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1. 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

2. First observations of core-transiting seismic phases on Mars.

Author: Irving, Jessica CE, Irving, Jessica CE, Lekić, Vedran, Durán, Cecilia, Drilleau, Mélanie, Kim, Doyeon, Rivoldini, Attilio, Khan, Amir, Samuel, Henri, Antonangeli, Daniele, Banerdt, William Bruce, Beghein, Caroline, Bozdağ, Ebru, Ceylan, Savas, Charalambous, Constantinos, Clinton, John, Davis, Paul, Garcia, Raphaël, Domenico Giardini, Horleston, Anna Catherine, Huang, Quancheng, Hurst, Kenneth J, Kawamura, Taichi, King, Scott D, Knapmeyer, Martin, Li, Jiaqi, Lognonné, Philippe, Maguire, Ross, Panning, Mark P, Plesa, Ana-Catalina, Schimmel, Martin, Schmerr, Nicholas C, Stähler, Simon C, Stutzmann, Eleonore, Xu, Zongbo, Irving, Jessica CE, Irving, Jessica CE, Lekić, Vedran, Durán, Cecilia, Drilleau, Mélanie, Kim, Doyeon, Rivoldini, Attilio, Khan, Amir, Samuel, Henri, Antonangeli, Daniele, Banerdt, William Bruce, Beghein, Caroline, Bozdağ, Ebru, Ceylan, Savas, Charalambous, Constantinos, Clinton, John, Davis, Paul, Garcia, Raphaël, Domenico Giardini, Horleston, Anna Catherine, Huang, Quancheng, Hurst, Kenneth J, Kawamura, Taichi, King, Scott D, Knapmeyer, Martin, Li, Jiaqi, Lognonné, Philippe, Maguire, Ross, Panning, Mark P, Plesa, Ana-Catalina, Schimmel, Martin, Schmerr, Nicholas C, Stähler, Simon C, Stutzmann, Eleonore, and Xu, Zongbo
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

3. 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

4. Empirical H/V spectral ratios at the InSight landing site and implications for the martian subsurface structure

Author: NASA Astrobiology Institute (US), Centre National D'Etudes Spatiales (France), California Institute of Technology, Carrasco, Sebastián, Knapmeyer‐Endrun, Brigitte, Margerin, Ludovic, Schmelzbach, C., Onodera, K., Pan, L., Lognonné, Philippe, Menina, Sabrina, Giardini, Domenico, Stutzmann, Eléonore, Clinton, John, Stähler, Simon C., Schimmel, Martin, Golombek, Matthew, Hobiger, Manuel, Hallo, Miroslav, Kedar, Sharon, Banerdt, William Bruce, NASA Astrobiology Institute (US), Centre National D'Etudes Spatiales (France), California Institute of Technology, Carrasco, Sebastián, Knapmeyer‐Endrun, Brigitte, Margerin, Ludovic, Schmelzbach, C., Onodera, K., Pan, L., Lognonné, Philippe, Menina, Sabrina, Giardini, Domenico, Stutzmann, Eléonore, Clinton, John, Stähler, Simon C., Schimmel, Martin, Golombek, Matthew, Hobiger, Manuel, Hallo, Miroslav, Kedar, Sharon, and Banerdt, William Bruce
Abstract: The horizontal-to-vertical (H/V) spectral ratio inversion is a traditional technique for deriving the local subsurface structure on Earth. We calculated the H/V from the ambient vibrations at different wind levels at the InSight landing site, on Mars, and also computed the H/V from the S-wave coda of the martian seismic events (marsquakes). Different H/V curves were obtained for different wind periods and from the marsquakes. From the ambient vibrations, the recordings during low-wind periods are close to the instrument self-noise level. During high-wind periods, the seismic recordings are highly contaminated by the interaction of the lander with the wind and the martian ground. Therefore, these recordings are less favourable for traditional H/V analysis. Instead, the recordings of the S-wave coda of marsquakes were preferred to derive the characteristic H/V curve of this site between 0.4 and 10 Hz. The final H/V curve presents a characteristic trough at 2.4 Hz and a strong peak at 8 Hz. Using a full diffuse wavefield approach as the forward computation and the Neighbourhood Algorithm as the sampling technique, we invert for the 1-D shear wave velocity structure at the InSight landing site. Based on our inversion results, we propose a strong site effect at the InSight site to be due to the presence of a shallow high-velocity layer (SHVL) over low-velocity units. The SHVL is likely placed below a layer of coarse blocky ejecta and can be associated with Early Amazonian basaltic lava flows. The units below the SHVL have lower velocities, possibly related to a Late Hesperian or Early Amazonian epoch with a different magmatic regime and/or a greater impact rate and more extensive weathering. An extremely weak buried low velocity layer (bLVL) between these lava flows explains the data around the 2.4 Hz trough, whereas a more competent bLVL would not generate this latter feature. These subsurface models are in good agreement with results from hammering experiment and compl
Published: 2023

5. 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

6. Monitoring microseismicity of the Hengill Geothermal Field in Iceland.

Author: Grigoli, Francesco, Grigoli, Francesco, Clinton, John F, Diehl, Tobias, Kaestli, Philipp, Scarabello, Luca, Agustsdottir, Thorbjorg, Kristjansdottir, Sigridur, Magnusson, Rognvaldur, Bean, Christopher J, Broccardo, Marco, Cesca, Simone, Dahm, Torsten, Hjorleifsdottir, Vala, Cabrera, Banu Mena, Milkereit, Claus, Nooshiri, Nima, Obermann, Anne, Racine, Roman, Rinaldi, Antonio Pio, Ritz, Vanille, Sanchez-Pastor, Pilar, Wiemer, Stefan, Grigoli, Francesco, Grigoli, Francesco, Clinton, John F, Diehl, Tobias, Kaestli, Philipp, Scarabello, Luca, Agustsdottir, Thorbjorg, Kristjansdottir, Sigridur, Magnusson, Rognvaldur, Bean, Christopher J, Broccardo, Marco, Cesca, Simone, Dahm, Torsten, Hjorleifsdottir, Vala, Cabrera, Banu Mena, Milkereit, Claus, Nooshiri, Nima, Obermann, Anne, Racine, Roman, Rinaldi, Antonio Pio, Ritz, Vanille, Sanchez-Pastor, Pilar, and Wiemer, Stefan
Abstract: Induced seismicity is one of the main factors that reduces societal acceptance of deep geothermal energy exploitation activities, and felt earthquakes are the main reason for closure of geothermal projects. Implementing innovative tools for real-time monitoring and forecasting of induced seismicity was one of the aims of the recently completed COSEISMIQ project. Within this project, a temporary seismic network was deployed in the Hengill geothermal region in Iceland, the location of the nation's two largest geothermal power plants. In this paper, we release raw continuous seismic waveforms and seismicity catalogues collected and prepared during this project. This dataset is particularly valuable since a very dense network was deployed in a seismically active region where thousand of earthquakes occur every year. For this reason, the collected dataset can be used across a broad range of research topics in seismology ranging from the development and testing of new data analysis methods to induced seismicity and seismotectonics studies.
Published: 2022

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

Author: Kawamura, Taichi, Grott, Matthias, Garcia, Raphael, Wieczorek, Mark, de Raucourt, Sebastien, Lognonne, Philippe, Bernauer, Felix, Breuer, Doris, Clinton, John, Delage, Pierre, Drilleau, Melanie, Ferraioli, Luigi, Fuji, Nobuaki, Horleston, Anna, Kletetschka, Gunther, Knapmeyer, Martin, Knapmeyer-Endrun, Brigitte, Padovan, Sebastiano, Plesa, Ana-Catalina, Rivoldini, Attilio, Robertsson, Johan, Rodriguez, Sebastien, Staehler, Simon C., Stutzmann, Eleonore, Teanby, Nicholas A., Tosi, Nicola, Vrettos, Christos, Banerdt, Bruce, Fa, Wenzhe, Huang, Qian, Irving, Jessica, Ishihara, Yoshiaki, Miljkovic, Katarina, Mittelholz, Anna, Nagihara, Seiichi, Neal, Clive, Qu, Shaobo, Schmerr, Nicholas, Tsuji, Takeshi, Kawamura, Taichi, Grott, Matthias, Garcia, Raphael, Wieczorek, Mark, de Raucourt, Sebastien, Lognonne, Philippe, Bernauer, Felix, Breuer, Doris, Clinton, John, Delage, Pierre, Drilleau, Melanie, Ferraioli, Luigi, Fuji, Nobuaki, Horleston, Anna, Kletetschka, Gunther, Knapmeyer, Martin, Knapmeyer-Endrun, Brigitte, Padovan, Sebastiano, Plesa, Ana-Catalina, Rivoldini, Attilio, Robertsson, Johan, Rodriguez, Sebastien, Staehler, Simon C., Stutzmann, Eleonore, Teanby, Nicholas A., Tosi, Nicola, Vrettos, Christos, Banerdt, Bruce, Fa, Wenzhe, Huang, Qian, Irving, Jessica, Ishihara, Yoshiaki, Miljkovic, Katarina, Mittelholz, Anna, Nagihara, Seiichi, Neal, Clive, Qu, Shaobo, Schmerr, Nicholas, and Tsuji, Takeshi
Abstract: Geophysical observations will provide key information about the inner structure of the planets and satellites and understanding the internal structure is a strong constraint on the bulk composition and thermal evolution of these bodies. Thus, geophysical observations are a key to uncovering the origin and evolution of the Moon. In this article, we propose the development of an autonomous lunar geophysical experiment package, composed of a suite of instruments and a central station with standardized interface, which can be installed on various future lunar missions. By fixing the interface between instruments and the central station, it would be possible to easily configure an appropriate experiment package for different missions. We describe here a series of geophysical instruments that may be included as part of the geophysical package: a seismometer, a magnetometer, a heat flow probe, and a laser reflector. These instruments will provide mechanical, thermal, and geodetic parameters of the Moon that are strongly related to the internal structure. We discuss the functionality required for future geophysical observations of the Moon, including the development of the central station that will be used commonly by different payloads.
Published: 2022

8. Empirical H/V spectral ratios at the InSight landing site and implications for the martian subsurface structure

Author: Carrasco, Sebastián, Knapmeyer-Endrun, Brigitte, Margerin, Ludovic, Schmelzbach, Cédric, Onodera, Keisuke, Pan, Lu, Lognonné, Philippe, Menina, Sabrina, Giardini, Domenico, Stutzmann, Eléonore, Clinton, John, Stähler, Simon, Schimmel, Martin, Golombek, Matthew, Hobiger, Manuel, Hallo, Miroslav, Kedar, Sharon, Banerdt, W. Bruce, Carrasco, Sebastián, Knapmeyer-Endrun, Brigitte, Margerin, Ludovic, Schmelzbach, Cédric, Onodera, Keisuke, Pan, Lu, Lognonné, Philippe, Menina, Sabrina, Giardini, Domenico, Stutzmann, Eléonore, Clinton, John, Stähler, Simon, Schimmel, Martin, Golombek, Matthew, Hobiger, Manuel, Hallo, Miroslav, Kedar, Sharon, and Banerdt, W. Bruce
Abstract: The horizontal-to-vertical (H/V) spectral ratio inversion is a traditional technique for deriving the local subsurface structure on Earth. We calculated the H/V from the ambient vibrations at different wind levels at the InSight landing site, on Mars, and also computed the H/V from the S-wave coda of the martian seismic events (marsquakes). Different H/V curves were obtained for different wind periods and from the marsquakes. From the ambient vibrations, the recordings during low-wind periods are close to the instrument self-noise level. During high-wind periods, the seismic recordings are highly contaminated by the interaction of the lander with the wind and the martian ground. Therefore, these recordings are less favourable for traditional H/V analysis. Instead, the recordings of the S-wave coda of marsquakes were preferred to derive the characteristic H/V curve of this site between 0.4 and 10 Hz. The final H/V curve presents a characteristic trough at 2.4 Hz and a strong peak at 8 Hz. Using a full diffuse wavefield approach as the forward computation and the Neighbourhood Algorithm as the sampling technique, we invert for the 1-D shear wave velocity structure at the InSight landing site. Based on our inversion results, we propose a strong site effect at the InSight site to be due to the presence of a shallow high-velocity layer (SHVL) over low-velocity units. The SHVL is likely placed below a layer of coarse blocky ejecta and can be associated with Early Amazonian basaltic lava flows. The units below the SHVL have lower velocities, possibly related to a Late Hesperian or Early Amazonian epoch with a different magmatic regime and/or a greater impact rate and more extensive weathering. An extremely weak buried low velocity layer (bLVL) between these lava flows explains the data around the 2.4 Hz trough, whereas a more competent bLVL would not generate this latter feature. These subsurface models are in good agreement with results from hammering experiment and compl
Published: 2022

