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331 results on '"Smrekar, Suzanne E"'

3. Plume‐Induced Delamination Initiated at Rift Zones on Venus

Author

Adams, Andrea C, Stegman, Dave R, Mohammadzadeh, Hiva, Smrekar, Suzanne E, and Tackley, Paul J

Subjects
Earth Sciences, Geochemistry, Geology, Geophysics, Astronomical and Space Sciences, Astronomical sciences
Abstract

Abstract: Venus' tectonic evolution is not well understood. Thousands of kilometers of possible subduction sites on Venus have been identified along networks of rift zone trenches called chasmata. Rift zones are strong candidates for tectonic recycling due to pre‐existing weaknesses in the lithosphere. Recently, peel‐back delamination (PBD) was proposed as a mechanism of regional‐scale lithospheric recycling initiated at Venusian rift zones (Adams et al., 2022, https://doi.org/10.1029/2022je007460). PBD occurs when the lithospheric mantle becomes sufficiently thick and negatively buoyant to decouple and peel away from the overlying crust remaining at the surface. Both positively and negatively buoyant lithosphere were shown to undergo buoyancy‐driven PBD, though delamination is inhibited by increasing positive plate buoyancy. In this study, we use 2D numerical models to verify that delamination can be initiated in thinner, more positively buoyant lithosphere than in models with no plume‐rift interactions. Our results show that plume‐induced PBD in positively buoyant plates is facilitated by the excess negative buoyancy in the lithospheric mantle and increasing plume buoyancy force, and it is inhibited by increasing crustal buoyancy and decreasing rift width. We propose an age‐progressive framework for delamination at rift zones, where young, thin plates require a larger plume buoyancy force to be destabilized than thicker, yet still positively buoyant plates. We use lithospheric thickness constraints to predict PBD may be most likely to initiate near the Dali‐Diana Chasmata system.

Published
2023

5. Volcanic and Tectonic Constraints on the Evolution of Venus

Author

Ghail, Richard C., Smrekar, Suzanne E., Widemann, Thomas, Byrne, Paul K., Gülcher, Anna J. P., O’Rourke, Joseph G., Borrelli, Madison E., Gilmore, Martha S., Herrick, Robert R., Ivanov, Mikhail A., Plesa, Ana-Catalina, Rolf, Tobias, Sabbeth, Leah, Schools, Joe W., and Gregory Shellnutt, J.

Published
2024
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6. Seismic detection of a deep mantle discontinuity within Mars by InSight

Author

Huang, Quancheng, Schmerr, Nicholas C, King, Scott D, Kim, Doyeon, Rivoldini, Attilio, Plesa, Ana-Catalina, Samuel, Henri, Maguire, Ross R, Karakostas, Foivos, Lekić, Vedran, Charalambous, Constantinos, Collinet, Max, Myhill, Robert, Antonangeli, Daniele, Drilleau, Mélanie, Bystricky, Misha, Bollinger, Caroline, Michaut, Chloé, Gudkova, Tamara, Irving, Jessica CE, Horleston, Anna, Fernando, Benjamin, Leng, Kuangdai, Nissen-Meyer, Tarje, Bejina, Frederic, Bozdağ, Ebru, Beghein, Caroline, Waszek, Lauren, Siersch, Nicki C, Scholz, John-Robert, Davis, Paul M, Lognonné, Philippe, Pinot, Baptiste, Widmer-Schnidrig, Rudolf, Panning, Mark P, Smrekar, Suzanne E, Spohn, Tilman, Pike, William T, Giardini, Domenico, and Banerdt, W Bruce

Subjects
Earth Sciences, Physical Sciences, Astronomical Sciences, Geology, Geophysics, Earth, Planet, Extraterrestrial Environment, Iron, Mars, Minerals, interior of Mars, mantle transition zone, thermal evolution of Mars
Abstract

Constraining the thermal and compositional state of the mantle is crucial for deciphering the formation and evolution of Mars. Mineral physics predicts that Mars' deep mantle is demarcated by a seismic discontinuity arising from the pressure-induced phase transformation of the mineral olivine to its higher-pressure polymorphs, making the depth of this boundary sensitive to both mantle temperature and composition. Here, we report on the seismic detection of a midmantle discontinuity using the data collected by NASA's InSight Mission to Mars that matches the expected depth and sharpness of the postolivine transition. In five teleseismic events, we observed triplicated P and S waves and constrained the depth of this discontinuity to be 1,006 [Formula: see text] 40 km by modeling the triplicated waveforms. From this depth range, we infer a mantle potential temperature of 1,605 [Formula: see text] 100 K, a result consistent with a crust that is 10 to 15 times more enriched in heat-producing elements than the underlying mantle. Our waveform fits to the data indicate a broad gradient across the boundary, implying that the Martian mantle is more enriched in iron compared to Earth. Through modeling of thermochemical evolution of Mars, we observe that only two out of the five proposed composition models are compatible with the observed boundary depth. Our geodynamic simulations suggest that the Martian mantle was relatively cold 4.5 Gyr ago (1,720 to 1,860 K) and are consistent with a present-day surface heat flow of 21 to 24 mW/m2.

