekar, S. E., additional, Knollenberg, J., additional, Hudson, T. L., additional, Krause, C., additional, Millour, E., additional, Forget, F., additional, Golombek, M., additional, Hagermann, A., additional, Attree, N., additional, Siegler, M., additional, and Banerdt, W. B., additional

Published
2021
Full Text
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39. Thermal Conductivity of the Martian Soil at the InSight Landing Site From HP3 Active Heating Experiments

Author

Grott, M., primary, Spohn, T., additional, Knollenberg, J., additional, Krause, C., additional, Hudson, T. L., additional, Piqueux, S., additional, Müller, N., additional, Golombek, M., additional, Vrettos, C., additional, Marteau, E., additional, Nagihara, S., additional, Morgan, P., additional, Murphy, J. P., additional, Siegler, M., additional, King, S. D., additional, Smrekar, S. E., additional, and Banerdt, W. B., additional

Published
2021
Full Text
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40. Relationships Among Regolith Thermal Conductivities and Seismic Velocities: Application to InSight Studies

Author

Morgan, P., Grott, Matthias, Schmelzbach, C., Golombek, M., Siegler, M.A., Delage, P., Müller, Nils, and Smrekar, S.

Subjects
Planetenphysik, Mars InSight Regolith Geophysics
Abstract

Studies of the thermal and seismic properties of planetary regoliths are complex because of uncertainties and variability in composition, particle and pore geometrical shape, size distribution, and three-dimensional physical connectivity. Therefore, correlations among physical properties that relate to geophysical parameters that may be measured directly or indirectly are potentially useful for studying regoliths. Studies of relationships among seismic velocities and thermal conductivities of terrestrial rocks and minerals indicate general positive correlations, often with non-Gaussian scatters in the correlations that may result in part from heterogeneity in samples used for thermal conductivity determinations. Plots of laboratory data for seismic velocities versus thermal conductivity under ambient conditions for minerals and rocks are shown in Figs. 1 and 2, respectively. These data indicate linear relationships within the limitations of the data chosen. In this contribution we have compiled and collated thermal and seismic velocity data relevant to the Mars regolith and present a preliminary relationship for the regolith at the InSight landing site.

Published
2021

41. Results from InSight's First Full Martian Year

Author

Panning M., Banerdt B., Smrekar S., Antonangeli D., Dehant, Véronique, and UCL - SST/ELI/ELIC - Earth & Climate

Abstract

The InSight mission landed on Mars in November of 2018 and completed installation of a seismometer (SEIS) on the surface about two months later [1]. In addition to SEIS, InSight carries a diverse geophysical observatory including a heat flow and physical properties package (HP3 ), a geodesy (planetary rotation dynamics) experiment (RISE) and a suite of environmental sensors measuring the magnetic field and atmospheric temperature, pressure and wind (APSS). For approximately 2 years, SEIS has been providing near-continuous seismic monitoring of Mars, with background noise levels orders of magnitude lower than that achievable on the Earth. Since the first detection of a marsquake in April of 2018, the SEIS team has identified more than 450 events that appear to be of tectonic origin. We present a summary of observations and results from the SEIS instrument as well as a summary of other geophysical observations made by InSight during the past 2 years.

Published
2021

42. Results from InSight's First Full Martian Year

Author

Panning, M., Banerdt, B., Smrekar, S., Antonangeli, D., Asmar, Sami, Banfield, D., Beghein, C., Beucler, E., Bowles, Neil, Bozdag, E., Ceylan, S., Chi, P. J., Christensen, U., Clinton, J., Collins, G., Daubar, I., Dehant, V, Fillingim, Matthew, Folkner, W., Garcia, R., Garvin, J., Giardini, D., Golombek, M., Grant, J.A., Grott, Matthias, Grygorczuk, J., Hudson, T.L., Irving, J., Johnson, C. L., Kargl, G., Kawamura, T., Kedar, S., King, S., Knapmeyer, Martin, Knapmeyer-Endrun, B., Lemmon, M., Lognonne, P., Lorenz, R., Maki, J., Margerin, L., McLennan, S M, Michaut, C., Mimoun, D., Morgan, P., Müller, Nils, Nagihara, S., Newman, C., Nimmo, F., Pike, T., Plesa, Ana-Catalina, Rodriguez-Manfredi, J. -A., Schmerr, N., Siegler, M.A., Spiga, A., Spohn, Tilman, Stanley, S., Teanby, N., Tromp, J., Warner, N., Weber, R., Wieczorek, M., and Insight, Science Team