9. Surface waves and crustal structure on Mars

Author: ETH Zurich, NASA Astrobiology Institute (US), Agence Nationale de la Recherche (France), UK Space Agency, California Institute of Technology, National Aeronautics and Space Administration (US), Kim, D., Banerdt, W. B., Ceylan, S., Giardini, Domenico, Lekic, Vedran, Lognonné, P., Beghein, C., Beucler, E., Carrasco, Sebastián, Charalambous, C., Clinton, John F., Drilleau, M., Duran, C., Golombek, M. P., Joshi, R., Khan, A., Knapmeyer‐Endrun, Brigitte, Li, J., Maguire, R., Pike, William T., Samuel, H., Schimmel, Martin, Schmerr, Nicholas C., Stähler, S. C., Stutzmann, E., Wieczorek, M., Xu, Z. D., Batov, A., Bozdag, E., Dahmen, N., Davis, P., Gudkova, T., Horleston, A., Huang, Quancheng, Kawamura, T., King, S., McLennan, S M, Nimmo, F., Plasman, M., Plesa, A. C., Stepanova, I. E., Weidner, E., Zenhäusern, Geraldine, Daubar, I., Fernando, B., García, R. F., Posiolova, L. V., Panning, Mark P., ETH Zurich, NASA Astrobiology Institute (US), Agence Nationale de la Recherche (France), UK Space Agency, California Institute of Technology, National Aeronautics and Space Administration (US), Kim, D., Banerdt, W. B., Ceylan, S., Giardini, Domenico, Lekic, Vedran, Lognonné, P., Beghein, C., Beucler, E., Carrasco, Sebastián, Charalambous, C., Clinton, John F., Drilleau, M., Duran, C., Golombek, M. P., Joshi, R., Khan, A., Knapmeyer‐Endrun, Brigitte, Li, J., Maguire, R., Pike, William T., Samuel, H., Schimmel, Martin, Schmerr, Nicholas C., Stähler, S. C., Stutzmann, E., Wieczorek, M., Xu, Z. D., Batov, A., Bozdag, E., Dahmen, N., Davis, P., Gudkova, T., Horleston, A., Huang, Quancheng, Kawamura, T., King, S., McLennan, S M, Nimmo, F., Plasman, M., Plesa, A. C., Stepanova, I. E., Weidner, E., Zenhäusern, Geraldine, Daubar, I., Fernando, B., García, R. F., Posiolova, L. V., and Panning, Mark P.
Abstract: We detected surface waves from two meteorite impacts on Mars. By measuring group velocity dispersion along the impact-lander path, we obtained a direct constraint on crustal structure away from the InSight lander. The crust north of the equatorial dichotomy had a shear wave velocity of approximately 3.2 kilometers per second in the 5- to 30-kilometer depth range, with little depth variation. This implies a higher crustal density than inferred beneath the lander, suggesting either compositional differences or reduced porosity in the volcanic areas traversed by the surface waves. The lower velocities and the crustal layering observed beneath the landing site down to a 10-kilometer depth are not a global feature. Structural variations revealed by surface waves hold implications for models of the formation and thickness of the martian crust.
Published: 2022

10. The Far Side of Mars: Two Distant Marsquakes Detected by InSight

Author: UK Space Agency, Agence Nationale de la Recherche (France), NASA Jet Propulsion Laboratory, Horleston, Anna C., Clinton, John F., Ceylan, S., Giardini, Domenico, Charalambous, C., Irving, Jessica C. E., Lognonné, P., Stähler, S. C., Zenhäusern, Geraldine, Dahmen, N. L., Duran, C., Kawamura, T., Khan, A., Kim, Doyeon, Plasman, Matthieu, Euchner, F., Beghein, Caroline, Beucler, E., Huang, Quancheng, Knapmeyer‐Endrun, Brigitte, Lekic, Vedran, Li, Jiaqi, Perrin, C., Schimmel, Martin, Schmerr, Nicholas C., Stott, A. E., Stutzmann, Éléonore, Teanby, Nicholas A., Xu, Zongbo, Panning, Mark, Banerdt, William B., UK Space Agency, Agence Nationale de la Recherche (France), NASA Jet Propulsion Laboratory, Horleston, Anna C., Clinton, John F., Ceylan, S., Giardini, Domenico, Charalambous, C., Irving, Jessica C. E., Lognonné, P., Stähler, S. C., Zenhäusern, Geraldine, Dahmen, N. L., Duran, C., Kawamura, T., Khan, A., Kim, Doyeon, Plasman, Matthieu, Euchner, F., Beghein, Caroline, Beucler, E., Huang, Quancheng, Knapmeyer‐Endrun, Brigitte, Lekic, Vedran, Li, Jiaqi, Perrin, C., Schimmel, Martin, Schmerr, Nicholas C., Stott, A. E., Stutzmann, Éléonore, Teanby, Nicholas A., Xu, Zongbo, Panning, Mark, and Banerdt, William B.
Abstract: For over three Earth years the Marsquake Service has been analyzing the data sent back from the Seismic Experiment for Interior Structure¿the seismometer placed on the surface of Mars by NASA¿s InSight lander. Although by October 2021, the Mars seismic catalog included 951 events, until recently all these events have been assessed as lying within a radius of 100° of InSight. Here we report two distant events that occurred within days of each other, located on the far side of Mars, giving us our first glimpse into Mars¿ core shadow zone. The first event, recorded on 25 August 2021 (InSight sol 976), shows clear polarized arrivals that we interpret to be PP and SS phases at low frequencies and locates to Valles Marineris, 146° ± 7° from InSight. The second event, occurring on 18 September 2021 (sol 1000), has significantly more broadband energy with emergent PP and SS arrivals, and a weak phase arriving before PP that we interpret as Pdiff¿. Considering uncertain pick times and poorly constrained travel times for Pdiff¿, we estimate this event is at a distance between 107° and 147° from InSight. With magnitudes of MMaw 4.2 and 4.1, respectively, these are the largest seismic events recorded so far on Mars.
Published: 2022

11. Tectonics of Cerberus Fossae unveiled by marsquakes

Author: Stähler, Simon C., Mittelholz, Anna, Perrin, Clément, Kawamura, Taichi, Kim, Doyeon, Knapmeyer, Martin, Zenhäusern, Géraldine, Clinton, John, Giardini, Domenico, Lognonné, Philippe, Banerdt, W. Bruce, Stähler, Simon C., Mittelholz, Anna, Perrin, Clément, Kawamura, Taichi, Kim, Doyeon, Knapmeyer, Martin, Zenhäusern, Géraldine, Clinton, John, Giardini, Domenico, Lognonné, Philippe, and Banerdt, W. Bruce
Abstract: The InSight mission has measured Mars' seismicity since February 2018 and has allowed to investigate tectonics on another planet. Seismic data shows that most of the widely distributed surface faults are not seismically active, and that seismicity is mostly originating from a single graben structure, the Cerberus Fossae. We show that both major families of marsquakes characterized by low and high frequency content, LF and HF events respectively, are located on central and eastern parts of this graben system. LF hypocenters are located at 15-50 km depth and the spectral character suggests a structurally weak, potentially warm source region consistent with recent volcanic activity at those depths. HF marsquakes occur in the brittle, shallow part of the crust and might originate in fault planes associated with the graben flanks. Estimated magnitudes are between 2.8 and 3.8, resulting in a total seismic moment release within Cerberus Fossae of 1.4-5.6 $\times10^{15}$ Nm/yr, or at least half of the observed value of the entire planet. Our findings confirm that Cerberus Fossae represents a unique tectonic setting shaped by current day volcanic processes, with implications for minimum local heat flow., Comment: 15 pages, 8 figures, Nature Astronomy (2022)
Published: 2022
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12. Potential Pitfalls in the Analysis and Structural Interpretation of Seismic Data from the Mars InSight Mission

Author: Kim, Doyeon, Davis, Paul, Lekic, Ved, Maguire, Ross, Compaire, Nicolas, Schimmel, Martin, Stutzmann, Eleonore, Irving, Jessica C. E., Lognonne, Philippe, Scholz, John-Robert, Clinton, John, Zenhaeusern, Geraldine, Dahmen, Nikolaj, Deng, Sizhuang, Levander, Alan, Panning, Mark P., Garcia, Raphael F., Giardini, Domenico, Hurst, Ken, Knapmeyer-Endrun, Brigitte, Nimmo, Francis, Pike, W. Tom, Pou, Laurent, Schmerr, Nicholas, Staehler, Simon C., Tauzin, Benoit, Widmer-Schnidrig, Rudolf, Banerdt, William B., Kim, Doyeon, Davis, Paul, Lekic, Ved, Maguire, Ross, Compaire, Nicolas, Schimmel, Martin, Stutzmann, Eleonore, Irving, Jessica C. E., Lognonne, Philippe, Scholz, John-Robert, Clinton, John, Zenhaeusern, Geraldine, Dahmen, Nikolaj, Deng, Sizhuang, Levander, Alan, Panning, Mark P., Garcia, Raphael F., Giardini, Domenico, Hurst, Ken, Knapmeyer-Endrun, Brigitte, Nimmo, Francis, Pike, W. Tom, Pou, Laurent, Schmerr, Nicholas, Staehler, Simon C., Tauzin, Benoit, Widmer-Schnidrig, Rudolf, and Banerdt, William B.
Abstract: The Seismic Experiment for Interior Structure (SEIS) of the InSight mission to Mars has been providing direct information on Martian interior structure and dynamics of that planet since it landed. Compared with seismic recordings on the Earth, ground-motion measurements acquired by SEIS on Mars are not only made under dramatically different ambient noise conditions, but also include idiosyncratic signals that arise from coupling between different InSight sensors and spacecraft components. This work is to synthesize what is known about these signal types, illustrate how they can manifest in waveforms and noise correlations, and present pitfalls in structural interpretations based on standard seismic analysis methods. We show that glitches (a type of prominent transient signal) can produce artifacts in ambient noise correlations. Sustained signals that vary in frequency, such as lander modes that are affected by variations in temperature and wind conditions over the course of the Martian sol, can also contaminate ambient noise results. Therefore, both types of signals have the potential to bias interpretation in terms of subsurface layering. We illustrate that signal processing in the presence of identified nonseismic signals must be informed by an understanding of the underlying physical processes in order for high-fidelity waveforms of ground motion to be extracted. Whereas the origins of the most idiosyncratic signals are well understood, the 2.4 Hz resonance remains debated, and the literature does not contain an explanation of its fine spectral structure. Even though the selection of idiosyncratic signal types discussed in this article may not be exhaustive, we provide guidance on the best practices for enhancing the robustness of structural interpretations.
Published: 2021

13. Resonances of the InSight Seismometer on Mars

Author: Hurst, Kenneth, Fayon, Lucile, Knapmeyer-Endrun, Brigitte, Schmelzbach, Cedric, van Driel, Martin, Ervin, Joan, Kedar, Sharon, Pike, William T., Calcutt, Simon, Warren, Tristram, Charalambous, Constantino, Stott, Alexander, Bierwirth, Marco, Lognonne, Philippe, de Raucourt, Sebastien, Gabsi, Taoufik, Nebut, Tanguy, Robert, Oliver, Tillier, Sylvain, Ceylan, Savas, Bose, Maren, Clinton, John, Giardini, Domenico, Horleston, Anna, Kawamura, Taichi, Khan, Amir, Orhand-Mainsant, Guenole, Scholz, John-Robert, Stahler, Simon, Stevanovic, Jennifer, Banerdt, William B., Hurst, Kenneth, Fayon, Lucile, Knapmeyer-Endrun, Brigitte, Schmelzbach, Cedric, van Driel, Martin, Ervin, Joan, Kedar, Sharon, Pike, William T., Calcutt, Simon, Warren, Tristram, Charalambous, Constantino, Stott, Alexander, Bierwirth, Marco, Lognonne, Philippe, de Raucourt, Sebastien, Gabsi, Taoufik, Nebut, Tanguy, Robert, Oliver, Tillier, Sylvain, Ceylan, Savas, Bose, Maren, Clinton, John, Giardini, Domenico, Horleston, Anna, Kawamura, Taichi, Khan, Amir, Orhand-Mainsant, Guenole, Scholz, John-Robert, Stahler, Simon, Stevanovic, Jennifer, and Banerdt, William B.
Abstract: (InSight) seismometer was deployed to the surface of Mars in December 2018- February 2019. The specific deployment conditions, which are very different from those of a standard broadband instrument on the Earth, result in resonances caused by different parts of the sensor assembly (SA) that are recorded by the seismometer. Here, we present and characterize the resonances known to be present in the SA and their causes to aid interpretation of the seismic signals observed on Mars. Briefly, there are resonances in the SA at about 2.9, 5.3, 9.5, 12, 14, 23-28, and 51 Hz. We discuss various methods and tests that were used to characterize these resonances, and provide evidence for some of them in data collected on Mars. In addition to their relevance for the high frequency analysis of seismic data from InSight, specifically for phase measurements near the resonant frequencies, the tests and observations described here are also of potential use in the further development of planetary seismometers, for example, for Mars, the
Published: 2021

14. First Focal Mechanisms of Marsquakes

Author: Brinkman, Nienke, Stahler, Simon C., Giardini, Domenico, Schmelzbach, Cedric, Khan, Amir, Jacob, Alice, Fuji, Nobuaki, Perrin, Clement, Lognonne, Philippe, Beucler, Eric, Bose, Maren, Ceylan, Savas, Charalambous, Constantinos, Clinton, John F., van Driel, Martin, Euchner, Fabian, Horleston, Anna, Kawamura, Taichi, Knapmeyer-Endrun, Brigitte, Mainsant, Guenole, Panning, Mark P., Pike, William T., Scholz, John-Robert, Robertsson, Johan O. A., Banerdt, William B., Brinkman, Nienke, Stahler, Simon C., Giardini, Domenico, Schmelzbach, Cedric, Khan, Amir, Jacob, Alice, Fuji, Nobuaki, Perrin, Clement, Lognonne, Philippe, Beucler, Eric, Bose, Maren, Ceylan, Savas, Charalambous, Constantinos, Clinton, John F., van Driel, Martin, Euchner, Fabian, Horleston, Anna, Kawamura, Taichi, Knapmeyer-Endrun, Brigitte, Mainsant, Guenole, Panning, Mark P., Pike, William T., Scholz, John-Robert, Robertsson, Johan O. A., and Banerdt, William B.
Abstract: Since February 2019, NASA's InSight lander is recording seismic signals on the planet Mars, which, for the first time, allows to observe ongoing tectonic processes with geophysical methods. A number of Marsquakes have been located in the Cerberus Fossae graben system in Elysium Planitia and further west, in the Orcus Patera depression. We present a first study of the focal mechanisms of three well-recorded events (S0173a, S0183a, S0235b) to determine the processes dominating in the source region. We infer for all three events a predominantly extensional setting. Our method is adapted to the case of a single, multicomponent receiver and based on fitting waveforms of P and S waves against synthetic seismograms computed for the initial crustal velocity model derived by the InSight team. We explore the uncertainty due to the single-station limitation and find that even data recorded by one station constrains the mechanisms (reasonably) well. For the events in the Cerberus Fossae region (S0173a, S0235b) normal faulting with a relatively steep dipping fault plane is inferred, suggesting an extensional regime mainly oriented E-W to NE-SW. The fault regime in the Orcus Patera region is not determined uniquely because only the P wave can be used for the source inversion. However, we find that the P and weak S waves of the S0183a event show similar polarities to the event S0173, which indicates similar fault regimes.
Published: 2021