Published
2022

7. Regional-Scale Lithospheric Recycling on Venus via Peel-Back Delamination

Author

Adams, Andrea C, Stegman, David R, Smrekar, Suzanne E, and Tackley, Paul J

Subjects
Venus, resurfacing, delamination
Abstract

We currently have a limited understanding of the tectonic framework that governs Venus. Schubert and Sandwell (1995) identified over 10,000 km of possible subduction sites at both coronae and chasmata rift zones. Previous numerical and experimental studies have shown the viability of regional-scale lithospheric recycling via plume-lithosphere interactions at coronae, yet little work has been done to study the possibility of resurfacing initiated at Venusian rift zones. We created 2D numerical models to test if and how regional-scale resurfacing could be initiated at a lateral lithospheric discontinuity. We observed several instances of peel-back delamination - a form of lithospheric recycling in which the dense lithospheric mantle decouples and peels away from the weak, initially 30 km-thick crust, leaving behind a hot, thinned layer of crust at the surface. Delamination initiation is driven by the negative buoyancy of the lithospheric mantle and is resisted by the coupling of the plate across the Moho, the significant positive buoyancy of the crust arising from a range of crustal densities, and the viscous strength of the plate. Initial plate bending promotes yielding and weakening in the crust, which is crucial to allow decoupling of the crust and lithospheric mantle. When there is sufficient excess negative buoyancy in the lithospheric mantle, both positively and negatively buoyant plates may undergo delamination. Following a delamination event, the emplacement of hot, buoyant asthenosphere beneath the crust may have consequences for regional-scale volcanism and local tectonic deformation on Venus within the context of the regional equilibrium resurfacing hypothesis.

Published
2022

8. InSight Constraints on the Global Character of the Martian Crust

Author

Wieczorek, Mark A, Broquet, Adrien, McLennan, Scott M, Rivoldini, Attilio, Golombek, Matthew, Antonangeli, Daniele, Beghein, Caroline, Giardini, Domenico, Gudkova, Tamara, Gyalay, Szilárd, Johnson, Catherine L, Joshi, Rakshit, Kim, Doyeon, King, Scott D, Knapmeyer‐Endrun, Brigitte, Lognonné, Philippe, Michaut, Chloé, Mittelholz, Anna, Nimmo, Francis, Ojha, Lujendra, Panning, Mark P, Plesa, Ana‐Catalina, Siegler, Matthew A, Smrekar, Suzanne E, Spohn, Tilman, and Banerdt, W Bruce

Subjects
mars, crust, crustal composition, gravity, seismology, Astronomical and Space Sciences, Geochemistry, Geology
Abstract

Analyses of seismic data from the InSight mission have provided the first in situ constraints on the thickness of the crust of Mars. These crustal thickness constraints are currently limited to beneath the lander that is located in the northern lowlands, and we use gravity and topography data to construct global crustal thickness models that satisfy the seismic data. These models consider a range of possible mantle and core density profiles, a range of crustal densities, a low-density surface layer, and the possibility that the crustal density of the northern lowlands is greater than that of the southern highlands. Using the preferred InSight three-layer seismic model of the crust, the average crustal thickness of the planet is found to lie between 30 and 72 km. Depending on the choice of the upper mantle density, the maximum permissible density of the northern lowlands and southern highlands crust is constrained to be between 2,850 and 3,100 kg m−3. These crustal densities are lower than typical Martian basaltic materials and are consistent with a crust that is on average more felsic than the materials found at the surface. We argue that a substantial portion of the crust of Mars is a primary crust that formed during the initial differentiation of the planet. Various hypotheses for the origin of the observed intracrustal seisimic layers are assessed, with our preferred interpretation including thick volcanic deposits, ejecta from the Utopia basin, porosity closure, and differentiation products of a Borealis impact melt sheet.

