337 results on '"Panning, Mark"'
Search Results
2. First observations of core-transiting seismic phases on Mars
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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, Giardini, Domenico, 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
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Mars ,core evolution ,planetary structure - 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.
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- 2023
3. Different Martian Crustal Seismic Velocities Across the Dichotomy Boundary From Multi‐Orbiting Surface Waves
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Li, Jiaqi, Beghein, Caroline, Lognonné, Philippe, McLennan, Scott M, Wieczorek, Mark A, Panning, Mark P, Knapmeyer‐Endrun, Brigitte, Davis, Paul, and Banerdt, W Bruce
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surface wave ,marsquake ,Rayleigh wave ,porosity ,Mars ,dichotomy ,Meteorology & Atmospheric Sciences - Published
- 2023
4. Seismic detection of a deep mantle discontinuity within Mars by InSight
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Huang, Quancheng, Schmerr, Nicholas C, King, Scott D, Kim, Doyeon, Rivoldini, Attilio, Plesa, Ana-Catalina, Samuel, Henri, Maguire, Ross R, Karakostas, Foivos, Lekić, Vedran, Charalambous, Constantinos, Collinet, Max, Myhill, Robert, Antonangeli, Daniele, Drilleau, Mélanie, Bystricky, Misha, Bollinger, Caroline, Michaut, Chloé, Gudkova, Tamara, Irving, Jessica CE, Horleston, Anna, Fernando, Benjamin, Leng, Kuangdai, Nissen-Meyer, Tarje, Bejina, Frederic, Bozdağ, Ebru, Beghein, Caroline, Waszek, Lauren, Siersch, Nicki C, Scholz, John-Robert, Davis, Paul M, Lognonné, Philippe, Pinot, Baptiste, Widmer-Schnidrig, Rudolf, Panning, Mark P, Smrekar, Suzanne E, Spohn, Tilman, Pike, William T, Giardini, Domenico, and Banerdt, W Bruce
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Earth Sciences ,Physical Sciences ,Astronomical Sciences ,Geology ,Geophysics ,Earth ,Planet ,Extraterrestrial Environment ,Iron ,Mars ,Minerals ,interior of Mars ,mantle transition zone ,thermal evolution of Mars - Abstract
Constraining the thermal and compositional state of the mantle is crucial for deciphering the formation and evolution of Mars. Mineral physics predicts that Mars' deep mantle is demarcated by a seismic discontinuity arising from the pressure-induced phase transformation of the mineral olivine to its higher-pressure polymorphs, making the depth of this boundary sensitive to both mantle temperature and composition. Here, we report on the seismic detection of a midmantle discontinuity using the data collected by NASA's InSight Mission to Mars that matches the expected depth and sharpness of the postolivine transition. In five teleseismic events, we observed triplicated P and S waves and constrained the depth of this discontinuity to be 1,006 [Formula: see text] 40 km by modeling the triplicated waveforms. From this depth range, we infer a mantle potential temperature of 1,605 [Formula: see text] 100 K, a result consistent with a crust that is 10 to 15 times more enriched in heat-producing elements than the underlying mantle. Our waveform fits to the data indicate a broad gradient across the boundary, implying that the Martian mantle is more enriched in iron compared to Earth. Through modeling of thermochemical evolution of Mars, we observe that only two out of the five proposed composition models are compatible with the observed boundary depth. Our geodynamic simulations suggest that the Martian mantle was relatively cold 4.5 Gyr ago (1,720 to 1,860 K) and are consistent with a present-day surface heat flow of 21 to 24 mW/m2.