15. High-Resolution Crustal S-wave Velocity Model and Moho Geometry Beneath the Southeastern Alps: New Insights From the SWATH-D Experiment

Author: Sadeghi-Bagherabadi, Amir, Vuan, Alessandro, Aoudia, Abdelkrim, Parolai, Stefano, Hetényi, György, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Bokelmann, Götz, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Hein , Gerrit, Bianchi, Irene, Sadeghi-Bagherabadi, Amir, Vuan, Alessandro, Aoudia, Abdelkrim, Parolai, Stefano, Hetényi, György, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Bokelmann, Götz, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Hein , Gerrit, and Bianchi, Irene
Abstract: We compiled a dataset of continuous recordings from the temporary and permanent seismic networks to compute the high-resolution 3D S-wave velocity model of the Southeastern Alps, the western part of the external Dinarides, and the Friuli and Venetian plains through ambient noise tomography. Part of the dataset is recorded by the SWATH-D temporary network and permanent networks in Italy, Austria, Slovenia and Croatia between October 2017 and July 2018. We computed 4050 vertical component cross-correlations to obtain the empirical Rayleigh wave Green’s functions. The dataset is complemented by adopting 1804 high-quality correlograms from other studies. The fast-marching method for 2D surface wave tomography is applied to the phase velocity dispersion curves in the 2–30 s period band. The resulting local dispersion curves are inverted for 1D S-wave velocity profiles using the non-perturbational and perturbational inversion methods. We assembled the 1D S-wave velocity profiles into a pseudo-3D S-wave velocity model from the surface down to 60 km depth. A range of iso-velocities, representing the crystalline basement depth and the crustal thickness, are determined. We found the average depth over the 2.8–3.0 and 4.1–4.3 km/s iso-velocity ranges to be reasonable representations of the crystalline basement and Moho depths, respectively. The basement depth map shows that the shallower crystalline basement beneath the Schio-Vicenza fault highlights the boundary between the deeper Venetian and Friuli plains to the east and the Po-plain to the west. The estimated Moho depth map displays a thickened crust along the boundary between the Friuli plain and the external Dinarides. It also reveals a N-S narrow corridor of crustal thinning to the east of the junction of Giudicarie and Periadriatic lines, which was not reported by other seismic imaging studies. This corridor of shallower Moho is located beneath the surface outcrop of the Permian magmatic rocks and seems to be connected
Published: 2021
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16. Crustal Thinning From Orogen to Back-Arc Basin: The Structure of the Pannonian Basin Region Revealed by P-to-S Converted Seismic Waves

Author: Kalmar, Daniel, Hetényi, György, Balazs, Attila, Bondar, Istvan, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Bianchi, Irene, Bokelmann, Götz, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Kalmar, Daniel, Hetényi, György, Balazs, Attila, Bondar, Istvan, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Bianchi, Irene, Bokelmann, Götz, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, and Žlebčíková, Helena
Abstract: We present the results of P-to-S receiver function analysis to improve the 3D image of the sedimentary layer, the upper crust, and lower crust in the Pannonian Basin area. The Pannonian Basin hosts deep sedimentary depocentres superimposed on a complex basement structure and it is surrounded by mountain belts. We processed waveforms from 221 three-component broadband seismological stations. As a result of the dense station coverage, we were able to achieve so far unprecedented spatial resolution in determining the velocity structure of the crust. We applied a three-fold quality control process; the first two being applied to the observed waveforms and the third to the calculated radial receiver functions. This work is the first comprehensive receiver function study of the entire region. To prepare the inversions, we performed station-wise H-Vp/Vs grid search, as well as Common Conversion Point migration. Our main focus was then the S-wave velocity structure of the area, which we determined by the Neighborhood Algorithm inversion method at each station, where data were sub-divided into back-azimuthal bundles based on similar Ps delay times. The 1D, nonlinear inversions provided the depth of the discontinuities, shear-wave velocities and Vp/Vs ratios of each layer per bundle, and we calculated uncertainty values for each of these parameters. We then developed a 3D interpolation method based on natural neighbor interpolation to obtain the 3D crustal structure from the local inversion results. We present the sedimentary thickness map, the first Conrad depth map and an improved, detailed Moho map, as well as the first upper and lower crustal thickness maps obtained from receiver function analysis. The velocity jump across the Conrad discontinuity is estimated at less than 0.2 km/s over most of the investigated area. We also compare the new Moho map from our approach to simple grid search results and prior knowledge from other techniques. Our Moho depth map presents local
Published: 2021
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17. Shear wave splitting in the Alpine region

Author: Hein, Gerrit, Kolínský, Petr, Bianchi, Irene, Bokelmann, Götz, Hetényi, György, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Hein, Gerrit, Kolínský, Petr, Bianchi, Irene, Bokelmann, Götz, Hetényi, György, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, and Žlebčíková, Helena
Abstract: To constrain seismic anisotropy under and around the Alps in Europe, we study SKS shear wave splitting from the region densely covered by the AlpArray seismic network. We apply a technique based on measuring the splitting intensity, constraining well both the fast orientation and the splitting delay. Four years of teleseismic earthquake data were processed, from 723 temporary and permanent broad-band stations of the AlpArray deployment including ocean-bottom seismometers, providing a spatial coverage that is unprecedented. The technique is applied automatically (without human intervention), and it thus provides a reproducible image of anisotropic structure in and around the Alpine region. As in earlier studies, we observe a coherent rotation of fast axes in the western part of the Alpine chain, and a region of homogeneous fast orientation in the Central Alps. The spatial variation of splitting delay times is particularly interesting though. On one hand, there is a clear positive correlation with Alpine topography, suggesting that part of the seismic anisotropy (deformation) is caused by the Alpine orogeny. On the other hand, anisotropic strength around the mountain chain shows a distinct contrast between the Western and Eastern Alps. This difference is best explained by the more active mantle flow around the Western Alps. The new observational constraints, especially the splitting delay, provide new information on Alpine geodynamics.
Published: 2021
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18. Transversely isotropic lower crust of Variscan central Europe imaged by ambient noise tomography of the Bohemian Massif

Author: Kvapil, J., Plomerova, J., Kampfova Exnerova, H., Babuska, V., Hetenyi, G., Abreu , Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Bokelmann, Götz, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Kvapil, J., Plomerova, J., Kampfova Exnerova, H., Babuska, V., Hetenyi, G., Abreu , Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Bokelmann, Götz, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, and Žlebčíková, Helena
Abstract: The recent development of ambient noise tomography, in combination with the increasing number of permanent seismic stations and dense networks of temporary stations operated during passive seismic experiments, provides a unique opportunity to build the first high-resolution 3-D shear wave velocity (vS) model of the entire crust of the Bohemian Massif (BM). This paper provides a regional-scale model of velocity distribution in the BM crust. The velocity model with a cell size of 22 km is built using a conventional two-step inversion approach from Rayleigh wave group velocity dispersion curves measured at more than 400 stations. The shear velocities within the upper crust of the BM are ∼0.2 km s−1 higher than those in its surroundings. The highest crustal velocities appear in its southern part, the Moldanubian unit. The Cadomian part of the region has a thinner crust, whereas the crust assembled, or tectonically transformed in the Variscan period, is thicker. The sharp Moho discontinuity preserves traces of its dynamic development expressed in remnants of Variscan subductions imprinted in bands of crustal thickening. A significant feature of the presented model is the velocity-drop interface (VDI) modelled in the lower part of the crust. We explain this feature by the anisotropic fabric of the lower crust, which is characterised as vertical transverse isotropy with the low velocity being the symmetry axis. The VDI is often interrupted around the boundaries of the crustal units, usually above locally increased velocities in the lowermost crust. Due to the north-west–south-east shortening of the crust and the late-Variscan strike-slip movements along the north-east–south-west oriented sutures preserved in the BM lithosphere, the anisotropic fabric of the lower crust was partly or fully erased along the boundaries of original microplates. These weakened zones accompanied by a velocity increase above the Moho (which indicate an emplacement of mantle rocks into the lower c
Published: 2021
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19. Relocation of earthquakes in the southern and eastern Alps (Austria, Italy) recorded by the dense, temporary SWATH-D network using a Markov chain Monte Carlo inversion

Author: Jozi Najafabadi, A., Haberland, Christian, Ryberg, Trond, Verwater, V. F., Le Breton, E., Handy, M. R., Weber, Michael, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Bokelmann, Götz, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Abreu, Rafael, Allegretti, Ivo, Al-Halbouni, Djamil, Jozi Najafabadi, A., Haberland, Christian, Ryberg, Trond, Verwater, V. F., Le Breton, E., Handy, M. R., Weber, Michael, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Bokelmann, Götz, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Abreu, Rafael, Allegretti, Ivo, and Al-Halbouni, Djamil
Abstract: In this study, we analyzed a large seismological dataset from temporary and permanent networks in the southern and eastern Alps to establish high-precision hypocenters and 1-D VP and VP/VS models. The waveform data of a subset of local earthquakes with magnitudes in the range of 1–4.2 ML were recorded by the dense, temporary SWATH-D network and selected stations of the AlpArray network between September 2017 and the end of 2018. The first arrival times of P and S waves of earthquakes are determined by a semi-automatic procedure. We applied a Markov chain Monte Carlo inversion method to simultaneously calculate robust hypocenters, a 1-D velocity model, and station corrections without prior assumptions, such as initial velocity models or earthquake locations. A further advantage of this method is the derivation of the model parameter uncertainties and noise levels of the data. The precision estimates of the localization procedure is checked by inverting a synthetic travel time dataset from a complex 3-D velocity model and by using the real stations and earthquakes geometry. The location accuracy is further investigated by a quarry blast test. The average uncertainties of the locations of the earthquakes are below 500 m in their epicenter and ∼ 1.7 km in depth. The earthquake distribution reveals seismicity in the upper crust (0–20 km), which is characterized by pronounced clusters along the Alpine frontal thrust, e.g., the Friuli-Venetia (FV) region, the Giudicarie–Lessini (GL) and Schio-Vicenza domains, the Austroalpine nappes, and the Inntal area. Some seismicity also occurs along the Periadriatic Fault. The general pattern of seismicity reflects head-on convergence of the Adriatic indenter with the Alpine orogenic crust. The seismicity in the FV and GL regions is deeper than the modeled frontal thrusts, which we interpret as indication for southward propagation of the southern Alpine deformation front (blind thrusts).
Published: 2021
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20. Seismicity and seismotectonics of the Albstadt Shear Zone in the northern Alpine foreland

Author: Mader, Sarah, Ritter, Joachim R. R., Reicherter, Klaus, Bokelmann, Götz, Hetényi, György, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Mader, Sarah, Ritter, Joachim R. R., Reicherter, Klaus, Bokelmann, Götz, Hetényi, György, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, and Žlebčíková, Helena
Abstract: The region around the town Albstadt, SW Germany, was struck by four damaging earthquakes with magnitudes greater than 5 during the last century. These earthquakes occurred along the Albstadt Shear Zone (ASZ), which is characterized by more or less continuous microseismicity. As there are no visible surface ruptures that may be connected to the fault zone, we study its characteristics by its seismicity distribution and faulting pattern. We use the earthquake data of the state earthquake service of Baden-Württemberg from 2011 to 2018 and complement it with additional phase picks beginning in 2016 at the AlpArray and StressTransfer seismic networks in the vicinity of the ASZ. This extended data set is used to determine new minimum 1-D seismic vp and vs velocity models and corresponding station delay times for earthquake relocation. Fault plane solutions are determined for selected events, and the principal stress directions are derived. The minimum 1-D seismic velocity models have a simple and stable layering with increasing velocity with depth in the upper crust. The corresponding station delay times can be explained well by the lateral depth variation of the crystalline basement. The relocated events align about north–south with most of the seismic activity between the towns of Tübingen and Albstadt, east of the 9∘ E meridian. The events can be separated into several subclusters that indicate a segmentation of the ASZ. The majority of the 25 determined fault plane solutions feature an NNE–SSW strike but NNW–SSE-striking fault planes are also observed. The main fault plane associated with the ASZ dips steeply, and the rake indicates mainly sinistral strike-slip, but we also find minor components of normal and reverse faulting. The determined direction of the maximum horizontal stress of 140–149∘ is in good agreement with prior studies. Down to ca. 7–8 km depth SHmax is bigger than SV; below this depth, SV is the main stress component. The direction of SHmax indicates
Published: 2021
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21. Shear-wave velocity structure beneath the Dinarides from the inversion of Rayleigh-wave dispersion