Published
2022

10. Correction to: Venus Evolution Through Time: Key Science Questions, Selected Mission Concepts and Future Investigations

Author

Widemann, Thomas, Smrekar, Suzanne E., Garvin, James B., Straume-Lindner, Anne Grete, Ocampo, Adriana C., Schulte, Mitchell D., Voirin, Thomas, Hensley, Scott, Dyar, M. Darby, Whitten, Jennifer L., Nunes, Daniel C., Getty, Stephanie A., Arney, Giada N., Johnson, Natasha M., Kohler, Erika, Spohn, Tilman, O’Rourke, Joseph G., Wilson, Colin F., Way, Michael J., Ostberg, Colby, Westall, Frances, Höning, Dennis, Jacobson, Seth, Salvador, Arnaud, Avice, Guillaume, Breuer, Doris, Carter, Lynn, Gilmore, Martha S., Ghail, Richard, Helbert, Jörn, Byrne, Paul, Santos, Alison R., Herrick, Robert R., Izenberg, Noam, Marcq, Emmanuel, Rolf, Tobias, Weller, Matt, Gillmann, Cedric, Korablev, Oleg, Zelenyi, Lev, Zasova, Ludmila, Gorinov, Dmitry, Seth, Gaurav, Rao, C. V. Narasimha, and Desai, Nilesh

Published
2023
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11. Venus Evolution Through Time: Key Science Questions, Selected Mission Concepts and Future Investigations

Author

Widemann, Thomas, Smrekar, Suzanne E., Garvin, James B., Straume-Lindner, Anne Grete, Ocampo, Adriana C., Schulte, Mitchell D., Voirin, Thomas, Hensley, Scott, Dyar, M. Darby, Whitten, Jennifer L., Nunes, Daniel C., Getty, Stephanie A., Arney, Giada N., Johnson, Natasha M., Kohler, Erika, Spohn, Tilman, O’Rourke, Joseph G., Wilson, Colin F., Way, Michael J., Ostberg, Colby, Westall, Frances, Höning, Dennis, Jacobson, Seth, Salvador, Arnaud, Avice, Guillaume, Breuer, Doris, Carter, Lynn, Gilmore, Martha S., Ghail, Richard, Helbert, Jörn, Byrne, Paul, Santos, Alison R., Herrick, Robert R., Izenberg, Noam, Marcq, Emmanuel, Rolf, Tobias, Weller, Matt, Gillmann, Cedric, Korablev, Oleg, Zelenyi, Lev, Zasova, Ludmila, Gorinov, Dmitry, Seth, Gaurav, Rao, C. V. Narasimha, and Desai, Nilesh

Published
2023
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12. MSS/1: Single‐Station and Single‐Event Marsquake Inversion

Author

Drilleau, Mélanie, Beucler, Éric, Lognonné, Philippe, Panning, Mark P, Knapmeyer‐Endrun, Brigitte, Banerdt, W Bruce, Beghein, Caroline, Ceylan, Savas, Driel, Martin, Joshi, Rakshit, Kawamura, Taichi, Khan, Amir, Menina, Sabrina, Rivoldini, Attilio, Samuel, Henri, Stähler, Simon, Xu, Haotian, Bonnin, Mickaël, Clinton, John, Giardini, Domenico, Kenda, Balthasar, Lekic, Vedran, Mocquet, Antoine, Murdoch, Naomi, Schimmel, Martin, Smrekar, Suzanne E, Stutzmann, Éléonore, Tauzin, Benoit, and Tharimena, Saikiran

Subjects
InSight, inversion, seismology
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

14. Resurfacing History and Volcanic Activity of Venus

Author

Herrick, Robert R., Bjonnes, Evan T., Carter, Lynn M., Gerya, Taras, Ghail, Richard C., Gillmann, Cédric, Gilmore, Martha, Hensley, Scott, Ivanov, Mikhail A., Izenberg, Noam R., Mueller, Nils T., O’Rourke, Joseph G., Rolf, Tobias, Smrekar, Suzanne E., and Weller, Matthew B.

Published
2023
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15. Mars from the InSight: Seismology Beyond Earth

Author

Knapmeyer-Endrun, Brigitte, Banerdt, W. Bruce, Smrekar, Suzanne E., Lognonné, Philippe, Giardini, Domenico, Beghein, Caroline, Beucler, Éric, Bozdağ, Ebru, Clinton, John, Garcia, Raphael F., Irving, Jessica C. E., Kawamura, Taichi, Kedar, Sharon, Margerin, Ludovic, Panning, Mark P., Pike, Tom W., Plesa, Ana-Catalina, Schmerr, Nicholas, Teanby, Nicholas, Weber, Renee, Wieczorek, Mark, Barkaoui, Salma, Brinkman, Nienke, Ceylan, Savas, Charalambous, Constantinos, Compaire, Nicolas, Dahmen, Nikolaj, van Driel, Martin, Horleston, Anna, Huang, Quancheng, Hurst, Kenneth, Kenda, Balthasar, Khan, Amir, Kim, Doyeon, Knapmeyer, Martin, Li, Jiaqi, Menina, Sabrina, Murdoch, Naomi, Perrin, Clément, Schimmel, Martin, Stähler, Simon C., Stutzmann, Eléonore, Bezaeva, Natalia S., Series Editor, Gomes Coe, Heloisa Helena, Series Editor, Nawaz, Muhammad Farrakh, Series Editor, Vacareanu, Radu, editor, and Ionescu, Constantin, editor