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- 2022
5. Spin state and deep interior structure of Mars from InSight radio tracking
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Le Maistre, Sébastien, Rivoldini, Attilio, Caldiero, Alfonso, Yseboodt, Marie, Baland, Rose-Marie, Beuthe, Mikael, Van Hoolst, Tim, Dehant, Véronique, Folkner, William M., Buccino, Dustin, Kahan, Daniel, Marty, Jean-Charles, Antonangeli, Daniele, Badro, James, Drilleau, Mélanie, Konopliv, Alex, Péters, Marie-Julie, Plesa, Ana-Catalina, Samuel, Henri, Tosi, Nicola, Wieczorek, Mark, Lognonné, Philippe, Panning, Mark, Smrekar, Suzanne, and Banerdt, W. Bruce
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- 2023
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6. InSight Constraints on the Global Character of the Martian Crust
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Wieczorek, Mark A, Broquet, Adrien, McLennan, Scott M, Rivoldini, Attilio, Golombek, Matthew, Antonangeli, Daniele, Beghein, Caroline, Giardini, Domenico, Gudkova, Tamara, Gyalay, Szilárd, Johnson, Catherine L, Joshi, Rakshit, Kim, Doyeon, King, Scott D, Knapmeyer‐Endrun, Brigitte, Lognonné, Philippe, Michaut, Chloé, Mittelholz, Anna, Nimmo, Francis, Ojha, Lujendra, Panning, Mark P, Plesa, Ana‐Catalina, Siegler, Matthew A, Smrekar, Suzanne E, Spohn, Tilman, and Banerdt, W Bruce
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mars ,crust ,crustal composition ,gravity ,seismology ,Astronomical and Space Sciences ,Geochemistry ,Geology - Abstract
Analyses of seismic data from the InSight mission have provided the first in situ constraints on the thickness of the crust of Mars. These crustal thickness constraints are currently limited to beneath the lander that is located in the northern lowlands, and we use gravity and topography data to construct global crustal thickness models that satisfy the seismic data. These models consider a range of possible mantle and core density profiles, a range of crustal densities, a low-density surface layer, and the possibility that the crustal density of the northern lowlands is greater than that of the southern highlands. Using the preferred InSight three-layer seismic model of the crust, the average crustal thickness of the planet is found to lie between 30 and 72 km. Depending on the choice of the upper mantle density, the maximum permissible density of the northern lowlands and southern highlands crust is constrained to be between 2,850 and 3,100 kg m−3. These crustal densities are lower than typical Martian basaltic materials and are consistent with a crust that is on average more felsic than the materials found at the surface. We argue that a substantial portion of the crust of Mars is a primary crust that formed during the initial differentiation of the planet. Various hypotheses for the origin of the observed intracrustal seisimic layers are assessed, with our preferred interpretation including thick volcanic deposits, ejecta from the Utopia basin, porosity closure, and differentiation products of a Borealis impact melt sheet.
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- 2022
7. The Lunar Geophysical Network Landing Sites Science Rationale
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Haviland, Heidi Fuqua, Weber, Renee C., Neal, Clive R., Lognonné, Philippe, Garcia, Raphaël F., Schmerr, Nicholas, Nagihara, Seiichi, Grimm, Robert, Currie, Douglas G., Dell'Agnello, Simone, Watters, Thomas R., Panning, Mark P., Johnson, Catherine L., Yamada, Ryuhei, Knapmeyer, Martin, Ostrach, Lillian R., Kawamura, Taichi, Petro, Noah, and Bremner, Paul M.
