Search

Your search keyword '"Antonangeli, D."' showing total 163 results
Start Over Author "Antonangeli, D."
163 results on '"Antonangeli, D."'

1. Equation of state of SiC at extreme conditions: new insight into the interior of carbon rich exoplanets

Author

Miozzi, F., Morard, G., Antonangeli, D., Clark, A. N., Mezouar, M., Dorn, C., Rozel, A., and Fiquet, G.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

There is a direct relation between the composition of a host star and that of the planets orbiting around it. As such, the recent discovery of stars with unusual chemical composition, notably enriched in carbon instead of oxygen, support the existence of exoplanets with a chemistry dominated by carbides instead of oxides. Accordingly several studies have been recently conducted on the Si C binary system at high pressure and temperature. Nonetheless, the properties of carbides at the P T conditions of exoplanets interiors are still inadequately constrained, effectively hampering reliable planetary modeling. Here we present an in situ X ray diffraction study of the Si C binary system up to 200 GPa and 3500 K, significantly enlarging the pressure range explored by previous experimental studies. The large amount of collected data allows us to properly investigate the phase diagram and to refine the Clapeyron slope of the transition line from the zinc blende to the rock salt structure. Furthermore the pressure volume temperature equation of state are provided for the high pressure phase, characterized by low compressibility and thermal expansion. Our results are used to model idealized C rich exoplanets of end members composition. In particular, we derived mass radius relations and performed numerical simulations defining rheological parameters and initial conditions which lead to onset of convection in such SiC planets. We demonstrate that if restrained to silicate rich mantle compositions, the interpretation of mass radius relations may underestimate the interior diversity of exoplanets., Comment: 30 Pages, 8 Figures

Published
2018
Full Text
View/download PDF

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
Full Text
View/download PDF

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
Full Text
View/download PDF

6. 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

7. 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

8. 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

9. A Cerberus Fossae Seismic Network

Author

Stahler, S. C., Panning, Mark P., Antonangeli, D., Banerdt, W. B., Banks, M., Ceylan, S., Charalambous, C., Clinton, John, Daubar, I., Fernando, B., Giardini, Domenico, Grott, M., Horleston, A., Hurst, K., Kawamura, T., Khan, A., Kim, D., Knapmeyer, M., Knapmeyer-Endrun, Brigitte, Lorenz, L., Margerin, L., Marusiak, A, Menina, S., Mittelholz, A., Murdoch, N., Nishikawa, Y., Nunn, C., Perrin, C., Pike, William T., Schmelzbach, C., Schmerr, N., Schimmel, Martin, Spiga, A., Stott, A., Taylor, J., Weber, R., Stahler, S. C., Panning, Mark P., Antonangeli, D., Banerdt, W. B., Banks, M., Ceylan, S., Charalambous, C., Clinton, John, Daubar, I., Fernando, B., Giardini, Domenico, Grott, M., Horleston, A., Hurst, K., Kawamura, T., Khan, A., Kim, D., Knapmeyer, M., Knapmeyer-Endrun, Brigitte, Lorenz, L., Margerin, L., Marusiak, A, Menina, S., Mittelholz, A., Murdoch, N., Nishikawa, Y., Nunn, C., Perrin, C., Pike, William T., Schmelzbach, C., Schmerr, N., Schimmel, Martin, Spiga, A., Stott, A., Taylor, J., and Weber, R.

Abstract

Scientific Rationale: It is by now widely accepted that Mars had a wet and periodically warm past in the Noachian e.g. [1], but it is still open whether liquid water has played any role geologically in recent times or is even present in significant amounts near the surface today e.g. [2]. One key young area are the Cerberus Fossae (C.F.), a system of < 10 Ma old, 1200 km long grabens in Eastern Elysium Planitia. They connect to sediments in Athabasca Valles that have been interpreted as fluvial sediments from a frozen water layer molten by volcanism 8-10 Ma ago [3], but could alternatively be explained by very low viscosity lava as well [4]