Published
2022
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19. CORONAE ON VENUS

Author

STOFAN, ELLEN R., primary, HAMILTON, VICTORIA E., additional, JANES, DANIEL M., additional, and SMREKAR, SUZANNE E., additional

Published
2022
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21. Companion guide to the marsquake catalog from InSight, Sols 0–478: Data content and non-seismic events

Author

Ceylan, Savas, Clinton, John F., Giardini, Domenico, Böse, Maren, Charalambous, Constantinos, Driel, Martin van, Horleston, Anna, Kawamura, Taichi, Khan, Amir, Orhand-Mainsant, Guenolé, Scholz, John-Robert, Stähler, Simon C., Euchner, Fabian, Banerdt, William B., Lognonné, Philippe, Banfield, Don, Beucler, Eric, Garcia, Raphaël F., Kedar, Sharon, Panning, Mark P., Pike, William T., Smrekar, Suzanne E., Spiga, Aymeric, Dahmen, Nikolaj L., Hurst, Kenneth, Stott, Alexander E., Lorenz, Ralph D., Schimmel, Martin, Stutzmann, Eléonore, Pierick, Jan ten, Conejero, Vincent, Pardo, Constanza, and Perrin, Clément

Published
2021
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22. The Marsquake catalogue from InSight, sols 0–478

Author

Clinton, John F., Ceylan, Savas, van Driel, Martin, Giardini, Domenico, Stähler, Simon C., Böse, Maren, Charalambous, Constantinos, Dahmen, Nikolaj L., Horleston, Anna, Kawamura, Taichi, Khan, Amir, Orhand-Mainsant, Guenolé, Scholz, John-Robert, Euchner, Fabian, Banerdt, William B., Lognonné, Philippe, Banfield, Don, Beucler, Eric, Garcia, Raphaël F., Kedar, Sharon, Panning, Mark P., Perrin, Clement, Pike, William T., Smrekar, Suzanne E., Spiga, Aymeric, and Stott, Alexander E.

Published
2021
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23. Mars Soil Temperature and Thermal Properties from InSight HP^3 Data

Author

Spohn, Tilman, primary, Krause, Christian, additional, Golombeck, Matthew, additional, Mueller, Nils T, additional, Grott, Matthias, additional, Knollenberg, Joerg, additional, Plesa, Ana-Catalina, additional, Breuer, Doris, additional, Morgan, Paul, additional, Bickel, Valentin T., additional, Banerdt, William Bruce, additional, and Smrekar, Suzanne E, additional

Published
2024
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25. The atmosphere of Mars as observed by InSight

Author

Banfield, Don, Spiga, Aymeric, Newman, Claire, Forget, François, Lemmon, Mark, Lorenz, Ralph, Murdoch, Naomi, Viudez-Moreiras, Daniel, Pla-Garcia, Jorge, Garcia, Raphaël F., Lognonné, Philippe, Karatekin, Özgür, Perrin, Clément, Martire, Léo, Teanby, Nicholas, Hove, Bart Van, Maki, Justin N., Kenda, Balthasar, Mueller, Nils T., Rodriguez, Sébastien, Kawamura, Taichi, McClean, John B., Stott, Alexander E., Charalambous, Constantinos, Millour, Ehouarn, Johnson, Catherine L., Mittelholz, Anna, Määttänen, Anni, Lewis, Stephen R., Clinton, John, Stähler, Simon C., Ceylan, Savas, Giardini, Domenico, Warren, Tristram, Pike, William T., Daubar, Ingrid, Golombek, Matthew, Rolland, Lucie, Widmer-Schnidrig, Rudolf, Mimoun, David, Beucler, Éric, Jacob, Alice, Lucas, Antoine, Baker, Mariah, Ansan, Véronique, Hurst, Kenneth, Mora-Sotomayor, Luis, Navarro, Sara, Torres, Josefina, Lepinette, Alain, Molina, Antonio, Marin-Jimenez, Mercedes, Gomez-Elvira, Javier, Peinado, Veronica, Rodriguez-Manfredi, Jose-Antonio, Carcich, Brian T., Sackett, Stephen, Russell, Christopher T., Spohn, Tilman, Smrekar, Suzanne E., and Banerdt, W. Bruce