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,Physics - Geophysics - Abstract
The Lunar Geophysical Network (LGN) mission is proposed to land on the Moon in 2030 and deploy packages at four locations to enable geophysical measurements for 6-10 years. Returning to the lunar surface with a long-lived geophysical network is a key next step to advance lunar and planetary science. LGN will greatly expand our primarily Apollo-based knowledge of the deep lunar interior by identifying and characterizing mantle melt layers, as well as core size and state. To meet the mission objectives, the instrument suite provides complementary seismic, geodetic, heat flow, and electromagnetic observations. We discuss the network landing site requirements and provide example sites that meet these requirements. Landing site selection will continue to be optimized throughout the formulation of this mission. Possible sites include the P-5 region within the Procellarum KREEP Terrane (PKT; (lat:$15^{\circ}$; long:$-35^{\circ}$), Schickard Basin (lat:$-44.3^{\circ}$; long:$-55.1^{\circ}$), Crisium Basin (lat:$18.5^{\circ}$; long:$61.8^{\circ}$), and the farside Korolev Basin (lat:$-2.4^{\circ}$; long:$-159.3^{\circ}$). Network optimization considers the best locations to observe seismic core phases, e.g., ScS and PKP. Ray path density and proximity to young fault scarps are also analyzed to provide increased opportunities for seismic observations. Geodetic constraints require the network to have at least three nearside stations at maximum limb distances. Heat flow and electromagnetic measurements should be obtained away from terrane boundaries and from magnetic anomalies at locations representative of global trends. An in-depth case study is provided for Crisium. In addition, we discuss the consequences for scientific return of less than optimal locations or number of stations., Comment: 34 pages, 12 figures, 3 tables, 1 appendix. Accepted manuscript, The Planetary Science Journal
- Published
- 2021
8. Instrumentation for Planetary Exploration
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Klonicki-Ference, Emily F., Malaska, Michael J., Panning, Mark P., Waller, Sarah E., Gasda, Patrick J., Badescu, Viorel, editor, Zacny, Kris, editor, and Bar-Cohen, Yoseph, editor
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- 2023
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9. Potential Pitfalls in the Analysis and Structural Interpretation of Seismic Data from the Mars InSight Mission.
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Kim, Doyeon, Davis, Paul, Lekić, Ved, Maguire, Ross, Compaire, Nicolas, Schimmel, Martin, Stutzmann, Eleonore, C. E. Irving, Jessica, Lognonné, Philippe, Scholz, John-Robert, Clinton, John, Zenhäusern, Géraldine, Dahmen, Nikolaj, Deng, Sizhuang, Levander, Alan, Panning, Mark P, Garcia, Raphaël F, Giardini, Domenico, Hurst, Ken, Knapmeyer-Endrun, Brigitte, Nimmo, Francis, Pike, W Tom, Pou, Laurent, Schmerr, Nicholas, Stähler, Simon C, Tauzin, Benoit, Widmer-Schnidrig, Rudolf, and Banerdt, William B
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Earth Sciences ,Geology ,Geophysics ,Civil Engineering ,Geochemistry & Geophysics ,Civil engineering - 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 to seismic recordings on Earth, ground motion measurements acquired by SEIS on Mars are made under dramatically different ambient noise conditions, but 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 which 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. While the origins of 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 paper may not be exhaustive, we provide guidance on best practices for enhancing the robustness of structural interpretations.
- Published
- 2021
10. On-deck seismology: Lessons from InSight for future planetary seismology
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Panning, Mark P., Pike, W. Tom, Lognonné, Philippe, Banerdt, W. Bruce, Murdoch, Naomi, Banfield, Don, Charalambous, Constantinos, Kedar, Sharon, Lorenz, Ralph D., Marusiak, Angela G., McClean, John B., Nunn, Ceri, Stähler, Simon C., Stott, Alexander E., and Warren, Tristram
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Physics - Geophysics ,Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
Before deploying to the surface of Mars, the short-period (SP) seismometer of the InSight mission operated on deck for a total of 48 hours. This dataset can be used to understand how deck-mounted seismometers can be used in future landed missions to Mars, Europa, and other planetary bodies. While operating on deck, the SP seismometer showed signals comparable to the Viking-2 seismometer near 3 Hz where the sensitivity of the Viking instrument peaked. Wind sensitivity showed similar patterns to the Viking instrument, although amplitudes on InSight were ~80% larger for a given wind velocity. However, during the low wind evening hours the instrument noise levels at frequencies between 0.1 and 1 Hz were comparable to quiet stations on Earth, although deployment to the surface below the Wind and Thermal Shield lowered installation noise by roughly 40 dB in acceleration power. With the observed noise levels and estimated seismicity rates for Mars, detection probability for quakes for a deck-mounted instrument are low enough that up to years of on-deck recordings may be necessary to observe an event. Because the noise is dominated by wind acting on the lander, though, deck-mounted seismometers may be more practical for deployment on airless bodies, and it is important to evaluate the seismicity of the target body and the specific design of the lander. Detection probabilities for operation on Europa reach over 99% for some proposed seismicity models for a similar duration of operation if noise levels are comparable to low-wind time periods on Mars., Comment: 20 pages, 7 figures, accepted to Journal of Geophysical Research: Planets
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- 2020
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11. Moonquake-triggered mass wasting processes on icy satellites
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Mills, Mackenzie M., Pappalardo, Robert T., Panning, Mark P., Leonard, Erin J., and Howell, Samuel M.