Author: Belinic, Tena, Kolínský, Petr, Stipčević, Josip, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Bianchi, Irene, Bokelmann, Götz, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Belinic, Tena, Kolínský, Petr, Stipčević, Josip, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Bianchi, Irene, Bokelmann, Götz, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, and Žlebčíková, Helena
Abstract: Highlights • Rayleigh-wave phase velocity in the wider Dinarides region using the two-station method. • Uppermost mantle shear-wave velocity model of the Dinarides-Adriatic Sea region. • Velocity model reveals a robust high-velocity anomaly present under the whole Dinarides. • High-velocity anomaly reaches depth of 160 km in the northern Dinarides to more than 200 km under southern Dinarides. • New structural model incorporating delamination as one of the processes controlling the continental collision in the Dinarides. The interaction between the Adriatic microplate (Adria) and Eurasia is the main driving factor in the central Mediterranean tectonics. Their interplay has shaped the geodynamics of the whole region and formed several mountain belts including Alps, Dinarides and Apennines. Among these, Dinarides are the least investigated and little is known about the underlying geodynamic processes. There are numerous open questions about the current state of interaction between Adria and Eurasia under the Dinaric domain. One of the most interesting is the nature of lithospheric underthrusting of Adriatic plate, e.g. length of the slab or varying slab disposition along the orogen. Previous investigations have found a low-velocity zone in the uppermost mantle under the northern-central Dinarides which was interpreted as a slab gap. Conversely, several newer studies have indicated the presence of the continuous slab under the Dinarides with no trace of the low velocity zone. Thus, to investigate the Dinaric mantle structure further, we use regional-to-teleseismic surface-wave records from 98 seismic stations in the wider Dinarides region to create a 3D shear-wave velocity model. More precisely, a two-station method is used to extract Rayleigh-wave phase velocity while tomography and 1D inversion of the phase velocity are employed to map the depth dependent shear-wave velocity. Resulting velocity model reveals a robust high-velocity anomaly present under the whole Dinar
Published: 2021
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22. Evidence for radial anisotropy in the lower crust of the Apennines from Bayesian ambient noise tomography in Europe

Author: Alder, C., Debayle, E., Bodin, T., Paul, A., Stehly, L., Pedersen, H., Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Abreu, Rafael, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Hein, Gerrit, Bianchi, Irene, Bokelmann, Götz, Hetényi, György, Alder, C., Debayle, E., Bodin, T., Paul, A., Stehly, L., Pedersen, H., Allegretti, Ivo, Apoloner, Maria-Theresia, Aubert, Coralie, Besançon, Simon, Bés de Berc, Maxime, Abreu, Rafael, Brunel, Didier, Capello, Marco, Čarman, Martina, Cavaliere, Adriano, Chéze, Jérôme, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, C. Crawford, Wayne, Cristiano, Luigia, Czifra, Tibor, D’Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasović, Iva, Deschamps, Anne, Dessa, Jean-Xavier, Doubre, Cécile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Gráczer, Zoltán, Gröschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jarić, Dejan, Jedlička, Petr, Jia, Yan, Jund, Hélène, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kolínský, Petr, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kühne, Lothar, Kuk, Krešo, Lange, Dietrich, Loos, Jürgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Métral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Péquegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerová, Jaroslava, Pondrelli, Silvia, Prevolnik, Snježan, Racine, Roman, Régnier, Marc, Reiss, Miriam, Ritter, Joachim, Rümpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-Kortnack, Detlef, Šipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipčević, Josip, Strollo, Angelo, Süle, Bálint, Szanyi, Gyöngyvér, Szűcs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Luděk, Voigt, René, Wassermann, Joachim, Wéber, Zoltán, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix Noah, Wolyniec, David, Zieke, Thomas, Živčić, Mladen, Žlebčíková, Helena, Hein, Gerrit, Bianchi, Irene, Bokelmann, Götz, and Hetényi, György
Abstract: Probing seismic anisotropy of the lithosphere provides valuable clues on the fabric of rocks. We present a 3-D probabilistic model of shear wave velocity and radial anisotropy of the crust and uppermost mantle of Europe, focusing on the mountain belts of the Alps and Apennines. The model is built from Love and Rayleigh dispersion curves in the period range 5–149 s. Data are extracted from seismic ambient noise recorded at 1521 broad-band stations, including the AlpArray network. The dispersion curves are first combined in a linearized least squares inversion to obtain 2-D maps of group velocity at each period. Love and Rayleigh maps are then jointly inverted at depth for shear wave velocity and radial anisotropy using a Bayesian Monte Carlo scheme that accounts for the trade-off between radial anisotropy and horizontal layering. The isotropic part of our model is consistent with previous studies. However, our anisotropy maps differ from previous large scale studies that suggested the presence of significant radial anisotropy everywhere in the European crust and shallow upper mantle. We observe instead that radial anisotropy is mostly localized beneath the Apennines while most of the remaining European crust and shallow upper mantle is isotropic. We attribute this difference to trade-offs between radial anisotropy and thin (hectometric) layering in previous studies based on least-squares inversions and long period data (>30 s). In contrast, our approach involves a massive data set of short period measurements and a Bayesian inversion that accounts for thin layering. The positive radial anisotropy (VSH > VSV) observed in the lower crust of the Apennines cannot result from thin layering. We rather attribute it to ductile horizontal flow in response to the recent and present-day extension in the region.
Published: 2021
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23. 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

24. The Polarization of Ambient Noise on Mars

Author: Stutzmann, E., Schimmel, Martin, Lognonné, P., Horleston, Anna, Ceylan, S., van Driel, M., Stahler, Simon, Banerdt, B., Calvet, Marie, Charalambous, C., Clinton, John F., Drilleau, M., Fayon, Lucile, García, Raphael, Jacob, A., Kawamura, T., Kenda, B., Margerin, Ludovic, Murdoch, N., Panning, Mark, Stutzmann, E., Schimmel, Martin, Lognonné, P., Horleston, Anna, Ceylan, S., van Driel, M., Stahler, Simon, Banerdt, B., Calvet, Marie, Charalambous, C., Clinton, John F., Drilleau, M., Fayon, Lucile, García, Raphael, Jacob, A., Kawamura, T., Kenda, B., Margerin, Ludovic, Murdoch, N., and Panning, Mark
Abstract: Seismic noise recorded at the surface of Mars has been monitored since February 2019, using the InSight seismometers.This noise can reach -200 dB and is 500 times lower than on Earth at night and it increases of 30 dB during the day. We analyze its polarization as a function of time and frequency in the band 0.03-1Hz. We use the degree of polarization to extract signals with stable polarization independent of their amplitude and type of polarization. We detect polarized signals at all frequencies and all times. Glitches correspond to linear polarized signals which are more abundant during the night. For signals with elliptical polarization, the ellipse is in the horizontal plane below 0.3 Hz (LF). Above 0.3 Hz (HF) and except in the evening, the ellipse is in the vertical plane and the major axis is tilted. While polarization azimuths are different in the two frequency bands, they both vary as a function of local hour and season. They are also correlated with wind direction, particularly during the daytime. We investigate possible aseismic and seismic origins of the polarized signals. Lander or tether noise can be discarded. Pressure fluctuations transported by wind may explain part of the HF polarization but not the tilt of the ellipse. This tilt can be obtained if the source is an acoustic emission coming from high altitude at critical angle. Finally, in the evening when the wind is low, the polarized signals may correspond to the seismic wavefield of the Mars background noise.
Published: 2021

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

Author: Swiss National Science Foundation, Agence Nationale de la Recherche (France), Swiss National Supercomputing Centre, UK Space Agency, Centre National D'Etudes Spatiales (France), ETH Zurich, State Secretariat for Education, Research and Innovation (Switzerland), Schimmel, Martin [0000-0003-2601-4462], Ceylan, S., Clinton, John F., Giardini, Domenico, Böse, M., Charalambous, C., van Driel, M., Horleston, A., Kawamura, T., Khan, A., Orhand-Mainsant, Guenolé, Scholz, J. R., Stahler, S. C., Euchner, F., Banerdt, W. B., Lognonné, P., Banfield, D., Beucler, E., Garcia, R. F., Kedar, S., Panning, M.P., Pike, William T., Smrekar, S. E., Spiga, A., Dahmen, N. L., Hurst, K., Stott, A. E., Lorenz, R. D., Schimmel, Martin, Stutzmann, E., ten Pierick, J., Conejero, Vicente, Pardo, C., Perrin, C., Swiss National Science Foundation, Agence Nationale de la Recherche (France), Swiss National Supercomputing Centre, UK Space Agency, Centre National D'Etudes Spatiales (France), ETH Zurich, State Secretariat for Education, Research and Innovation (Switzerland), Schimmel, Martin [0000-0003-2601-4462], Ceylan, S., Clinton, John F., Giardini, Domenico, Böse, M., Charalambous, C., van Driel, M., Horleston, A., Kawamura, T., Khan, A., Orhand-Mainsant, Guenolé, Scholz, J. R., Stahler, S. C., Euchner, F., Banerdt, W. B., Lognonné, P., Banfield, D., Beucler, E., Garcia, R. F., Kedar, S., Panning, M.P., Pike, William T., Smrekar, S. E., Spiga, A., Dahmen, N. L., Hurst, K., Stott, A. E., Lorenz, R. D., Schimmel, Martin, Stutzmann, E., ten Pierick, J., Conejero, Vicente, Pardo, C., and Perrin, C.
Abstract: The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed on the surface of Mars on November 26, 2018. One of the scientific instruments in the payload that is essential to the mission is the SEIS package (Seismic Experiment for Interior Structure) which includes a very broadband and a short period seismometer. More than one year since the landing, SEIS continues to be fully operational and has been collecting an exceptional data set which contains not only the signals of seismic origins, but also noise and artifacts induced by the martian environment, the hardware on the ground that includes the seismic sensors, and the programmed operational activities of the lander. Many of these non-seismic signals will be unfamiliar to the scientific community. In addition, many of these signals have signatures that may resemble seismic events either or both in time and frequency domains. Here, we report our observations of common non-seismic signals as seen during the first 478 sols of the SEIS data, i.e. from landing until the end of March 2020. This manuscript is intended to provide a guide to scientists who use the data recorded on SEIS, detailing the general attributes of the most commonly observed non-seismic features. It will help to clarify the characteristics of the seismic dataset for future research, and to avoid misinterpretations when searching for marsquakes.
Published: 2021

26. The Polarization of Ambient Noise on Mars

Author: Agence Nationale de la Recherche (France), UK Space Agency, Ministerio de Ciencia, Innovación y Universidades (España), Schimmel, Martin [0000-0003-2601-4462], Stutzmann, E., Schimmel, Martin, Lognonné, P., Horleston, A., Ceylan, S., van Driel, M., Stähler, S., Banerdt, B., Calvet, M., Charalambous, C., Clinton, John F., Drilleau, M., Fayon, L., Garcia, R. F., Giardini, Domenico, Hurst, K., Jacob, A., Kawamura, T., Kenda, B., Margerin, L., Murdoch, N., Panning, M., Pike, T., Scholz, J. R., Spiga, A., Agence Nationale de la Recherche (France), UK Space Agency, Ministerio de Ciencia, Innovación y Universidades (España), Schimmel, Martin [0000-0003-2601-4462], Stutzmann, E., Schimmel, Martin, Lognonné, P., Horleston, A., Ceylan, S., van Driel, M., Stähler, S., Banerdt, B., Calvet, M., Charalambous, C., Clinton, John F., Drilleau, M., Fayon, L., Garcia, R. F., Giardini, Domenico, Hurst, K., Jacob, A., Kawamura, T., Kenda, B., Margerin, L., Murdoch, N., Panning, M., Pike, T., Scholz, J. R., and Spiga, A.
Abstract: Seismic noise recorded at the surface of Mars has been monitored since February 2019, using the InSight seismometers. This noise can reach -200 dB. It is 500 times lower than on Earth at night and it increases of 30 dB during the day. We analyze its polarization as a function of time and frequency in the band 0.03-1 Hz. We use the degree of polarization to extract signals with stable polarization independent of their amplitude and type of polarization. We detect polarized signals at all frequencies and all times. Glitches correspond to linear polarized signals which are more abundant during the night. For signals with elliptical polarization, the ellipse is in the horizontal plane below 0.3 Hz. In the 0.3-1Hz high frequency band (HF) and except in the evening, the ellipse is in the vertical plane and the major axis is tilted. While polarization azimuths are different in the two frequency bands, they both vary as a function of local hour and season. They are also correlated with wind direction, particularly during the daytime. We investigate possible aseismic and seismic origins of the polarized signals. Lander or tether noise can be discarded. Pressure fluctuations transported by wind may explain part of the HF polarization but not the tilt of the ellipse. This tilt can be obtained if the source is an acoustic emission coming from high altitude at critical angle. Finally, in the evening when the wind is low, the measured polarized signals may correspond to the seismic wavefield of the Mars background noise. Plain Language Summary Seismic noise at the surface of Mars was unknown until the first measurements by the seismometers from the InSight mission in January 2019. On Earth, the microseismic noise (0.05-1 Hz) is composed dominantly of surface waves generated by the numerous sources related to ocean wave activities. On Mars, because there is no ocean, seismic noise is down to 500 times lower than on Earth reaching -200 dB in acceleration at night. In order to deter
Published: 2021

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., InSight, Science Team, 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