Published
2020
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26. Initial results from the InSight mission on Mars

Author

Banerdt, W. Bruce, Smrekar, Suzanne E., Banfield, Don, Giardini, Domenico, Golombek, Matthew, Johnson, Catherine L., Lognonné, Philippe, Spiga, Aymeric, Spohn, Tilman, Perrin, Clément, Stähler, Simon C., Antonangeli, Daniele, Asmar, Sami, Beghein, Caroline, Bowles, Neil, Bozdag, Ebru, Chi, Peter, Christensen, Ulrich, Clinton, John, Collins, Gareth S., Daubar, Ingrid, Dehant, Véronique, Drilleau, Mélanie, Fillingim, Matthew, Folkner, William, Garcia, Raphaël F., Garvin, Jim, Grant, John, Grott, Matthias, Grygorczuk, Jerzy, Hudson, Troy, Irving, Jessica C. E., Kargl, Günter, Kawamura, Taichi, Kedar, Sharon, King, Scott, Knapmeyer-Endrun, Brigitte, Knapmeyer, Martin, Lemmon, Mark, Lorenz, Ralph, Maki, Justin N., Margerin, Ludovic, McLennan, Scott M., Michaut, Chloe, Mimoun, David, Mittelholz, Anna, Mocquet, Antoine, Morgan, Paul, Mueller, Nils T., Murdoch, Naomi, Nagihara, Seiichi, Newman, Claire, Nimmo, Francis, Panning, Mark, Pike, W. Thomas, Plesa, Ana-Catalina, Rodriguez, Sébastien, Rodriguez-Manfredi, Jose Antonio, Russell, Christopher T., Schmerr, Nicholas, Siegler, Matt, Stanley, Sabine, Stutzmann, Eléanore, Teanby, Nicholas, Tromp, Jeroen, van Driel, Martin, Warner, Nicholas, Weber, Renee, and Wieczorek, Mark

Published
2020
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27. Crustal and time-varying magnetic fields at the InSight landing site on Mars

Author

Johnson, Catherine L., Mittelholz, Anna, Langlais, Benoit, Russell, Christopher T., Ansan, Véronique, Banfield, Don, Chi, Peter J., Fillingim, Matthew O., Forget, Francois, Haviland, Heidi Fuqua, Golombek, Matthew, Joy, Steve, Lognonné, Philippe, Liu, Xinping, Michaut, Chloé, Pan, Lu, Quantin-Nataf, Cathy, Spiga, Aymeric, Stanley, Sabine, Thorne, Shea N., Wieczorek, Mark A., Yu, Yanan, Smrekar, Suzanne E., and Banerdt, William B.

Published
2020
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31. Laboratory VNIR emissivity of Venus analog rocks and the VEM on VERITAS and the VenSpec-M on EnVision calibration and data verification plan

Author

Alemanno, Giulia, primary, Helbert, Jörn, additional, Maturilli, Alessandro, additional, Dyar, Melinda D., additional, Pertenais, Martin, additional, Säuberlich, Thomas, additional, Hagelschuer, Till, additional, Peter, Gisbert, additional, Griessbach, Denis, additional, Adeli, Solmaz, additional, Barraud, Oceane, additional, Van Den Neucker, Aurelie, additional, Ytsma, Cai, additional, and Smrekar, Suzanne E., additional

Published
2023
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34. Mars from the InSight: Seismology Beyond Earth