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- 2023
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12. MSS/1: Single‐Station and Single‐Event Marsquake Inversion
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Drilleau, Mélanie, Beucler, Éric, Lognonné, Philippe, Panning, Mark P, Knapmeyer‐Endrun, Brigitte, Banerdt, W Bruce, Beghein, Caroline, Ceylan, Savas, Driel, Martin, Joshi, Rakshit, Kawamura, Taichi, Khan, Amir, Menina, Sabrina, Rivoldini, Attilio, Samuel, Henri, Stähler, Simon, Xu, Haotian, Bonnin, Mickaël, Clinton, John, Giardini, Domenico, Kenda, Balthasar, Lekic, Vedran, Mocquet, Antoine, Murdoch, Naomi, Schimmel, Martin, Smrekar, Suzanne E, Stutzmann, Éléonore, Tauzin, Benoit, and Tharimena, Saikiran
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InSight ,inversion ,seismology - Abstract
SEIS, the seismometer of the InSight mission, which landed on Mars on 26 November 2018, is monitoring the seismic activity of the planet. The goal of the Mars Structure Service (MSS) is to provide, as a mission product, the first average 1-D velocity model of Mars from the recorded InSight data. Prior to the mission, methodologies have been developed and tested to allow the location of the seismic events and estimation of the radial structure, using surface waves and body waves arrival times, and receiver functions. The paper describes these validation tests and compares the performance of the different algorithms to constrain the velocity model below the InSight station and estimate the 1-D average model over the great circle path between source and receiver. These tests were performed in the frame of a blind test, during which synthetic data were inverted. In order to propagate the data uncertainties on the output model distribution, Bayesian inversion techniques are mainly used. The limitations and strengths of the methods are assessed. The results show the potential of the MSS approach to retrieve the structure of the crust and underlying mantle. However, at this time, large quakes with clear surface waves have not yet been recorded by SEIS, which makes the estimation of the 1-D average seismic velocity model challenging. Additional locatable events, especially at large epicentral distances, and development of new techniques to fully investigate the data, will ultimately provide more constraints on the crust and mantle of Mars.