Published
2023

10. 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

11. Amorpheus: a Python-based software for the treatment of X-ray scattering data of amorphous and liquid systems

Author

Boccato, S., Garino, Y., Morard, G., Zhao, B., Xu, F., Sanloup, C., King, A., Guignot, N., Clark, A., Garbarino, G., Morand, M., Antonangeli, D., Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), and Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.COND.CM-MS]Physics [physics]/Condensed Matter [cond-mat]/Materials Science [cond-mat.mtrl-sci], [PHYS.COND.CM-DS-NN]Physics [physics]/Condensed Matter [cond-mat]/Disordered Systems and Neural Networks [cond-mat.dis-nn], Condensed Matter Physics, [PHYS.PHYS.PHYS-DATA-AN]Physics [physics]/Physics [physics]/Data Analysis, Statistics and Probability [physics.data-an]
Abstract

International audience

Published
2022
Full Text
View/download PDF

12. A Cerberus Fossae Seismic Network

Author

Stähler, S., Panning, M., Antonangeli, D., Banerdt, B., Banfield, D., Banks, M., Ceylan, S., Charalambous, C., Clinton, John, Daubar, I., Fernando, B., Giardini, D., Grott, Matthias, Horleston, A., Hurst, K., Kawamura, T., Khan, A., Kim, D., Knapmeyer, Martin, Knapmeyer-Endrun, B., Lorenz, R. D., Margerin, L., Marusiak, A, Menina, S., Mittelholz, A., Murdoch, N., Nishikawa, Yasuhiro, Nunn, C., Perrin, C., Pike, W.T., Schmelzbach, C., Schmerr, N., Schimmel, M., Spiga, A., Stott, A., Taylor, Jake, and Weber, R.

Subjects
Mars Seismology Missions
Published
2023

15. X-ray diffraction study of phase transformation dynamics of Fe and Fe-Si alloys along the shock Hugoniot using an x-ray free electron laser

Author

Krygier, A., primary, Harmand, M., additional, Albertazzi, B., additional, McBride, E. E., additional, Miyanishi, K., additional, Antonangeli, D., additional, Inubushi, Y., additional, Kodama, R., additional, Koenig, M., additional, Matsuoka, T., additional, Mogni, G., additional, Pietrucci, F., additional, Saitta, A. M., additional, Togashi, T., additional, Umeda, Y., additional, Vinci, T., additional, Yabashi, M., additional, Yabuuchi, T., additional, Fiquet, G., additional, and Ozaki, N., additional

Published
2022
Full Text
View/download PDF

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

Author

Wieczorek, MA, Wieczorek, MA, Broquet, A, McLennan, SM, Rivoldini, A, Golombek, M, Antonangeli, D, Beghein, C, Giardini, D, Gudkova, T, Gyalay, S, Johnson, CL, Joshi, R, Kim, D, King, SD, Knapmeyer-Endrun, B, Lognonné, P, Michaut, C, Mittelholz, A, Nimmo, F, Ojha, L, Panning, MP, Plesa, AC, Siegler, MA, Smrekar, SE, Spohn, T, Banerdt, WB, Wieczorek, MA, Wieczorek, MA, Broquet, A, McLennan, SM, Rivoldini, A, Golombek, M, Antonangeli, D, Beghein, C, Giardini, D, Gudkova, T, Gyalay, S, Johnson, CL, Joshi, R, Kim, D, King, SD, Knapmeyer-Endrun, B, Lognonné, P, Michaut, C, Mittelholz, A, Nimmo, F, Ojha, L, Panning, MP, Plesa, AC, Siegler, MA, Smrekar, SE, Spohn, T, and Banerdt, WB