Author

Knapmeyer-Endrun, Brigitte [0000-0003-3309-6785], Banerdt, W. Bruce [0000-0003-3125-1542], Smrekar, Suzanne E. [0000-0001-8775-075X], Lognonné, Philippe [0000-0002-1014-920X], Giardini, Domenico [0000-0002-5573-7638], Beghein, Caroline [0000-0002-3158-2213], Beucler, Éric [0000-0003-2605-4990], Bozdağ, Ebru 0000-0002-4269-3533`], Clinton, John [0000-0001-8626-2703], Garcia, Raphael F. [0000-0003-1460-6663], Irving, Jessica C. E. [0000-0002-0866-8246], Kawamura, Taichi [0000-0001-5246-5561], Kedar, Sharon [0000-0001-6315-5446], Margerin, Ludovic [0000-0003-4848-3227], Panning, Mark P. [0000-0002-2041-3190], Pike, Tom W. [0000-0002-7660-6231], Plesa, Ana Catalina [0000-0003-3366-7621], Schmerr, Nicholas [0000-0002-3256-1262], Teanby, Nicholas [0000-0003-3108-5775], Weber, Renee [0000-0002-1649-483X], Wieczorek, Mark [0000-0001-7007-4222], Barkaoui, Salma [0000-0001-7266-0815], Brinkman, Nienke [0000-0002-1842-0834], Ceylan, Savas [0000-0002-6552-6850], Charalambous, Constantinos [0000-0002-9139-3895], Compaire, Nicolas [0000-0002-8932-732X], Van Driel, Martin [0000-0002-8938-4615], Horleston, Anna [0000-0002-6748-6522], Huang, Quancheng [0000-0002-5681-5159], Hurst, Kenneth [0000-0002-3822-4689], Kenda, Balthasar [0000-0002-2572-8749], Khan, Amir [0000-0003-4462-3173], Kim, Doyeon [0000-0003-4594-2336], Knapmeyer, Martin [0000-0003-0319-2514], Li, Jiaqi [0000-0001-7525-5401], Menina, Sabrina [0000-0003-1044-6877], Murdoch, Naomi [0000-0002-9701-4075], Perrin, Clément [0000-0002-7200-5682], Schimmel, Martin [0000-0003-2601-4462], Stähler, Simon C. [0000-0002-0783-2489], Stutzmann, Eléonore [0000-0002-4348-7475], Knapmeyer-Endrun, Brigitte, Banerdt, W. Bruce, Smrekar, Suzanne E., Lognonné, Philippe, Giardini, Domenico, Beghein, Caroline, Beucler, Éric, Bozdağ, Ebru, Clinton, John, Garcia, Raphael F., Irving, Jessica C. E., Kawamura, Taichi, Kedar, Sharon, Margerin, Ludovic, Panning, Mark P., Pike, Tom W., Plesa, Ana Catalina, Schmerr, Nicholas, Teanby, Nicholas, Weber, Renee, Wieczorek, Mark, Barkaoui, Salma, Brinkman, Nienke, Ceylan, Savas, Charalambous, Constantinos, Compaire, Nicolas, Dahmen, Nikolaj, van Driel, Martin, Horleston, Anna, Huang, Quancheng, Hurst, Kenneth, Kenda, Balthasar, Khan, Amir, Kim, Doyeon, Knapmeyer, Martin, Li, Jiaqi, Menina, Sabrina, Murdoch, Naomi, Perrin, Clément, Schimmel, Martin, Stähler, Simon C., Stutzmann, Eléonore, Knapmeyer-Endrun, Brigitte [0000-0003-3309-6785], Banerdt, W. Bruce [0000-0003-3125-1542], Smrekar, Suzanne E. [0000-0001-8775-075X], Lognonné, Philippe [0000-0002-1014-920X], Giardini, Domenico [0000-0002-5573-7638], Beghein, Caroline [0000-0002-3158-2213], Beucler, Éric [0000-0003-2605-4990], Bozdağ, Ebru 0000-0002-4269-3533`], Clinton, John [0000-0001-8626-2703], Garcia, Raphael F. [0000-0003-1460-6663], Irving, Jessica C. E. [0000-0002-0866-8246], Kawamura, Taichi [0000-0001-5246-5561], Kedar, Sharon [0000-0001-6315-5446], Margerin, Ludovic [0000-0003-4848-3227], Panning, Mark P. [0000-0002-2041-3190], Pike, Tom W. [0000-0002-7660-6231], Plesa, Ana Catalina [0000-0003-3366-7621], Schmerr, Nicholas [0000-0002-3256-1262], Teanby, Nicholas [0000-0003-3108-5775], Weber, Renee [0000-0002-1649-483X], Wieczorek, Mark [0000-0001-7007-4222], Barkaoui, Salma [0000-0001-7266-0815], Brinkman, Nienke [0000-0002-1842-0834], Ceylan, Savas [0000-0002-6552-6850], Charalambous, Constantinos [0000-0002-9139-3895], Compaire, Nicolas [0000-0002-8932-732X], Van Driel, Martin [0000-0002-8938-4615], Horleston, Anna [0000-0002-6748-6522], Huang, Quancheng [0000-0002-5681-5159], Hurst, Kenneth [0000-0002-3822-4689], Kenda, Balthasar [0000-0002-2572-8749], Khan, Amir [0000-0003-4462-3173], Kim, Doyeon [0000-0003-4594-2336], Knapmeyer, Martin [0000-0003-0319-2514], Li, Jiaqi [0000-0001-7525-5401], Menina, Sabrina [0000-0003-1044-6877], Murdoch, Naomi [0000-0002-9701-4075], Perrin, Clément [0000-0002-7200-5682], Schimmel, Martin [0000-0003-2601-4462], Stähler, Simon C. [0000-0002-0783-2489], Stutzmann, Eléonore [0000-0002-4348-7475], Knapmeyer-Endrun, Brigitte, Banerdt, W. Bruce, Smrekar, Suzanne E., Lognonné, Philippe, Giardini, Domenico, Beghein, Caroline, Beucler, Éric, Bozdağ, Ebru, Clinton, John, Garcia, Raphael F., Irving, Jessica C. E., Kawamura, Taichi, Kedar, Sharon, Margerin, Ludovic, Panning, Mark P., Pike, Tom W., Plesa, Ana Catalina, Schmerr, Nicholas, Teanby, Nicholas, Weber, Renee, Wieczorek, Mark, Barkaoui, Salma, Brinkman, Nienke, Ceylan, Savas, Charalambous, Constantinos, Compaire, Nicolas, Dahmen, Nikolaj, van Driel, Martin, Horleston, Anna, Huang, Quancheng, Hurst, Kenneth, Kenda, Balthasar, Khan, Amir, Kim, Doyeon, Knapmeyer, Martin, Li, Jiaqi, Menina, Sabrina, Murdoch, Naomi, Perrin, Clément, Schimmel, Martin, Stähler, Simon C., and Stutzmann, Eléonore