28. Earthquakes in Switzerland and surrounding regions during 2014

Author: Diehl, Tobias, Deichmann, Nicolas, Clinton, John, Kästli, Philipp, Cauzzi, Carlo, Kraft, Toni, Behr, Yannik, Edwards, Benjamin, Guilhem, Aurélie, Korger, Edith, Hobiger, Manuel, Haslinger, Florian, Fäh, Donat, Wiemer, Stefan, Diehl, Tobias, Deichmann, Nicolas, Clinton, John, Kästli, Philipp, Cauzzi, Carlo, Kraft, Toni, Behr, Yannik, Edwards, Benjamin, Guilhem, Aurélie, Korger, Edith, Hobiger, Manuel, Haslinger, Florian, Fäh, Donat, and Wiemer, Stefan
Abstract: During 2014, 817 earthquakes and 180 quarry blasts were detected and located in the region under consideration. An additional 160 earthquakes with ML≤1.0 were located using supplementary analysis techniques. The number of located earthquakes in 2014 was the largest since the installation of a seismic network in Switzerland in 1975. This unusually large number is mainly due to the occurrence of two vigorous earthquake sequences, and the local reduction of the earthquake detection thresholds of the Swiss seismic network. With a total of 22 earthquakes of ML≥2.5, the seismic activity of larger and potentially felt events was close to the average of 23 earthquakes over the previous 39years. The most noteworthy seismicity was the earthquake sequence near Diemtigen, west of Lake Thun, where more than 270 events were located between April and December. High-precision hypocenter relocation was applied to image the spatio-temporal evolution of this seismicity. The sequence culminated in an M L 3.2 event in October, which was felt in the region of Lake Thun and Bern. Other cases of earthquakes felt by the public include earthquakes in the region of Biel (ML 3.2), in Vallorcine (ML 3.2), and in Stalden (ML 3.0). Finally, a small but unusually deep earthquake was recorded beneath the Jura Mountains. Focal depth, apparent velocities, as well as waveform characteristics of this earthquake are consistent with a source in the uppermost mantle. This earthquake is the first reliable record of a sub-Moho event ever observed in Switzerland. Zusammenfassung: Dieser Bericht des Schweizerischen Erdbebendienstes stellt eine Zusammenfassung der im Vorjahr in der Schweiz und Umgebung aufgetretenen Erdbeben dar. Im Jahr 2014 wurden im erwähnten Gebiet 817 Erdbeben sowie 180 Sprengungen erfasst und lokalisiert. Weitere 160 Beben mit Magnituden ML≤1.0 wurden mit Hilfe von zusätzlichen Auswertungsmethoden lokalisiert. Die Zahl der in 2014 lokalisierten Erdbeben ist die höchste seit der Installat
Published: 2021

29. Potential Pitfalls in the Analysis and Structural Interpretation of Seismic Data from the Mars InSight Mission

Author: German Centre for Air and Space Travel, David and Lucile Packard Foundation, California Institute of Technology, Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Agence Nationale de la Recherche (France), Schimmel, Martin [0000-0003-2601-4462], Kim, Doyeon, Davis, Paul, Lekic, Vedran, Maguire, Ross, Compaire, Nicolas, Schimmel, Martin, Stutzmann, E., Irving, Jessica C. E., Lognonné, P., Scholz, J. R., Clinton, John F., Zenhäusern, G., Deng, Sizhuang, Levander, A., Panning, Mark P., Garcia, Raphael F., Giardini, Domenico, Hurst, K., Knapmeyer‐Endrun, Brigitte, Nimmo, F., Pike, William T., Pou, Laurent, Schmerr, N., Stahler, S. C., Tauzin, Benoit, Widmer‐Schnidrig, Rudolf, Banerdt, William B., German Centre for Air and Space Travel, David and Lucile Packard Foundation, California Institute of Technology, Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Agence Nationale de la Recherche (France), Schimmel, Martin [0000-0003-2601-4462], Kim, Doyeon, Davis, Paul, Lekic, Vedran, Maguire, Ross, Compaire, Nicolas, Schimmel, Martin, Stutzmann, E., Irving, Jessica C. E., Lognonné, P., Scholz, J. R., Clinton, John F., Zenhäusern, G., Deng, Sizhuang, Levander, A., Panning, Mark P., Garcia, Raphael F., Giardini, Domenico, Hurst, K., Knapmeyer‐Endrun, Brigitte, Nimmo, F., Pike, William T., Pou, Laurent, Schmerr, N., Stahler, S. C., Tauzin, Benoit, Widmer‐Schnidrig, Rudolf, and Banerdt, William B.
Abstract: The Seismic Experiment for Interior Structure (SEIS) of the InSight mission to Mars has been providing direct information on Martian interior structure and dynamics of that planet since it landed. Compared with seismic recordings on the Earth, ground‐motion measurements acquired by SEIS on Mars are not only made under dramatically different ambient noise conditions, but also include idiosyncratic signals that arise from coupling between different InSight sensors and spacecraft components. This work is to synthesize what is known about these signal types, illustrate how they can manifest in waveforms and noise correlations, and present pitfalls in structural interpretations based on standard seismic analysis methods. We show that glitches (a type of prominent transient signal) can produce artifacts in ambient noise correlations. Sustained signals that vary in frequency, such as lander modes that are affected by variations in temperature and wind conditions over the course of the Martian sol, can also contaminate ambient noise results. Therefore, both types of signals have the potential to bias interpretation in terms of subsurface layering. We illustrate that signal processing in the presence of identified nonseismic signals must be informed by an understanding of the underlying physical processes in order for high‐fidelity waveforms of ground motion to be extracted. Whereas the origins of the most idiosyncratic signals are well understood, the 2.4 Hz resonance remains debated, and the literature does not contain an explanation of its fine spectral structure. Even though the selection of idiosyncratic signal types discussed in this article may not be exhaustive, we provide guidance on the best practices for enhancing the robustness of structural interpretations.
Published: 2021

30. Resonances and Lander Modes Observed by InSight on Mars (1–9 Hz)

Author: National Aeronautics and Space Administration (US), Centre National D'Etudes Spatiales (France), State Secretariat for Education, Research and Innovation (Switzerland), Centre National de la Recherche Scientifique (France), Schimmel, Martin [0000-0003-2601-4462], Dahmen, N. L., Zenhäusern, G., Clinton, John F., Giardini, Domenico, Stahler, S. C., Ceylan, S., Charalambous, C., van Driel, M., Hurst, Kenneth J., Kedar, S., Lognonné, P., Murdoch, N., Myhill, Robert, Panning, Mark P., Pike, William T., Schimmel, Martin, Schmelzbach, C., Scholz, J. R., Stott, A. E., Stutzmann, E., Banerdt, William B., National Aeronautics and Space Administration (US), Centre National D'Etudes Spatiales (France), State Secretariat for Education, Research and Innovation (Switzerland), Centre National de la Recherche Scientifique (France), Schimmel, Martin [0000-0003-2601-4462], Dahmen, N. L., Zenhäusern, G., Clinton, John F., Giardini, Domenico, Stahler, S. C., Ceylan, S., Charalambous, C., van Driel, M., Hurst, Kenneth J., Kedar, S., Lognonné, P., Murdoch, N., Myhill, Robert, Panning, Mark P., Pike, William T., Schimmel, Martin, Schmelzbach, C., Scholz, J. R., Stott, A. E., Stutzmann, E., and Banerdt, William B.
Abstract: The National Aeronautics and Space Administration’s (NASAs) Interior exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) lander successfully touched down on Mars in November 2018, and, for the first time, a seismometer was deployed on the surface of the planet. The seismic recordings reveal diurnal and seasonal changes of the broadband noise level that are consistent with variations of the local atmospheric conditions. The seismic data include a variety of spectral peaks, which are interpreted as wind-excited,mechanical resonances of the lander, resonances of the subsurface, or artifacts produced in themeasurement system. Understanding the origin of these signals is critical for the detection and characterization of marsquakes as well as for studies investigating the ambient noise. We identify the major spectral peaks up to 9 Hz, corresponding to the frequency range the most relevant to observed marsquakes. We track the variations in frequency, amplitude, and polarization of these peaks over the duration of the mission so far. The majority of these peaks can readily be classified as measurement artifacts or lander resonances (lander modes), of which the latter have a temperature-dependent peak frequency and a wind-sensitive amplitude. Of particular interest is a prominent resonance at 2.4 Hz, which is used to discriminate between seismic events and local noise and is possibly produced by a subsurface structure. In contrast to the lander modes, the 2.4 Hz resonance has distinctly different features: (1) a broad and stable spectral shape, slightly shifted on each component; (2) predominantly vertical energy; (3) temperature-independent peak frequency; (4) comparatively weak amplification by local winds, though there is a slow change in the diurnal and seasonal amplitude; and (5) excitation during all seismic events that excite this frequency band. Based on these observations, we suggest that the 2.4 Hz resonance is the only mode below 9 Hz t
Published: 2021

31. 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

32. Initial results from the InSight mission on Mars

Author: Banerdt, W. Bruce, Smrekar, Suzanne E., Banfield, Don, Giardini, Domenico, Golombek, Matthew, Johnson, Catherine L., Lognonne, Philippe, Spiga, Aymeric, Spohn, Tilman, Perrin, Clement, Staehler, Simon C., Antonangeli, Daniele, Asmar, Sami, Beghein, Caroline, Bowles, Neil, Bozdag, Ebru, Chi, Peter, Christensen, Ulrich, Clinton, John, Collins, Gareth S., Daubar, Ingrid, Dehant, Veronique, Drilleau, Melanie, Fillingim, Matthew, Folkner, William, Garcia, Raphael F., Garvin, Jim, Grant, John, Grott, Matthias, Grygorczuk, Jerzy, Hudson, Troy, Irving, Jessica C. E., Kargl, Guenter, 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, Sebastien, Rodriguez-Manfredi, Jose Antonio, Russell, Christopher T., Schmerr, Nicholas, Siegler, Matt, Stanley, Sabine, Stutzmann, Eleanore, Teanby, Nicholas, Tromp, Jeroen, Van Driel, Martin, Warner, Nicholas, Weber, Renee, Wieczorek, Mark, Banerdt, W. Bruce, Smrekar, Suzanne E., Banfield, Don, Giardini, Domenico, Golombek, Matthew, Johnson, Catherine L., Lognonne, Philippe, Spiga, Aymeric, Spohn, Tilman, Perrin, Clement, Staehler, Simon C., Antonangeli, Daniele, Asmar, Sami, Beghein, Caroline, Bowles, Neil, Bozdag, Ebru, Chi, Peter, Christensen, Ulrich, Clinton, John, Collins, Gareth S., Daubar, Ingrid, Dehant, Veronique, Drilleau, Melanie, Fillingim, Matthew, Folkner, William, Garcia, Raphael F., Garvin, Jim, Grant, John, Grott, Matthias, Grygorczuk, Jerzy, Hudson, Troy, Irving, Jessica C. E., Kargl, Guenter, 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, Sebastien, Rodriguez-Manfredi, Jose Antonio, Russell, Christopher T., Schmerr, Nicholas, Siegler, Matt, Stanley, Sabine, Stutzmann, Eleanore, Teanby, Nicholas, Tromp, Jeroen, Van Driel, Martin, Warner, Nicholas, Weber, Renee, and Wieczorek, Mark
Abstract: NASA's InSight (Interior exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed in Elysium Planitia on Mars on 26 November 2018. It aims to determine the interior structure, composition and thermal state of Mars, as well as constrain present-day seismicity and impact cratering rates. Such information is key to understanding the differentiation and subsequent thermal evolution of Mars, and thus the forces that shape the planet's surface geology and volatile processes. Here we report an overview of the first ten months of geophysical observations by InSight. As of 30 September 2019, 174 seismic events have been recorded by the lander's seismometer, including over 20 events of moment magnitude M-w = 3-4. The detections thus far are consistent with tectonic origins, with no impact-induced seismicity yet observed, and indicate a seismically active planet. An assessment of these detections suggests that the frequency of global seismic events below approximately M-w = 3 is similar to that of terrestrial intraplate seismic activity, but there are fewer larger quakes; no quakes exceeding M-w = 4 have been observed. The lander's other instruments-two cameras, atmospheric pressure, temperature and wind sensors, a magnetometer and a radiometer-have yielded much more than the intended supporting data for seismometer noise characterization: magnetic field measurements indicate a local magnetic field that is ten-times stronger than orbital estimates and meteorological measurements reveal a more dynamic atmosphere than expected, hosting baroclinic and gravity waves and convective vortices. With the mission due to last for an entire Martian year or longer, these results will be built on by further measurements by the InSight lander. Geophysical and meteorological measurements by NASA's InSight lander on Mars reveal a planet that is seismically active and provide information about the interior, surface and atmospheric workings of Mars.
Published: 2020

33. Detection, Analysis, and Removal of Glitches From InSight's Seismic Data From Mars

Author: Scholz, John-Robert, Widmer-Schnidrig, Rudolf, Davis, Paul, Lognonne, Philippe, Pinot, Baptiste, Garcia, Raphael F., Hurst, Kenneth, Pou, Laurent, Nimmo, Francis, Barkaoui, Salma, De Raucourt, Sebastien, Knapmeyer-Endrun, Brigitte, Knapmeyer, Martin, Orhand-Mainsant, Guenole, Compaire, Nicolas, Cuvier, Arthur, Beucler, Eric, Bonnin, Mickael, Joshi, Rakshit, Sainton, Gregory, Stutzmann, Eleonore, Schimmel, Martin, Horleston, Anna, Bose, Maren, Ceylan, Savas, Clinton, John, Van Driel, Martin, Kawamura, Taichi, Khan, Amir, Stahler, Simon C., Giardini, Domenico, Charalambous, Constantinos, Stott, Alexander E., Pike, William T., Christensen, Ulrich R., Banerdt, W. Bruce, Scholz, John-Robert, Widmer-Schnidrig, Rudolf, Davis, Paul, Lognonne, Philippe, Pinot, Baptiste, Garcia, Raphael F., Hurst, Kenneth, Pou, Laurent, Nimmo, Francis, Barkaoui, Salma, De Raucourt, Sebastien, Knapmeyer-Endrun, Brigitte, Knapmeyer, Martin, Orhand-Mainsant, Guenole, Compaire, Nicolas, Cuvier, Arthur, Beucler, Eric, Bonnin, Mickael, Joshi, Rakshit, Sainton, Gregory, Stutzmann, Eleonore, Schimmel, Martin, Horleston, Anna, Bose, Maren, Ceylan, Savas, Clinton, John, Van Driel, Martin, Kawamura, Taichi, Khan, Amir, Stahler, Simon C., Giardini, Domenico, Charalambous, Constantinos, Stott, Alexander E., Pike, William T., Christensen, Ulrich R., and Banerdt, W. Bruce
Abstract: The instrument package SEIS (Seismic Experiment for Internal Structure) with the three very broadband and three short-period seismic sensors is installed on the surface on Mars as part of NASA's InSight Discovery mission. When compared to terrestrial installations, SEIS is deployed in a very harsh wind and temperature environment that leads to inevitable degradation of the quality of the recorded data. One ubiquitous artifact in the raw data is an abundance of transient one-sided pulses often accompanied by high-frequency spikes. These pulses, which we term glitches, can be modeled as the response of the instrument to a step in acceleration, while the spikes can be modeled as the response to a simultaneous step in displacement. We attribute the glitches primarily to SEIS-internal stress relaxations caused by the large temperature variations to which the instrument is exposed during a Martian day. Only a small fraction of glitches correspond to a motion of the SEIS package as a whole caused by minuscule tilts of either the instrument or the ground. In this study, we focus on the analysis of the glitch+spike phenomenon and present how these signals can be automatically detected and removed from SEIS's raw data. As glitches affect many standard seismological analysis methods such as receiver functions, spectral decomposition and source inversions, we anticipate that studies of the Martian seismicity as well as studies of Mars' internal structure should benefit from deglitched seismic data. Plain Language Summary The instrument package SEIS (Seismic Experiment for Internal Structure) with two fully equipped seismometers is installed on the surface of Mars as part of NASA's InSight Discovery mission. When compared to terrestrial installations, SEIS is more exposed to wind and daily temperature changes that leads to inevitable degradation of the quality of the recorded data. One consequence is the occurrence of a specific type of transient noise that we term glitch. Glitc
Published: 2020