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

17. 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

18. 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

19. A view into the deep interior of Mars from nutation measured by InSight RISE

Author

Rivoldini, Attilio, Le Maistre, Sébastien, Caldiero, Alfonso, Yseboodt, Marie, Baland, Rose-Marie, Beuthe, Mikael, van Hoolst, Tim, Dehant, Veronique, Folkner, William M., Buccino, Dustin, Kahan, Daniel S., Marty, Jean-Charles, Antonangeli, D., Badro, James, Drilleau, Mélanie, Konopliv, Alex S., Peters, Marie-Julie, Plesa, Ana-Catalina, Samuel, Henri, and Tosi, Nicola

Subjects
Mars, RISE, Interior structure, InSight
Abstract

We report the results of more than 2 years of monitoring the rotation of Mars with the RISE instrument on InSight. Small periodic variations of the spin axis orientation, called nutations, can be extracted from the Doppler data with enough precision to identify the influence of the Martian fluid core. For the first time for a planetary body other than the Earth, we can measure the period of the Free Core Nutation (FCN), which is a rotational normal mode arising from the misalignment of the rotation axes of the core and mantle. In this way, we confirm the liquid state of the core and estimate its moment of inertia as well as its size. The FCN period depends on the dynamical flattening of the core and on its ability to deform. Since the shape and gravity field of Mars deviate significantly from those of a uniformly rotating fluid body, deviations from that state can also be expected for the core. Models accounting for the dynamical shape of Mars can thus be tested by comparing core shape predictions to nutation constraints. The observed FCN period can be accounted for by interior models having a very thick lithosphere loaded by degree-two mass anomalies at the bottom. The combination of nutation data and interior structure modeling allows us to deduce the radius of the core and to constrain its density, and thus, to address the nature and abundance of light elements alloyed to iron. The inferred core radius agrees with previous estimates based on geodesy and seismic data. The large fraction of light elements required to match the core density implies that its liquidus is significantly lower than the expected core temperature, making the presence of an inner core highly unlikely. Besides, the existence of an inner core would lead to an additional rotational normal mode the signature of which has not been detected in the RISE data.

Published
2022
Full Text
View/download PDF

20. The deep interior of Mars from nutation measured by InSight RISE

Author

Le Maistre, Sébastien, Rivoldini, Attilio, Caldiero, Alfonso, Yseboodt, M., Baland, Rose-Marie, Beuthe, Mikael, van Hoolst, Tim, Dehant, Veronique, Folkner, William M., Buccino, Dustin, Kahan, Daniel S., Marty, Jean-Charles, Antonangeli, D., Badro, James, Drilleau, Mélanie, Konopliv, Alex S., Peters, Marie-Julie, Plesa, Ana-Catalina, Samuel, Henri, Tosi, Nicola, and UCL - SST/ELI/ELIC - Earth & Climate

Subjects
Mars, RISE, Interior structure, InSight
Abstract

We report here the results of more than 2 years of monitoring the rotation of Mars with the RISE instrument on InSight. Small periodic variations of the spin axis orientation, called nutations, can be extracted from the Doppler data with enough precision to identify the influence of the Martian fluid core. For the first time for a planetary body other than the Earth, we can measure the period of the Free Core Nutation (FCN), which is a rotational normal mode arising from the misalignment of the rotation axes of the core and mantle. In this way, we confirm the liquid state of the core and estimate its moment of inertia as well as its likely size.The FCN period depends on the dynamical flattening of the core and on its ability to deform. Since the shape and gravity field of Mars deviate significantly from those of a uniformly rotating fluid body, deviations from that state can also be expected for the core. Models accounting for the dynamical shape of Mars can thus be tested by comparing core shape predictions to nutation constraints. The observed FCN period can be accounted for by interior models having a very thick lithosphere loaded by degree-two mass anomalies at the bottom.The combination of nutation data and interior structure modeling allows us to deduce the radius of the core and to constrain its density, and thus, to address the nature and abundance of light elements alloyed to iron. The inferred core radius agrees with previous estimates based on geodesy and seismic data. The large fraction of light elements required to match the core density implies that its liquidus is significantly lower than the expected core temperature, making the presence of an inner core highly unlikely. Besides, the existence of an inner core would lead to an additional rotational normal mode the signature of which has not been detected in the RISE data.