Abstract

When NASA’s InSight lander touched down in Elysium Planitia, Mars, in November 2018 and deployed its seismometer SEIS, it ushered in a new age for planetary seismology - more than 40 years after the first attempt to record marsquakes with the Viking missions. SEIS, an extremely sensitive instrument, has by now provided near continuous seismic records for more than 3 years. Its rich dataset shows Mars to be seismically active, with over 1,300 marsquakes detected so far, mostly with magnitudes below 4. Despite their small size, these quakes provide important and unprecedented constraints on the interior structure of the planet, from the shallow subsurface via the crust, the lithosphere, and the mantle transition zone down to the core, and allow to study Martian tectonics and thermo-chemical evolution. Single-station seismology has answered some of the big questions about the interior of our planetary neighbour, and this contribution gives an overview of results and surprises so far.

Published
2022

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

Author

Grott, Matthias, primary, Piqueux, Sylvain, additional, Spohn, Tilman, additional, Knollenberg, Joerg, additional, Krause, Christian, additional, Marteau, Eloise, additional, Hudson, Troy L., additional, Forget, Francois, additional, Lange, Lucas, additional, Müller, N., additional, Golombek, Matthew P., additional, Nagihara, Seiichi, additional, Morgan, Paul, additional, Murphy, J.P., additional, Siegler, Matthew Adam, additional, King, Scott D., additional, Banfield, Donald, additional, Smrekar, Suzanne E, additional, and Banerdt, William Bruce, additional

Published
2023
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38. The InSight HP³ Penetrator (Mole) on Mars: Soil Properties Derived from the Penetration Attempts and Related Activities

Author

Spohn, Tilman, Hudson, Troy L., Marteau, Eloïse, Golombek, Matthew, Grott, Matthias, Wippermann, Torben, Ali, Khaled S., Schmelzbach, Cédric, Kedar, Sharon, Hurst, Ken, Trebi-Ollennu, Ashitey, Ansan, Véronique, Garvin, James, Knollenberg, Jörg, Müller, N., Piqueux, Sylvain, Lichtenheldt, Roy, Krause, Christian, Fantinati, Cinzia, Brinkman, Nienke, Sollberger, David, Delage, Pierre, Vrettos, Christos, Reershemius, Siebo, Wisniewski, Lukasz, Grygorczuk, Jurek, Robertsson, Johan, Edme, Pascal, Andersson, Fredrik, Krömer, O., Lognonné, Philippe, Giardini, Domenico, Smrekar, Suz̀anne E., and Banerdt, William B.

Subjects
Record of operating a penetrator on Mars, Homestead Hollow near surface structure, Martian soil mechanical and thermal properties
Abstract

The NASA InSight Lander on Mars includes the Heat Flow and Physical Properties Package HP3 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 tip finally reached a depth of about 37 cm, bringing the mole back-end 1–2 cm below the surface. It reversed its downward motion twice during attempts to provide friction through pressure on the regolith instead of directly with the scoop to the mole hull. The penetration record of the mole was used to infer mechanical soil parameters such as the penetration resistance of the duricrust of 0.3–0.7 MPa and a penetration resistance of a deeper layer (> 30 cm depth) of 4.9±0.4 MPa. Using the mole’s thermal sensors, thermal conductivity and diffusivity were measured. Applying cone penetration theory, the resistance of the duricrust was used to estimate a cohesion of the latter of 2–15 kPa depending on the internal friction angle of the duricrust. Pushing the scoop with its blade into the surface and chopping off a piece of duricrust provided another estimate of the cohesion of 5.8 kPa. The hammerings of the mole were recorded by the seismometer SEIS and the signals were used to derive P-wave and S-wave velocities representative of the topmost tens of cm of the regolith. Together with the density provided by a thermal conductivity and diffusivity measurement using the mole’s thermal sensors, the elastic moduli were calculated from the seismic velocities. Using empirical correlations from terrestrial soil studies between the shear modulus and cohesion, the previous cohesion estimates were found to be consistent with the elastic moduli. 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 containing debris from a small impact crater is inferred. The thermal conductivity increases from 14 mW/m K to 34 mW/m K through the 1 cm sand/dust layer, keeps the latter value in the duricrust and the sand layer underneath and then increases to 64 mW/m K in the sand/gravel layer below., Space Science Reviews, 218 (8), ISSN:1572-9672, ISSN:0038-6308