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

Author: Drilleau, Melanie, Beucler, Eric, Lognonne, Philippe, Panning, Mark P., Knapmeyer-Endrun, Brigitte, Banerdt, W. Bruce, Beghein, Caroline, Ceylan, Savas, van Driel, Martin, Joshi, Rakshit, Kawamura, Taichi, Khan, Amir, Menina, Sabrina, Rivoldini, Attilio, Samuel, Henri, Stahler, Simon, Xu, Haotian, Bonnin, Mickael, Clinton, John, Giardini, Domenico, Kenda, Balthasar, Lekic, Vedran, Mocquet, Antoine, Murdoch, Naomi, Schimmel, Martin, Smrekar, Suzanne E., Stutzmann, Eleonore, Tauzin, Benoit, Tharimena, Saikiran, Drilleau, Melanie, Beucler, Eric, Lognonne, Philippe, Panning, Mark P., Knapmeyer-Endrun, Brigitte, Banerdt, W. Bruce, Beghein, Caroline, Ceylan, Savas, van Driel, Martin, Joshi, Rakshit, Kawamura, Taichi, Khan, Amir, Menina, Sabrina, Rivoldini, Attilio, Samuel, Henri, Stahler, Simon, Xu, Haotian, Bonnin, Mickael, Clinton, John, Giardini, Domenico, Kenda, Balthasar, Lekic, Vedran, Mocquet, Antoine, Murdoch, Naomi, Schimmel, Martin, Smrekar, Suzanne E., Stutzmann, Eleonore, Tauzin, Benoit, and Tharimena, Saikiran
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

35. Initial results from the InSight mission on Mars

Author: UCL - SST/ELI/ELIC - Earth & Climate, 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, UCL - SST/ELI/ELIC - Earth & Climate, 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, and Dehant, Véronique
Abstract: Initial results from the InSight mission on Mars, getting information on the interior of Mars.
Published: 2020

36. Measuring Fundamental and Higher Mode Surface Wave Dispersion on Mars From Seismic Waveforms

Author: Xu, Haotian, Xu, Haotian, Beghein, Caroline, Panning, Mark Paul, Drilleau, Mélanie, Lognonné, Philippe Henri, van Driel, Martin, Ceylan, Savas, Böse, Maren, Brinkman, Nienke, Clinton, John, Euchner, Fabian, Giardini, Domenico, Horleston, Anna Catherine, Kawamura, Taichi, Kenda, Balthasar, Murdoch, Naomi, Stähler, Simon C, Xu, Haotian, Xu, Haotian, Beghein, Caroline, Panning, Mark Paul, Drilleau, Mélanie, Lognonné, Philippe Henri, van Driel, Martin, Ceylan, Savas, Böse, Maren, Brinkman, Nienke, Clinton, John, Euchner, Fabian, Giardini, Domenico, Horleston, Anna Catherine, Kawamura, Taichi, Kenda, Balthasar, Murdoch, Naomi, and Stähler, Simon C
Published: 2020

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

Author: California Institute of Technology, National Aeronautics and Space Administration (US), National Supercomputing Center of Tianjin, Swiss National Science Foundation, NASA Jet Propulsion Laboratory, Schimmel, Martin [0000-0003-2601-4462], Drilleau, M., Beucler, E., Lognonné, P., Panning, M.P., Knapmeyer‐Endrun, Brigitte, Banerdt, W. B., Beghein, C., Ceylan, S., van Driel, M., Joshi, R., Kawamura, T., Khan, A., Menina, S., Rivoldini, A., Samuel, H., Stähler, S., Xu, H., Bonnin, Mickaël, Clinton, John F., Giardini, Domenico, Kenda, B., Lekic, Vedran, Mocquet, A., Murdoch, N., Schimmel, Martin, Smrekar, S. E., Stutzmann, E., Tauzin, B., Tharimena, S., California Institute of Technology, National Aeronautics and Space Administration (US), National Supercomputing Center of Tianjin, Swiss National Science Foundation, NASA Jet Propulsion Laboratory, Schimmel, Martin [0000-0003-2601-4462], Drilleau, M., Beucler, E., Lognonné, P., Panning, M.P., Knapmeyer‐Endrun, Brigitte, Banerdt, W. B., Beghein, C., Ceylan, S., van Driel, M., Joshi, R., Kawamura, T., Khan, A., Menina, S., Rivoldini, A., Samuel, H., Stähler, S., Xu, H., Bonnin, Mickaël, Clinton, John F., Giardini, Domenico, Kenda, B., Lekic, Vedran, Mocquet, A., Murdoch, N., Schimmel, Martin, Smrekar, S. E., Stutzmann, E., Tauzin, B., and Tharimena, S.
Abstract: SEIS, the seismometer of the InSight mission, which landed on Mars on 26 November 2018, is monitoring the seismic activity of the planet. The goal of the Mars Structure Service (MSS) is to provide, as a mission product, the first average 1-D velocity model of Mars from the recorded InSight data. Prior to the mission, methodologies have been developed and tested to allow the location of the seismic events and estimation of the radial structure, using surface waves and body waves arrival times, and receiver functions. The paper describes these validation tests and compares the performance of the different algorithms to constrain the velocity model below the InSight station and estimate the 1-D average model over the great circle path between source and receiver. These tests were performed in the frame of a blind test, during which synthetic data were inverted. In order to propagate the data uncertainties on the output model distribution, Bayesian inversion techniques are mainly used. The limitations and strengths of the methods are assessed. The results show the potential of the MSS approach to retrieve the structure of the crust and underlying mantle. However, at this time, large quakes with clear surface waves have not yet been recorded by SEIS, which makes the estimation of the 1-D average seismic velocity model challenging. Additional locatable events, especially at large epicentral distances, and development of new techniques to fully investigate the data, will ultimately provide more constraints on the crust and mantle of Mars. ©2020 The Authors.
Published: 2020

38. InSight seismic data from Mars: Effect and treatment of transient data disturbances.

Author: Widmer-Schnidrig, Rudolf, Scholz, J. R., Davis, Paul, Lognonné, P., Pinot, Baptiste, García, Raphael, Hurst, K., Pou, Laurent, Nimmo, F., Barkaoui, Salma, De Raucourt, Sebastien, Knapmeyer‐Endrun, Brigitte, Knapmeyer, M., Orhand-Mainsant, Guenolé, Compaire, Nicolas, Cuvier, Arthur, Beucler, E., Bonnin, Mickaël J. A., Joshi, Rakshit, Sainton, G., Stutzmann, E., Schimmel, Martin, Horleston, Anna C., Böse, M., Ceylan, S., Clinton, John F., van Driel, M., Kawamura, T., Khan, A., Staehler, Simon C., Giardini, Domenico, Charalambous, C., Stott, Alexander, Pike, William T., Christensen, U., Banerdt, William B., Widmer-Schnidrig, Rudolf, Scholz, J. R., Davis, Paul, Lognonné, P., Pinot, Baptiste, García, Raphael, Hurst, K., Pou, Laurent, Nimmo, F., Barkaoui, Salma, De Raucourt, Sebastien, Knapmeyer‐Endrun, Brigitte, Knapmeyer, M., Orhand-Mainsant, Guenolé, Compaire, Nicolas, Cuvier, Arthur, Beucler, E., Bonnin, Mickaël J. A., Joshi, Rakshit, Sainton, G., Stutzmann, E., Schimmel, Martin, Horleston, Anna C., Böse, M., Ceylan, S., Clinton, John F., van Driel, M., Kawamura, T., Khan, A., Staehler, Simon C., Giardini, Domenico, Charalambous, C., Stott, Alexander, Pike, William T., Christensen, U., and Banerdt, William B.
Abstract: The instrument package SEIS (Seismic Experiment for Internal Structure) with the two co-located seismometers VBB and SP is installed on the surface of Mars as part of NASA's InSight mission. When compared to terrestrial installations, SEIS is deployed in a very harsh wind and temperature environment that leads to inevitable degradation of the quality of the recorded data. The daily atmospheric temperature variations of approx. 80K are attenuated by different insulation layers to approx. 15K peak-to-peak at the sensor level. Typical wind speeds vary between 0 and 5 m/s leading to a diurnal variation in the broad-band rms noise level by two orders of magnitude. One ubiquitous artifact in the raw broad-band data is an abundance of one-sided, transient pulses often accompanied by high-frequency spikes. We show that these pulses, which we term "glitches", can be modeled as the response of the instrument to a step in acceleration, while the spikes can be modeled as the response to a simultaneous step in displacement. We attribute the glitches primarily to intermittent stress relaxation events internal to SEIS caused by the large diurnal temperature variations to which the instrument is exposed during a Martian sol. Only a small fraction of glitches correspond to a motion of the SEIS package as a whole caused by minuscule tilts of the instrument. Whilst such kind of data disturbances are typically discarded when occurring in terrestrial data, this is no option for the data returned from the Red Planet. We therefore do not only demonstrate their effects on the seismic data and analyze their origins, but also propose algorithms that are able to detect and remove many of these (mostly) non-seismic signals. We further published our codes (both Python and MATLAB) so that interested researchers can make their own choices on how to treat the data and to which extent.
Published: 2020

39. Detection, Analysis, and Removal of Glitches From InSight's Seismic Data From Mars

Author: Agence Nationale de la Recherche (France), Swiss Space Office, Schimmel, Martin [0000-0003-2601-4462], Scholz, J. R., Widmer‐Schnidrig, Rudolf, Davis, Paul, Lognonné, P., Pinot, Baptiste, Garcia, Raphael F., Hurst, K., Pou, Laurent, Nimmo, F., Barkaoui, Salma, De Raucourt, Sebastien, Knapmeyer‐Endrun, Brigitte, Knapmeyer, M., Orhand-Mainsant, Guenolé, Compaire, Nicolas, Cuvier, Arthur, Beucler, E., Bonnin, Mickaël, Joshi, Rakshit, Sainton, G., Stutzmann, E., Schimmel, Martin, Horleston, Anna, Böse, M., Ceylan, S., Clinton, John F., van Driel, M., Kawamura, T., Khan, A., Stähler, S. C., Giardini, Domenico, Charalambous, C., Stott, A. E., Pike, William T., Christensen, U., Banerdt, William B., Agence Nationale de la Recherche (France), Swiss Space Office, Schimmel, Martin [0000-0003-2601-4462], Scholz, J. R., Widmer‐Schnidrig, Rudolf, Davis, Paul, Lognonné, P., Pinot, Baptiste, Garcia, Raphael F., Hurst, K., Pou, Laurent, Nimmo, F., Barkaoui, Salma, De Raucourt, Sebastien, Knapmeyer‐Endrun, Brigitte, Knapmeyer, M., Orhand-Mainsant, Guenolé, Compaire, Nicolas, Cuvier, Arthur, Beucler, E., Bonnin, Mickaël, Joshi, Rakshit, Sainton, G., Stutzmann, E., Schimmel, Martin, Horleston, Anna, Böse, M., Ceylan, S., Clinton, John F., van Driel, M., Kawamura, T., Khan, A., Stähler, S. C., Giardini, Domenico, Charalambous, C., Stott, A. E., Pike, William T., Christensen, U., and Banerdt, William B.
Abstract: The instrument package SEIS (Seismic Experiment for Internal Structure) with the three very broadband and three short‐period seismic sensors is installed on the surface on Mars as part of NASA's InSight Discovery mission. When compared to terrestrial installations, SEIS is deployed in a very harsh wind and temperature environment that leads to inevitable degradation of the quality of the recorded data. One ubiquitous artifact in the raw data is an abundance of transient one‐sided pulses often accompanied by high‐frequency spikes. These pulses, which we term “glitches”, can be modeled as the response of the instrument to a step in acceleration, while the spikes can be modeled as the response to a simultaneous step in displacement. We attribute the glitches primarily to SEIS‐internal stress relaxations caused by the large temperature variations to which the instrument is exposed during a Martian day. Only a small fraction of glitches correspond to a motion of the SEIS package as a whole caused by minuscule tilts of either the instrument or the ground. In this study, we focus on the analysis of the glitch+spike phenomenon and present how these signals can be automatically detected and removed from SEIS's raw data. As glitches affect many standard seismological analysis methods such as receiver functions, spectral decomposition and source inversions, we anticipate that studies of the Martian seismicity as well as studies of Mars' internal structure should benefit from deglitched seismic data.
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