Published
2022
Full Text
View/download PDF

22. 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

23. 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

24. Thermal expansion of liquid Fe-S alloy at high pressure

Author

Xu, F., primary, Morard, G., additional, Guignot, N., additional, Rivoldini, A., additional, Manthilake, G., additional, Chantel, J., additional, Xie, L., additional, Yoneda, A., additional, King, A., additional, Boulard, E., additional, Pandolfi, S., additional, Ryerson, F.J., additional, and Antonangeli, D., additional

Published
2021
Full Text
View/download PDF

25. 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

26. 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

27. 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

29. 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

30. 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

31. 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

32. 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

33. 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

36. New seismological constraints on the crustal structure of Mars and the Moon

Author

Knapmeyer-Endrun, B., Panning, M., Bissig, Felix, Joshi, Rakshit, Khan, A., Kim, Doyeon, Lekic, V., Tauzin, B., Tharimena, S., Plasman, Matthieu, Compaire, Nicolas, Garcia, Raphaël F., Margerin, L., Schimmel, M., Stutzmann, Éléonore, Schmerr, N., Antonangeli, D., Bozdag, E., McLennan, S M, Peter, Daniel, Plesa, Ana-Catalina, Samuel, H., Wieczorek, M., Davis, Paul, Lognonne, P., Pinot, Baptiste, Scholz, J.-R., Stähler, S., Knapmeyer, Martin, Brinkmann, Nienke, van Driel, M, Giardini, D., Johnson, Catherine L., Smrekar, S., and Banerdt, B.

Subjects
receiver functions, crustal thickness, Mars, seismological constraints, InSight
Abstract

Planetary crusts are the results of mantle differentiation, so their thickness provides important constraints on the thermochemical evolution of a planet, including its heat budget and mantle rheology. Information on crustal layering and seismic velocities can also provide important constraints on porosity and geochemistry of the crust. Here, we use data from the InSight mission, which landed in November 2018, to provide seismological constraints on the crustal layering and thickness of Mars for the first time. Results are mainly based on Ps-receiver functions from three events with magnitudes between 3.1 and 3.6 at distances between 27.5° and 47° (±10°) from the lander, originating in the Cerberus Fossae region, the only events, so far, with clear, impulsive P-wave onsets and known epicenter. Ps-receiver functions use converted phases in the P-wave coda to derive information on discontinuities beneath the seismometer. Due to the limited number of events and the small epicentral distance range covered, inversions of the data are still ambiguous. Two sets of models can explain the waveforms, one consisting of a two-layer crust of about 20 to 23 km thickness, the other having a three-layer crust of about 40 to 45 km thickness. By excluding crustal thicknesses in excess of 45 km at the landing site, we can constrain the global average crustal thickness of Mars to be less than 70 km. Both model types also agree with S-receiver functions for two events and seismic P-waves reflected in the crust and extracted from autocorrelations using the coda of different types of marsquakes as well as the background wavefield. Furthermore, the results are compatible with independently conducted moment tensor inversions for a limited number of events as well as modeling of the wave-propagation of high-frequency events. We find low seismic P-wave velocities below 3.4 km/s within the upper approximately 10 km, likely indicating a high porosity. For the Moon, we present Sp-receiver functions for three Apollo landing sites, including the first application of this method to Apollo 15 and 16 data. Data are compatible with a two-layer crust beneath a thin, low-velocity regolith layer and a crustal thickness of 35 to 45 km, with an increased thickness at the Apollo 15 and 16 sites compared to the Apollo12 location.