Subjects
Mars, InSight
Published
2021

44. 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

45. Thermal Conductivity of the Martian Regolith at the InSight Landing Site from HP3 Active Heating Experiments

Author

Grott, Matthias, Spohn, Tilman, Knollenberg, Jörg, Krause, Christian, Nagihara, S., Morgan, P., Piqueux, S., Müller, Nils, Golombek, M., Murphy, J., Siegler, M.A., King, S.D., Vrettos, C., Hudson, T.L., Smrekar, S., and Banerdt, B.

Subjects
Planetenphysik, InSight Heat Flow Mars Geophysics, Institut für Planetenforschung, Nutzerzentrum für Weltraumexperimente (MUSC)
Abstract

The InSight Mars mission landed in Homestead hollow in the Elysium Planitia region of Mars at 4.50°N, 135.62°E on Nov. 3rd, 2018. The Heat Flow and Physical Properties Package (HP3) is part of the InSight payload and is designed to emplace sensors into the martian regolith to measure regolith thermal conductivity and the geothermal gradient in the 0-5 m depth range [2]. Due to unexpected soil properties, the lander’s robotic arm needed to assist in probe emplacement. We estimate the mole’s back-cap to be 2-3 cm below the surface during the measurement, and since the mole is 40 cm long and inclined 30° with respect to vertical, he mole tip is likely at 37 cm depth.

Published
2021

46. Results from InSight's First Full Martian Year.

Author

UCL - SST/ELI/ELIC - Earth & Climate, Panning M., Banerdt B., Smrekar S., Antonangeli D., Dehant, Véronique, UCL - SST/ELI/ELIC - Earth & Climate, Panning M., Banerdt B., Smrekar S., Antonangeli D., and Dehant, Véronique

Abstract

The InSight mission landed on Mars in November of 2018 and completed installation of a seismometer (SEIS) on the surface about two months later [1]. In addition to SEIS, InSight carries a diverse geophysical observatory including a heat flow and physical properties package (HP3 ), a geodesy (planetary rotation dynamics) experiment (RISE) and a suite of environmental sensors measuring the magnetic field and atmospheric temperature, pressure and wind (APSS). For approximately 2 years, SEIS has been providing near-continuous seismic monitoring of Mars, with background noise levels orders of magnitude lower than that achievable on the Earth. Since the first detection of a marsquake in April of 2018, the SEIS team has identified more than 450 events that appear to be of tectonic origin. We present a summary of observations and results from the SEIS instrument as well as a summary of other geophysical observations made by InSight during the past 2 years.