42. Direct observations of a three million cubic meter rock-slope collapse with almost immediate initiation of ensuing debris flows

Author: Walter, Fabian, Amann, Florian, Kos, Andrew, Kenner, Robert, Phillips, Marcia, Preux, Antoine de, Huss, Matthias, Tognacca, Christian, Clinton, John, Diehl, Tobias, Bonanomi, Yves, Walter, Fabian, Amann, Florian, Kos, Andrew, Kenner, Robert, Phillips, Marcia, Preux, Antoine de, Huss, Matthias, Tognacca, Christian, Clinton, John, Diehl, Tobias, and Bonanomi, Yves
Abstract: Catastrophic collapse of large rock slopes ranks as one of the most hazardous natural phenomena in mountain landscapes. The cascade of events, from rock- slope failure, to rock avalanche and the near-immediate release of debris flows has not previously been described from direct observations. We report on the 2017, 3.0 × 106 m3 failure on Pizzo Cengalo in Switzerland, which led to human casualties and significant damage to infrastructure. Based on remote sensing and field investigations, we find a change in critical slope stability prior to failure for which permafrost may have played a destabilizing role. The resulting rock avalanche traveled for 3.2 km and removed over one million m3 of glacier ice and debris deposits from a previous rock avalanche in 2011. Whereas this entrainment did not lead to an unusually large runout distance, it favored debris flow activity from the 2017 rock avalanche deposits: the first debris flow occurred with a delay of 30 s followed by ten debris flows within 9.5 h and two additional events two days later, notably in the absence of rainfall. We hypothesize that entrainment and impact loading of saturated sediments explain the initial mobility of the 2017 rock avalanche deposits leading to a near- immediate initiation of debris flows. This explains why an earlier rock avalanche at the same site in 2011 was not directly followed by debris flows and underlines the importance of considering sediment saturation in a rock avalanche’s runout path for Alpine hazard assessments.
Published: 2020

43. Inventory control in a multi-warehouse system

Author: Clinton, John Oakley
Subjects: 519.5, Statistics
Published: 1969

44. Arrival angles of teleseismic fundamental mode Rayleigh waves across the AlpArray

Author: Kolinsky, Petr, Bokelmann, Goetz, Hetenyi, Gyorgy, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-theresia, Aubert, Coralie, Besancon, Simon, Bes De Berc, Maxime, Bokel-mann, Gotz, Brunel, Didier, Capello, Marco, Carman, Martina, Cavaliere, Adriano, Cheze, Jerome, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, Crawford, Wayne C., Cristiano, Luigia, Czifra, Tibor, D'Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasovic, Iva, Deschamps, Anne, Dessa, Jean-xavier, Doubre, Cecile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Graczer, Zoltan, Groschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jaric, Dejan, Jedlicka, Petr, Jia, Yan, Jund, Helene, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kuhne, Lothar, Kuk, Kreso, Lange, Dietrich, Loos, Jurgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Metral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Pequegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerova, Jaroslava, Pondrelli, Silvia, Prevolnik, Snjezan, Racine, Roman, Regnier, Marc, Reiss, Miriam, Ritter, Joachim, Rumpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-kortnack, Detlef, Sipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipcevic, Josip, Strollo, Angelo, Sule, Balint, Szanyi, Gyongyver, Szucs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Ludek, Voigt, Rene, Wassermann, Joachim, Weber, Zoltan, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix, Wolyniec, David, Zieke, Thomas, Zivcic, Mladen, Zlebcikova, Helena, Kolinsky, Petr, Bokelmann, Goetz, Hetenyi, Gyorgy, Abreu, Rafael, Allegretti, Ivo, Apoloner, Maria-theresia, Aubert, Coralie, Besancon, Simon, Bes De Berc, Maxime, Bokel-mann, Gotz, Brunel, Didier, Capello, Marco, Carman, Martina, Cavaliere, Adriano, Cheze, Jerome, Chiarabba, Claudio, Clinton, John, Cougoulat, Glenn, Crawford, Wayne C., Cristiano, Luigia, Czifra, Tibor, D'Alema, Ezio, Danesi, Stefania, Daniel, Romuald, Dannowski, Anke, Dasovic, Iva, Deschamps, Anne, Dessa, Jean-xavier, Doubre, Cecile, Egdorf, Sven, Fiket, Tomislav, Fischer, Kasper, Friederich, Wolfgang, Fuchs, Florian, Funke, Sigward, Giardini, Domenico, Govoni, Aladino, Graczer, Zoltan, Groschl, Gidera, Heimers, Stefan, Heit, Ben, Herak, Davorka, Herak, Marijan, Huber, Johann, Jaric, Dejan, Jedlicka, Petr, Jia, Yan, Jund, Helene, Kissling, Edi, Klingen, Stefan, Klotz, Bernhard, Kopp, Heidrun, Korn, Michael, Kotek, Josef, Kuhne, Lothar, Kuk, Kreso, Lange, Dietrich, Loos, Jurgen, Lovati, Sara, Malengros, Deny, Margheriti, Lucia, Maron, Christophe, Martin, Xavier, Massa, Marco, Mazzarini, Francesco, Meier, Thomas, Metral, Laurent, Molinari, Irene, Moretti, Milena, Nardi, Anna, Pahor, Jurij, Paul, Anne, Pequegnat, Catherine, Petersen, Daniel, Pesaresi, Damiano, Piccinini, Davide, Piromallo, Claudia, Plenefisch, Thomas, Plomerova, Jaroslava, Pondrelli, Silvia, Prevolnik, Snjezan, Racine, Roman, Regnier, Marc, Reiss, Miriam, Ritter, Joachim, Rumpker, Georg, Salimbeni, Simone, Santulin, Marco, Scherer, Werner, Schippkus, Sven, Schulte-kortnack, Detlef, Sipka, Vesna, Solarino, Stefano, Spallarossa, Daniele, Spieker, Kathrin, Stipcevic, Josip, Strollo, Angelo, Sule, Balint, Szanyi, Gyongyver, Szucs, Eszter, Thomas, Christine, Thorwart, Martin, Tilmann, Frederik, Ueding, Stefan, Vallocchia, Massimiliano, Vecsey, Ludek, Voigt, Rene, Wassermann, Joachim, Weber, Zoltan, Weidle, Christian, Wesztergom, Viktor, Weyland, Gauthier, Wiemer, Stefan, Wolf, Felix, Wolyniec, David, Zieke, Thomas, Zivcic, Mladen, and Zlebcikova, Helena
Abstract: The dense AlpArray network allows studying seismic wave propagation with high spatial resolution. Here we introduce an array approach to measure arrival angles of teleseismic Rayleigh waves. The approach combines the advantages of phase correlation as in the two-station method with array beamforming to obtain the phase-velocity vector. 20 earthquakes from the first two years of the AlpArray project are selected, and spatial patterns of arrival-angle deviations across the AlpArray are shown in maps, depending on period and earthquake location. The cause of these intriguing spatial patterns is discussed. A simple wave-propagation modelling example using an isolated anomaly and a Gaussian beam solution suggests that much of the complexity can be explained as a result of wave interference after passing a structural anomaly along the wave paths. This indicates that arrival-angle information constitutes useful additional information on the Earth structure, beyond what is currently used in inversions.
Published: 2019
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45. Preparing for InSight: Evaluation of the Blind Test for Martian Seismicity

Author: van Driel, Martin, Ceylan, Savas, Clinton, John Francis, Giardini, Domenico, Alemany, Hector, Allam, Amir, Ambrois, David, Balestra, Julien, Banerdt, Bruce, Becker, Dirk, Bose, Maren, Boxberg, Marc S., Brinkman, Nienke, Casademont, Titus, Cheze, Jerome, Daubar, Ingrid, Deschamps, Anne, Dethof, Fabian, Ditz, Manuel, Drilleau, Melanie, Essing, David, Euchner, Fabian, Fernando, Benjamin, Garcia, Raphael, Garth, Thomas, Godwin, Harriet, Golombek, Matthew P., Grunert, Katharina, Hadziioannou, Celine, Haindl, Claudia, Hammer, Conny, Hochfeld, Isabell, Hosseini, Kasra, Hu, Hao, Kedar, Sharon, Kenda, Balthasar, Khan, Amir, Kilchling, Tabea, Knapmeyer-Endrun, Brigitte, Lamert, Andre, Li, Jiaxuan, Lognonne, Philippe, Mader, Sarah, Marten, Lorenz, Mehrkens, Franziska, Mercerat, Diego, Mimoun, David, Moeller, Thomas, Murdoch, Naomi, Neumann, Paul, Neurath, Robert, Paffrath, Marcel, Panning, Mark P., Peix, Fabrice, Perrin, Ludovic, Rolland, Lucie, Schimmel, Martin, Schroeer, Christoph, Spiga, Aymeric, Stahler, Simon Christian, Steinmann, Rene, Stutzmann, Eleonore, Szenicer, Alexandre, Trumpik, Noah, Tsekhmistrenko, Maria, Twardzik, Cedric, Weber, Renee, Werdenbach-Jarklowski, Philipp, Zhang, Shane, Zheng, Yingcai, van Driel, Martin, Ceylan, Savas, Clinton, John Francis, Giardini, Domenico, Alemany, Hector, Allam, Amir, Ambrois, David, Balestra, Julien, Banerdt, Bruce, Becker, Dirk, Bose, Maren, Boxberg, Marc S., Brinkman, Nienke, Casademont, Titus, Cheze, Jerome, Daubar, Ingrid, Deschamps, Anne, Dethof, Fabian, Ditz, Manuel, Drilleau, Melanie, Essing, David, Euchner, Fabian, Fernando, Benjamin, Garcia, Raphael, Garth, Thomas, Godwin, Harriet, Golombek, Matthew P., Grunert, Katharina, Hadziioannou, Celine, Haindl, Claudia, Hammer, Conny, Hochfeld, Isabell, Hosseini, Kasra, Hu, Hao, Kedar, Sharon, Kenda, Balthasar, Khan, Amir, Kilchling, Tabea, Knapmeyer-Endrun, Brigitte, Lamert, Andre, Li, Jiaxuan, Lognonne, Philippe, Mader, Sarah, Marten, Lorenz, Mehrkens, Franziska, Mercerat, Diego, Mimoun, David, Moeller, Thomas, Murdoch, Naomi, Neumann, Paul, Neurath, Robert, Paffrath, Marcel, Panning, Mark P., Peix, Fabrice, Perrin, Ludovic, Rolland, Lucie, Schimmel, Martin, Schroeer, Christoph, Spiga, Aymeric, Stahler, Simon Christian, Steinmann, Rene, Stutzmann, Eleonore, Szenicer, Alexandre, Trumpik, Noah, Tsekhmistrenko, Maria, Twardzik, Cedric, Weber, Renee, Werdenbach-Jarklowski, Philipp, Zhang, Shane, and Zheng, Yingcai
Abstract: In December 2018, the National Aeronautics and Space Administration (NASA) Interior exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission deployed a seismometer on the surface of Mars. In preparation for the data analysis, in July 2017, the marsquake service initiated a blind test in which participants were asked to detect and characterize seismicity embedded in a one Earth year long synthetic data set of continuous waveforms. Synthetic data were computed for a single station, mimicking the streams that will be available from InSight as well as the expected tectonic and impact seismicity, and noise conditions on Mars (Clinton et al., 2017). In total, 84 teams from 20 countries registered for the blind test and 11 of them submitted their results in early 2018. The collection of documentations, methods, ideas, and codes submitted by the participants exceeds 100 pages. The teams proposed well established as well as novel methods to tackle the challenging target of building a global seismicity catalog using a single station. This article summarizes the performance of the teams and highlights the most successful contributions.
Published: 2019

46. Mars Structure Service: Single-Station and Single-Event Marsquake Inversion for Structure Using Synthetic Martian Waveforms

Author: Khan, A., Drilleau, M., Beucler, E., Panning, M., Lognonné, P., Beghein, Caroline, Xu, H., Menina, Sabrina, Barkaoui, S., Lekic, Vedran, Stähler, S., van Driel, M., Kenda, B., Murdoch, N., Clinton, John F., Giardini, Domenico, Smrekar, S., Stutzmann, E., Schimmel, Martin, Khan, A., Drilleau, M., Beucler, E., Panning, M., Lognonné, P., Beghein, Caroline, Xu, H., Menina, Sabrina, Barkaoui, S., Lekic, Vedran, Stähler, S., van Driel, M., Kenda, B., Murdoch, N., Clinton, John F., Giardini, Domenico, Smrekar, S., Stutzmann, E., and Schimmel, Martin
Abstract: Introduction: The InSight lander successfully delivered a geophysical instrument package on the Martian surface on November 26th, 2018, including a broadband and a short-period seismometer (Seismic Experiment for Interior Structure, SEIS). The seismic instrument package is specifically designed to record marsquakes and meteoritic impacts in Martian conditions [1]. Routine operations are split into two services: the Mars Structure Service (MSS) and the Marsquake Service (MQS that are responsible for defining structure models and seismicity catalogs, respectively [2, 3]. The first ¿deliverable¿ of the MSS will be a model based on the events detected during the first 3 months of seismic monitoring of the mission, for which only a few quakes might be expected based on current estimates of Mars seismic activity. To test our approach of determining the interior model of Mars and to prepare the InSight science team for data return, we made use of a ¿blind test¿ time series for which the Marsquake parameters (location, depth, origin time, and moment tensor) and interior model were unknown to the group at large.
Published: 2019