Published
2022

40. Pre-mission InSights on the Interior of Mars

Author

Smrekar, Suzanne E., Lognonné, Philippe, Spohn, Tilman, Banerdt, W. Bruce, Breuer, Doris, Christensen, Ulrich, Dehant, Véronique, Drilleau, Mélanie, Folkner, William, Fuji, Nobuaki, Garcia, Raphael F., Giardini, Domenico, Golombek, Matthew, Grott, Matthias, Gudkova, Tamara, Johnson, Catherine, Khan, Amir, Langlais, Benoit, Mittelholz, Anna, Mocquet, Antoine, Myhill, Robert, Panning, Mark, Perrin, Clément, Pike, Tom, Plesa, Ana-Catalina, Rivoldini, Attilio, Samuel, Henri, Stähler, Simon C., van Driel, Martin, Van Hoolst, Tim, Verhoeven, Olivier, Weber, Renee, and Wieczorek, Mark

Published
2018
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43. InSight Constraints on the Global Character of the Martian Crust

Author

Wieczorek, Mark A., Broquet, Adrien, McLennan, Scott M., Rivoldini, Attilio, Golombek, Matthew, Antonangeli, Daniele, Beghein, Caroline, Giardini, Domenico, Gudkova, Tamara, Gyalay, Szilárd, Johnson, Catherine L., Joshi, Rakshit, Kim, Doyeon, King, Scott D., Knapmeyer-Endrun, Brigitte, Lognonné, Philippe, Mittelholz, Anna, Nimmo, Francis, Ojha, Lujendra, Panning, Mark P., Plesa, Ana-Catalina, Siegler, Matthew A., Smrekar, Suzanne E., Spohn, Tilman, and Banerdt, Bruce W.

Subjects
crustal composition, mars, crust, gravity, seismology
Abstract

Analyses of seismic data from the InSight mission have provided the first in situ constraints on the thickness of the crust of Mars. These crustal thickness constraints are currently limited to beneath the lander that is located in the northern lowlands, and we use gravity and topography data to construct global crustal thickness models that satisfy the seismic data. These models consider a range of possible mantle and core density profiles, a range of crustal densities, a low-density surface layer, and the possibility that the crustal density of the northern lowlands is greater than that of the southern highlands. Using the preferred InSight three-layer seismic model of the crust, the average crustal thickness of the planet is found to lie between 30 and 72 km. Depending on the choice of the upper mantle density, the maximum permissible density of the northern lowlands and southern highlands crust is constrained to be between 2,850 and 3,100 kg m(-3). These crustal densities are lower than typical Martian basaltic materials and are consistent with a crust that is on average more felsic than the materials found at the surface. We argue that a substantial portion of the crust of Mars is a primary crust that formed during the initial differentiation of the planet. Various hypotheses for the origin of the observed intracrustal seisimic layers are assessed, with our preferred interpretation including thick volcanic deposits, ejecta from the Utopia basin, porosity closure, and differentiation products of a Borealis impact melt sheet., Journal of Geophysical Research: Planets, 127 (5), ISSN:0148-0227, ISSN:2169-9097

Published
2022

50. Mars North Polar Deposits: Stratigraphy, Age, and Geodynamical Response

Author

Phillips, Roger J., Zuber, Maria T., Smrekar, Suzanne E., Mellon, Michael T., Head, James W., Tanaka, Kenneth L., Putzig, Nathaniel E., Milkovich, Sarah M., Campbell, Bruce A., Plaut, Jeffrey J., Safaeinili, Ali, Seu, Roberto, Biccari, Daniela, Carter, Lynn M., Picardi, Giovanni, Orosei, Roberto, Mohit, P. Surdas, Heggy, Essam, Zurek, Richard W., Egan, Anthony F., giacommoni, Emanuele, Russo, Federica, Cutigni, Macro, Pettinelli, Elena, Holt, John W., Leuschen, Carl J., and Marinangeli, Lucia

Published
2008
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