Published
2021

47. Companion guide to the marsquake catalog from InSight, Sols 0–478: Data content and non-seismic events

Author

Swiss National Science Foundation, Agence Nationale de la Recherche (France), Swiss National Supercomputing Centre, UK Space Agency, Centre National D'Etudes Spatiales (France), ETH Zurich, State Secretariat for Education, Research and Innovation (Switzerland), Schimmel, Martin [0000-0003-2601-4462], Ceylan, S., Clinton, John F., Giardini, Domenico, Böse, M., Charalambous, C., van Driel, M., Horleston, A., Kawamura, T., Khan, A., Orhand-Mainsant, Guenolé, Scholz, J. R., Stahler, S. C., Euchner, F., Banerdt, W. B., Lognonné, P., Banfield, D., Beucler, E., Garcia, R. F., Kedar, S., Panning, M.P., Pike, William T., Smrekar, S. E., Spiga, A., Dahmen, N. L., Hurst, K., Stott, A. E., Lorenz, R. D., Schimmel, Martin, Stutzmann, E., ten Pierick, J., Conejero, Vicente, Pardo, C., Perrin, C., Swiss National Science Foundation, Agence Nationale de la Recherche (France), Swiss National Supercomputing Centre, UK Space Agency, Centre National D'Etudes Spatiales (France), ETH Zurich, State Secretariat for Education, Research and Innovation (Switzerland), Schimmel, Martin [0000-0003-2601-4462], Ceylan, S., Clinton, John F., Giardini, Domenico, Böse, M., Charalambous, C., van Driel, M., Horleston, A., Kawamura, T., Khan, A., Orhand-Mainsant, Guenolé, Scholz, J. R., Stahler, S. C., Euchner, F., Banerdt, W. B., Lognonné, P., Banfield, D., Beucler, E., Garcia, R. F., Kedar, S., Panning, M.P., Pike, William T., Smrekar, S. E., Spiga, A., Dahmen, N. L., Hurst, K., Stott, A. E., Lorenz, R. D., Schimmel, Martin, Stutzmann, E., ten Pierick, J., Conejero, Vicente, Pardo, C., and Perrin, C.

Abstract

The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed on the surface of Mars on November 26, 2018. One of the scientific instruments in the payload that is essential to the mission is the SEIS package (Seismic Experiment for Interior Structure) which includes a very broadband and a short period seismometer. More than one year since the landing, SEIS continues to be fully operational and has been collecting an exceptional data set which contains not only the signals of seismic origins, but also noise and artifacts induced by the martian environment, the hardware on the ground that includes the seismic sensors, and the programmed operational activities of the lander. Many of these non-seismic signals will be unfamiliar to the scientific community. In addition, many of these signals have signatures that may resemble seismic events either or both in time and frequency domains. Here, we report our observations of common non-seismic signals as seen during the first 478 sols of the SEIS data, i.e. from landing until the end of March 2020. This manuscript is intended to provide a guide to scientists who use the data recorded on SEIS, detailing the general attributes of the most commonly observed non-seismic features. It will help to clarify the characteristics of the seismic dataset for future research, and to avoid misinterpretations when searching for marsquakes.

Published
2021

48. Seismic Constraints on the Thickness and Structure of the Martian Crust from InSight

Author

California Institute of Technology, Panning, M., Knapmeyer‐Endrun, Brigitte, Bissig, F., Joshi, R., Khan, A., Kim, D., Lekic, Vedran, Tauzin, B., Tharimena, S., Plasman, M., Compaire, N., Garcia, R., Margerin, L., Schimmel, Martin, Stutzmann, E., Schmerr, N., Bozdag, E., Plesa, A. C., Wieczorek, M., Broquet, A., Antonangeli, D., McLennan, Scott M., Samuel, H., Michaut, C., Pan, L., Perrin , C., Smrekar, S., Johnson, C. L., Brinkmann, N., Mittelholz, A., Rivoldini, A., Davis, P., Lognonné, P., Pinot, B, Scholz, J. R., Stähler, S., Knapmeyer, M., van Driel, M., Giardini, Domenico, Banerdt, B., California Institute of Technology, Panning, M., Knapmeyer‐Endrun, Brigitte, Bissig, F., Joshi, R., Khan, A., Kim, D., Lekic, Vedran, Tauzin, B., Tharimena, S., Plasman, M., Compaire, N., Garcia, R., Margerin, L., Schimmel, Martin, Stutzmann, E., Schmerr, N., Bozdag, E., Plesa, A. C., Wieczorek, M., Broquet, A., Antonangeli, D., McLennan, Scott M., Samuel, H., Michaut, C., Pan, L., Perrin , C., Smrekar, S., Johnson, C. L., Brinkmann, N., Mittelholz, A., Rivoldini, A., Davis, P., Lognonné, P., Pinot, B, Scholz, J. R., Stähler, S., Knapmeyer, M., van Driel, M., Giardini, Domenico, and Banerdt, B.