47. SEIS: Overview, Deployment, and First Science on the Ground

Author: Lognonné, P., Banerdt, W. B., Pike, William T., Giardini, Domenico, Banfield, D., Christensen, U., Bierwirth, M., S. Calcutt, S., Clinton, John F., Kedar, S., Garcia, R., de Raucourt, S., Hurst, K., Kawamura, T., Mimoun, D., Panning, M., Spiga, A., Zweifel, P., Beucler, E., Verdier, N. Ceylan, S., Charalambous, C., Drilleau, M., Eberhardt, M., Fayon, L., Gabsi, T., Kenda, B., Kramer, A., Mainsant, G., Mance, D., McClean, J., Murdoch, N., Nebut, T., Pardo, C., Perrin, C., Robert, O., Savoie, D., Schimmel, Martin, Stähler, S., Stutzmann, E., Stott, A., Ten Pierick, J., Tillier, S., van Driel, M., Warren, T., Widmer-Schnidrig, R., Lognonné, P., Banerdt, W. B., Pike, William T., Giardini, Domenico, Banfield, D., Christensen, U., Bierwirth, M., S. Calcutt, S., Clinton, John F., Kedar, S., Garcia, R., de Raucourt, S., Hurst, K., Kawamura, T., Mimoun, D., Panning, M., Spiga, A., Zweifel, P., Beucler, E., Verdier, N. Ceylan, S., Charalambous, C., Drilleau, M., Eberhardt, M., Fayon, L., Gabsi, T., Kenda, B., Kramer, A., Mainsant, G., Mance, D., McClean, J., Murdoch, N., Nebut, T., Pardo, C., Perrin, C., Robert, O., Savoie, D., Schimmel, Martin, Stähler, S., Stutzmann, E., Stott, A., Ten Pierick, J., Tillier, S., van Driel, M., Warren, T., and Widmer-Schnidrig, R.
Abstract: Introduction: The InSight mission landed on Mars on November, 26, 2018. This is the first planetary mission designed to deploy a complete geophysical observatory on Mars, following in the footsteps of the Apollo Lunar Surface Experiments Package (ALSEP) deployed on the Moon in the 1970s [1]. It will thus provide the first ground truth constraints on interior structure of the planet. The Seismic Experiment for Interior Structure (SEIS) [2] is one of three primary scientific investigations, the others being the Heat Flow and Physical Properties Package (HP3) [3] and the Rotation and Interior Structure Experiment (RISE) [4]. SEIS is supported by the APSS package, (Auxiliary Payload Sensor Suite, [5]), whose goal is to document environmental sources of seismic noise and signals, as well as an imaging system [6]. After a brief description of the SEIS experiment, we will describe the deployment process, including the evolution of the SEIS noise from the deck (with only SPs) to the ground (with both VBBs and SPs), first without and finally with wind shield. We will then discuss early scientific observations, providing first constrains on the Mars micro-seismic noise, atmospherically-generated seismic signals, and surface and subsurface elastic structure.
Published: 2019

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

Author: Barkaoui, Salma, Lognonné, P., Dehoop, Maarten, Drilleau, M., Kawamura, T., Stutzmann, E., van Driel, M., Kenda, B., Sainton, G., Seydoux, Leonard, Clinton, John F., Schimmel, Martin, Murdoch, N., Barkaoui, Salma, Lognonné, P., Dehoop, Maarten, Drilleau, M., Kawamura, T., Stutzmann, E., van Driel, M., Kenda, B., Sainton, G., Seydoux, Leonard, Clinton, John F., Schimmel, Martin, and Murdoch, N.
Abstract: Exploring the internal structure and the dynamics of our solar system is mandatory to understand the behavior of our universe and its origin. One of the tools chosen by NASA is seismology particularly in order to constrain the parameters of the deep interior structure of the red planet via the Insight (Interior Exploration using Seismic Investigations, Geodesy, and Heat Transport) mission. InSight was successfully landed on November 26th, 2018 in Elysium Planitia with geophysical instruments a short-period seismometer and a broadband seismometer (SEIS, Seismic Experiment for Interior Structure). Both seismometers are now installed directly on Mars surface and enable to analyze the continuous seismic signal.But, before making the structure inversion, we need to extract the features from SEIS data. However, those features may nevertheless be hidden into noise, or may escape from analysis due to the limitations imposed by the current methodologies.Therefore, the aim of this study is to overcome this problem by well extracting, recognizing and classifying the instrument signals using Machine Learning and Deep Learning new strategies inspired from the Deep scattering network.This is very promising for the SIES data as, we¿re going to be able not only to detect the familiar signals, but the exciting part is the unseen or the unknown ones. This technique is used to clean the data from the glitches. In fact, this tool has recently proved to be powerful in signal processing, data automatic feature extraction and may even be helpful to detect new types of signals. Those new signals can reveal unknown processes and lead to new discoveries about Mars physical processes.The method used in this study is divided into three fundamental steps. The first one, to make an automatic feature extraction using the Deep scattering transform which is a convolution neural network that computes a cascade of wavelets calculations and filtering operations to get a stable waveform representation
Published: 2019

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

Author: Drilleau, M., Lognonné, P., Panning, Mark P., Beucler, E., Khan, A., van Driel, M., Beghein, Caroline, Staehler, Simon C., Knapmeyer‐Endrun, Brigitte, Ceylan, S., Barkaoui, Salma, Clinton, John F., Giardini, Domenico, Joshi, R., Kenda, B., Lekic, Vedran, Menina, Sabrina, Murdoch, N., Rivoldini, A., Samuel, H., Schimmel, Martin, Smrekar, Suzanne, Stutzmann, Martin, Tauzin, Benoit, Tharimena, S., Xu, Haotian, Drilleau, M., Lognonné, P., Panning, Mark P., Beucler, E., Khan, A., van Driel, M., Beghein, Caroline, Staehler, Simon C., Knapmeyer‐Endrun, Brigitte, Ceylan, S., Barkaoui, Salma, Clinton, John F., Giardini, Domenico, Joshi, R., Kenda, B., Lekic, Vedran, Menina, Sabrina, Murdoch, N., Rivoldini, A., Samuel, H., Schimmel, Martin, Smrekar, Suzanne, Stutzmann, Martin, Tauzin, Benoit, Tharimena, S., and Xu, Haotian
Abstract: The SEIS seismometer package was successfully deployed on Mars by February 2019. Routine operations are split into two services: the Mars Structure Service (MSS) and the Marsquake Service (MQS), which are responsible for defining interior structure models and seismicity catalogs, respectively. Initial model delivery from MSS is based on a limited dataset of two Marsquakes with a clear P and S arrivals. Different inversion algorithms were developed by the MSS team in order to retrieve the first 1D averaged model of Mars. Two complementary approaches are considered. One set of models (called M1) is parameterized in seismic velocity and density as a function of depth. A second set of models (called M2) is obtained by parameterizing with geodynamical constraints like temperature and composition. We use Bayesian inversion techniques to obtain robust probability density functions of seismic velocity profiles. Different types of data are considered for these inversions including body waves, surface waves and receiver functions. To characterize what we could learn about Mars¿ interior structure with only one station and with the first seismic event, we performed inversions of synthetic data following a blind test process, where the interior model and the Marsquake parameters (location, depth, origin time, and moment tensor) were unknown to all team members carrying out data analysis and inversion. In this presentation we will discuss the results of this blind test in terms of structure and compare different methods developed by the MSS. We will then show results from investigations of the first, real seismic data due to quakes on Mars recorded by SEIS in terms of the structure and quake locations. We will especially focus our investigation on joint inversions made not only with the arrival time, but also with secondary seismic data extracted from the detected events, including apparent attenuation rate and with receiver functions. Of course, much more detailed analysis will
Published: 2019

50. SEIS first year: nm/s^2 (and less) broadband seismology on Mars and first steps in Mars-Earth-Moon comparative seismology. (Invited)

Author: Lognonné, P., Banerdt, William B., Pike, William T., Giardini, Domenico, Banfield, D., Christensen, U., Beucler, E., Bierwirth, Marco, Calcutt, Simon B., Daubar, I., Clinton, John F., Kedar, S., Gabsi, T., Garcia, Raphael G., Hurst, K., Kawamura, T., Knapmeyer‐Endrun, Brigitte, Margerin, Ludovic, Mimoun, D., Nimmo, F., Panning, Mark P., De Raucourt, Sebastien, Schmerr, Nicholas C., Smrekar, Suzanne, Spiga, A., Teanby, Nicholas A., Weber, R. C., Wieczorek, M., Zweifel, Peter, Yana, C., Barkaoui, Salma, Brinkman, N., Ceylan, S., Conejero, Vicente, Compaire, Nicolas, Charalambous, C., Davis, Paul, van Driel, M., Drilleau, M., Fayon, Lucile, Kenda, B., Mance, Davor, McClean, John, Murdoch, N., Nebut, Tanguy, Pardo, Constanza, Pinot, Baptiste, Pou, Laurent, Perrin, C., Sainton, G., Sollberger, David, Scholz, J. R., Staehler, Simon C., Roberts, Oliver, Schmelzbach, C., Stott, A., Schimmel, Martin, Stutzmann, E., Tillier, Sylvain, Verdier, Nicolas, Warren, T., Widmer-Schnidrig, Rudolf, Böse, M., Euchner, F., Horleston, Anna C., Khan, A., Orhand-Mainsant, Guenolé, Barrett, E., Gaudin, E., Kerjean, Laurent, Julien, Agnès, Nonon, M., Llorca-Cejudo, R., Laudet, Philippe, Maki, Justin, Mouret, Jean-Marie, Pont, Gabriel, Meunier, Frederic A., Rochas, Ludovic, de Larclause, Isabel Savin, Sylvestre-Baron, Annick, Trebi-Ollenu, Ashitey, Valladeau, J., Delage, P., Jacob, A., Calvet, Marie, Grotte, M., Rodríguez-Manfredi, José Antonio, Lekic, Vedran, Menina, Sabrina, Robertsson, John O.A., Spohn, Tilman, Tauzin, Benoit, Tharimena, S., Pierick, Jen Ten, Lognonné, P., Banerdt, William B., Pike, William T., Giardini, Domenico, Banfield, D., Christensen, U., Beucler, E., Bierwirth, Marco, Calcutt, Simon B., Daubar, I., Clinton, John F., Kedar, S., Gabsi, T., Garcia, Raphael G., Hurst, K., Kawamura, T., Knapmeyer‐Endrun, Brigitte, Margerin, Ludovic, Mimoun, D., Nimmo, F., Panning, Mark P., De Raucourt, Sebastien, Schmerr, Nicholas C., Smrekar, Suzanne, Spiga, A., Teanby, Nicholas A., Weber, R. C., Wieczorek, M., Zweifel, Peter, Yana, C., Barkaoui, Salma, Brinkman, N., Ceylan, S., Conejero, Vicente, Compaire, Nicolas, Charalambous, C., Davis, Paul, van Driel, M., Drilleau, M., Fayon, Lucile, Kenda, B., Mance, Davor, McClean, John, Murdoch, N., Nebut, Tanguy, Pardo, Constanza, Pinot, Baptiste, Pou, Laurent, Perrin, C., Sainton, G., Sollberger, David, Scholz, J. R., Staehler, Simon C., Roberts, Oliver, Schmelzbach, C., Stott, A., Schimmel, Martin, Stutzmann, E., Tillier, Sylvain, Verdier, Nicolas, Warren, T., Widmer-Schnidrig, Rudolf, Böse, M., Euchner, F., Horleston, Anna C., Khan, A., Orhand-Mainsant, Guenolé, Barrett, E., Gaudin, E., Kerjean, Laurent, Julien, Agnès, Nonon, M., Llorca-Cejudo, R., Laudet, Philippe, Maki, Justin, Mouret, Jean-Marie, Pont, Gabriel, Meunier, Frederic A., Rochas, Ludovic, de Larclause, Isabel Savin, Sylvestre-Baron, Annick, Trebi-Ollenu, Ashitey, Valladeau, J., Delage, P., Jacob, A., Calvet, Marie, Grotte, M., Rodríguez-Manfredi, José Antonio, Lekic, Vedran, Menina, Sabrina, Robertsson, John O.A., Spohn, Tilman, Tauzin, Benoit, Tharimena, S., and Pierick, Jen Ten
Abstract: InSight is the first planetary mission with a seismometer package, SEIS, since the Apollo Lunar Surface Experiments Package. SEIS is complimented by APSS, which has as a goal to document the atmospheric source of seismic noise and signals. Since June 2019, SEIS has been delivering 6 axis 20 sps continuous seismic data, a rate one order of magnitude larger originally planned. More than 50 events have been detected by the end of July 2019 but only three have amplitudes significantly above the SEIS instrument requirement. Two have clear and coherent arrivals of P and S waves, enabling location, diffusion/attenuation characterization and receiver function analysis. The event¿s magnitudes are likely ¿ 3 and no clear surface waves nor deep interior phases have been identified. This suggests deep events with scattering along their final propagation paths and with large propagation differences as compared to Earth and Moon quakes. Most of the event¿s detections are made possible due to the very low noise achieved by the instrument installation strategy and the very low VBB self-noise. Most of the SEIS signals have amplitudes of spectral densities in the 0.03-5Hz frequency bandwidth ranging from 10-10 m/s2/Hz1/2 to 5 10-9 m/s2/Hz1/2. The smallest noise levels occurs during the early night, with angstrom displacements or nano-radian tilts. This monitors the elastic and seismic interaction of a planetary surface with its atmosphere, illustrated not only by a wide range of SEIS signals correlated with pressure vortexes, dust devils or wind activity but also by modulation of resonances above 1 Hz, amplified by ultra-low velocity surface layers. After about one half of a Martian year, clear seasonal changes appear also in the noise, which will be discussed. One year after landing, the seismic noise is therefore better and better understood, and noise correction techniques begun to be implemented, either thanks to the APSS wind and pressure sensors, or by SEIS only data processing
Published: 2019

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