Published
2020

38. 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

39. New seismological constraints on the crustal structure of Mars and the Moon

Author

Knapmeyer‐Endrun, Brigitte, Panning, Mark P., Bissig, F., Joshi, Rakshit, Khan, A., Kim, Doyeon, Lekic, Vedran, Tauzin, Benoit, Tharimena, S., Plasman, Matthieu, Compaire, Nicolas, Garcia, Raphael F., Margerin, Ludovic, Schimmel, Martin, Stutzmann, E., Schmerr, Nicholas C., Antonangeli, D., Bozdag, E., McLennan, S., Peter, Daniel B., Plesa, A. C., Samuel, H., Wieczorek, M., Davis, Paul, Lognonné, P., Pinot, Baptiste, Scholz, J. R., Staehler, Simon C., Knapmeyer, M., Brinkman, N., van Driel, M., Giardini, Domenico, Johnson, C., Smrekar, S. E., Banerdt, William B., Knapmeyer‐Endrun, Brigitte, Panning, Mark P., Bissig, F., Joshi, Rakshit, Khan, A., Kim, Doyeon, Lekic, Vedran, Tauzin, Benoit, Tharimena, S., Plasman, Matthieu, Compaire, Nicolas, Garcia, Raphael F., Margerin, Ludovic, Schimmel, Martin, Stutzmann, E., Schmerr, Nicholas C., Antonangeli, D., Bozdag, E., McLennan, S., Peter, Daniel B., Plesa, A. C., Samuel, H., Wieczorek, M., Davis, Paul, Lognonné, P., Pinot, Baptiste, Scholz, J. R., Staehler, Simon C., Knapmeyer, M., Brinkman, N., van Driel, M., Giardini, Domenico, Johnson, C., Smrekar, S. E., and Banerdt, William B.

Abstract

Planetary crusts are the results of mantle differentiation, so their thickness provides important constraints on the thermochemical evolution of a planet, including its heat budget and mantle rheology. Information on crustal layering and seismic velocities can also provide important constraints on porosity and geochemistry of the crust. Here, we use data from the InSight mission, which landed in November 2018, to provide seismological constraints on the crustal layering and thickness of Mars for the first time. Results are mainly based on Ps-receiver functions from three events with magnitudes between 3.1 and 3.6 at distances between 27.5° and 47° (±10°) from the lander, originating in the Cerberus Fossae region, the only events, so far, with clear, impulsive P-wave onsets and known epicenter. Ps-receiver functions use converted phases in the P-wave coda to derive information on discontinuities beneath the seismometer. Due to the limited number of events and the small epicentral distance range covered, inversions of the data are still ambiguous. Two sets of models can explain the waveforms, one consisting of a two-layer crust of about 20 to 23 km thickness, the other having a three-layer crust of about 40 to 45 km thickness. By excluding crustal thicknesses in excess of 45 km at the landing site, we can constrain the global average crustal thickness of Mars to be less than 70 km. Both model types also agree with S-receiver functions for two events and seismic P-waves reflected in the crust and extracted from autocorrelations using the coda of different types of marsquakes as well as the background wavefield. Furthermore, the results are compatible with independently conducted moment tensor inversions for a limited number of events as well as modeling of the wave-propagation of high-frequency events. We find low seismic P-wave velocities below 3.4 km/s within the upper approximately 10 km, likely indicating a high porosity. For the Moon, we present Sp-receiver functi

Published
2020

40. 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

41. 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

44. Subsurface Structure at the InSight Landing Site From Compliance Measurements by Seismic and Meteorological Experiments

Author

Kenda, B., primary, Drilleau, M., additional, Garcia, R. F., additional, Kawamura, T., additional, Murdoch, N., additional, Compaire, N., additional, Lognonné, P., additional, Spiga, A., additional, Widmer‐Schnidrig, R., additional, Delage, P., additional, Ansan, V., additional, Vrettos, C., additional, Rodriguez, S., additional, Banerdt, W. B., additional, Banfield, D., additional, Antonangeli, D., additional, Christensen, U., additional, Mimoun, D., additional, Mocquet, A., additional, and Spohn, T., additional