Abstract

NASA¿s InSight mission [1] has for the first time placed a very broad-band seismometer on the surface of Mars. The Seismic Experiment for Interior Structure (SEIS) [2] has been collecting continuous data since early February 2019. The main focus of InSight is to enhance our understanding of the internal structure and dynamics of Mars, which includes the goal to better constrain the crustal thickness of the planet [3]. Knowing the present-day crustal thickness of Mars has important implications for its thermal evolution [4] as well as for the partitioning of silicates and heat-producing elements between the different layers of Mars. Current estimates for the crustal thickness of Mars are based on modeling the relationship between topography and gravity [5,6], but these studies rely on different assumptions, e.g. on the density of the crust and upper mantle, or the bulk silicate composition of the planet and the crust. The resulting values for the average crustal thickness differ by more than 100%, from 30 km to more than 100 km [7]. New independent constraints from InSight will be based on seismically determining the crustal thickness at the landing site. This single firm measurement of crustal thickness at one point on the planet will allow to constrain both the average crustal thickness of Mars as well as thickness variations across the planet when combined with constraints from gravity and topography [8]. Here we describe the determination of the crustal structure and thickness at the InSight landing site based on seismic receiver functions for three marsquakes compared with autocorrelations of InSight data [9].

Published
2021

49. Thickness and structure of the Martian crust from InSight seismic data

Author

California Institute of Technology, Swiss National Science Foundation, European Commission, NASA Astrobiology Institute (US), Canadian Space Agency, European Space Agency, Knapmeyer‐Endrun, Brigitte, Panning, M.P., Bissig, F., Joshi, R., Khan, A., Kim, D., Lekic, Vedran, Tauzin, B., Tharimena, S., Plasman, M., Compaire, N., Garcia, R. F., Margerin, L., Schimmel, Martin, Stutzmann, E., Schmerr, N., Bozdag, E., Plesa, A. C., Wieczorek, M. A., Broquet, A., Antonangeli, D., McLennan, Scott M., Samuel, H., Michaut, C., Pan, L., Smrekar, S. E., Johnson, C.L., Brinkman, N., Mittelholz, A., Rivoldini, A., Davis, P. M., Lognonné, P., Pinot, B, Scholz, J. R., Stahler, Simon, Knapmeyer, M., van Driel, M., Giardini, Domenico, Banerdt, W. B., California Institute of Technology, Swiss National Science Foundation, European Commission, NASA Astrobiology Institute (US), Canadian Space Agency, European Space Agency, Knapmeyer‐Endrun, Brigitte, Panning, M.P., Bissig, F., Joshi, R., Khan, A., Kim, D., Lekic, Vedran, Tauzin, B., Tharimena, S., Plasman, M., Compaire, N., Garcia, R. F., Margerin, L., Schimmel, Martin, Stutzmann, E., Schmerr, N., Bozdag, E., Plesa, A. C., Wieczorek, M. A., Broquet, A., Antonangeli, D., McLennan, Scott M., Samuel, H., Michaut, C., Pan, L., Smrekar, S. E., Johnson, C.L., Brinkman, N., Mittelholz, A., Rivoldini, A., Davis, P. M., Lognonné, P., Pinot, B, Scholz, J. R., Stahler, Simon, Knapmeyer, M., van Driel, M., Giardini, Domenico, and Banerdt, W. B.

Abstract

A planet's crust bears witness to the history of planetary formation and evolution, but for Mars, no absolute measurement of crustal thickness has been available. Here, we determine the structure of the crust beneath the InSight landing site on Mars using both marsquake recordings and the ambient wavefield. By analyzing seismic phases that are reflected and converted at subsurface interfaces, we find that the observations are consistent with models with at least two and possibly three interfaces. If the second interface is the boundary of the crust, the thickness is 20 +/- 5 kilometers, whereas if the third interface is the boundary, the thickness is 39 +/- 8 kilometers. Global maps of gravity and topography allow extrapolation of this point measurement to the whole planet, showing that the average thickness of the martian crust lies between 24 and 72 kilometers. Independent bulk composition and geodynamic constraints show that the thicker model is consistent with the abundances of crustal heat-producing elements observed for the shallow surface, whereas the thinner model requires greater concentration at depth.

Published
2021

50. 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

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