Published
2020
Full Text
View/download PDF

48. Equation of State of SiC at Extreme Conditions: New Insight Into the Interior of Carbon‐Rich Exoplanets

Author

Miozzi, F; https://orcid.org/0000-0001-8926-4122, Morard, G; https://orcid.org/0000-0002-4225-0767, Antonangeli, D; https://orcid.org/0000-0002-4952-5700, Clark, A N; https://orcid.org/0000-0003-3049-3857, Mezouar, M, Dorn, C; https://orcid.org/0000-0001-6110-4610, Rozel, A; https://orcid.org/0000-0002-7408-1099, Fiquet, G; https://orcid.org/0000-0001-8961-3281, Miozzi, F; https://orcid.org/0000-0001-8926-4122, Morard, G; https://orcid.org/0000-0002-4225-0767, Antonangeli, D; https://orcid.org/0000-0002-4952-5700, Clark, A N; https://orcid.org/0000-0003-3049-3857, Mezouar, M, Dorn, C; https://orcid.org/0000-0001-6110-4610, Rozel, A; https://orcid.org/0000-0002-7408-1099, and Fiquet, G; https://orcid.org/0000-0001-8961-3281

Abstract

There is a direct relation between the composition of a host star and that of the planets orbiting around it. As such, the recent discovery of stars with unusual chemical composition, notably enriched in carbon instead of oxygen, supports the existence of exoplanets with a chemistry dominated by carbides instead of oxides. Accordingly, several studies have been recently conducted on the Si–C binary system at high pressure and temperature. Nonetheless, the properties of carbides at the pressure‐temperature conditions of exoplanets interiors are still inadequately constrained, effectively hampering reliable planetary modeling. Here we present an in situ X‐ray diffraction study of the Si–C binary system up to 200 GPa and 3,500 K, significantly enlarging the pressure range explored by previous experimental studies. The large amount of collected data allows us to properly investigate the phase diagram and to refine the Clapeyron slope of the transition line from the zinc blende to the rock salt structure. Furthermore, the pressure‐volume‐temperature equation of state is provided for the high‐pressure phase, characterized by low compressibility and thermal expansion. Our results are used to model idealized C‐rich exoplanets of end‐members composition. In particular, we derived mass‐radius relations and performed numerical simulations defining rheological parameters and initial conditions which lead to onset of convection in such SiC planets. We demonstrate that if restrained to silicate‐rich mantle compositions, the interpretation of mass‐radius relations may underestimate the interior diversity of exoplanets.

Published
2018

49. Structure and Density of Fe-C Liquid Alloys Under High Pressure

Author

Morard, G., Nakajima, Y., Andrault, D., Antonangeli, D., Auzende, A. L., Boulard, E., Cervera, S., Clark, A. N., Lord, O. T., Siebert, J., Svitlyk, V., Garbarino, G., Mezouar, M., Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS), Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Institut national des sciences de l'Univers (INSU - CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Laboratoire Magmas et Volcans (LMV), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement et la société-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA)-Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut des Sciences de la Terre (ISTerre), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Gustave Eiffel-Université Grenoble Alpes (UGA), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), European Synchrotron Radiation Facility (ESRF), and Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])

Subjects
High-pressure behavior, liquid density, Composition of the planets, light elements, [SDU]Sciences of the Universe [physics], Experimental mineralogy and petrology, X-ray, neutron and electron spectroscopy and diffraction, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Earth's core
Abstract

International audience; The density and structure of liquid Fe-C alloys have been measured up to 58 GPa and 3,200 K by in situ X-ray diffraction using a Paris-Edinburgh press and laser-heated diamond anvil cell. Study of the pressure evolution of the local structure inferred by X-ray diffraction measurements is important to understand the compression mechanism of the liquid. Obtained data show that the degree of compression is greater for the first coordination sphere than the second and third coordination spheres. The extrapolation of the measured density suggests that carbon cannot be the only light element alloyed to iron in the Earth's core, as 8-16 at % C (1.8-3.7 wt % C) would be necessary to explain the density deficit of the outer core relative to pure Fe. This concentration is too high to account for outer core velocity. The presence of other light elements (e.g., O, Si, S, and H) is thus required.

Published
2017
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results