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- 2020
13. Enceladus as a potential oasis for life: Science goals and investigations for future explorations
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Choblet, Gaël, Tobie, Gabriel, Buch, Arnaud, Čadek, Ondrej, Barge, Laura M., Bēhounková, Marie, Camprubi, Eloi, Freissinet, Caroline, Hedman, Matt, Jones, Geraint, Lainey, Valery, Le Gall, Alice, Lucchetti, Alice, MacKenzie, Shannon, Mitri, Giuseppe, Neveu, Marc, Nimmo, Francis, Olsson-Francis, Karen, Panning, Mark, Postberg, Frank, Saur, Joachim, Schmidt, Jürgen, Sekine, Yasuhito, Shibuya, Takazo, Sotin, Christophe, Soucek, Ondrej, Szopa, Cyril, Usui, Tomohiro, Vance, Steven, and Van Hoolst, Tim
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- 2022
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14. Newly formed craters on Mars located using seismic and acoustic wave data from InSight
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Garcia, Raphael F., Daubar, Ingrid J., Beucler, Éric, Posiolova, Liliya V., Collins, Gareth S., Lognonné, Philippe, Rolland, Lucie, Xu, Zongbo, Wójcicka, Natalia, Spiga, Aymeric, Fernando, Benjamin, Speth, Gunnar, Martire, Léo, Rajšić, Andrea, Miljković, Katarina, Sansom, Eleanor K., Charalambous, Constantinos, Ceylan, Savas, Menina, Sabrina, Margerin, Ludovic, Lapeyre, Rémi, Neidhart, Tanja, Teanby, Nicholas A., Schmerr, Nicholas C., Bonnin, Mickaël, Froment, Marouchka, Clinton, John F., Karatekin, Ozgur, Stähler, Simon C., Dahmen, Nikolaj L., Durán, Cecilia, Horleston, Anna, Kawamura, Taichi, Plasman, Matthieu, Zenhäusern, Géraldine, Giardini, Domenico, Panning, Mark, Malin, Mike, and Banerdt, William Bruce
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- 2022
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15. Seismic Signals from Waves on Titan's Seas
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Stähler, Simon C., Panning, Mark P., Hadziioannou, Céline, Lorenz, Ralph, Vance, Steve, Klingbeil, Knut, and Kedar, Sharon
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Astrophysics - Earth and Planetary Astrophysics ,Physics - Geophysics - Abstract
Seismology is the main tool for inferring the deep interior structures of Earth and potentially also of other planetary bodies in the solar system. Terrestrial seismology is influenced by the presence of the ocean-generated microseismic signal, which sets a lower limit on the earthquake detection capabilities but also provides a strong energy source to infer the interior structure on scales from local to continental. Titan is the only other place in the solar system with permanent surface liquids and future lander missions there might carry a seismic package. Therefore, the presence of microseisms would be of great benefit for interior studies, but also for detecting storm-generated waves on the lakes remotely. We estimated the strength of microseismic signals on Titan, based on wind speeds predicted from modeled global circulation models interior structure. We find that storms of more than 2 m/s wind speed, would create a signal that is globally observable with a high-quality broadband sensor and observable to a thousand kilometer distance with a space-ready seismometer, such as the InSight instruments currently operating on the surface of Mars., Comment: 24 pages, 6 figures
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- 2019
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16. Measuring Fundamental and Higher Mode Surface Wave Dispersion on Mars From Seismic Waveforms
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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
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- 2020
17. Mars from the InSight: Seismology Beyond Earth
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Knapmeyer-Endrun, Brigitte, Banerdt, W. Bruce, Smrekar, Suzanne E., Lognonné, Philippe, Giardini, Domenico, Beghein, Caroline, Beucler, Éric, Bozdağ, Ebru, Clinton, John, Garcia, Raphael F., Irving, Jessica C. E., Kawamura, Taichi, Kedar, Sharon, Margerin, Ludovic, Panning, Mark P., Pike, Tom W., Plesa, Ana-Catalina, Schmerr, Nicholas, Teanby, Nicholas, Weber, Renee, Wieczorek, Mark, Barkaoui, Salma, Brinkman, Nienke, Ceylan, Savas, Charalambous, Constantinos, Compaire, Nicolas, Dahmen, Nikolaj, van Driel, Martin, Horleston, Anna, Huang, Quancheng, Hurst, Kenneth, Kenda, Balthasar, Khan, Amir, Kim, Doyeon, Knapmeyer, Martin, Li, Jiaqi, Menina, Sabrina, Murdoch, Naomi, Perrin, Clément, Schimmel, Martin, Stähler, Simon C., Stutzmann, Eléonore, Bezaeva, Natalia S., Series Editor, Gomes Coe, Heloisa Helena, Series Editor, Nawaz, Muhammad Farrakh, Series Editor, Vacareanu, Radu, editor, and Ionescu, Constantin, editor
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- 2022
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18. Development of elastic wave analyzer for icy sub-surfaces (EWAIS) in water-bearing worlds
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Lee, Hyeong Jae, primary, Bar-Cohen, Yoseph, additional, Badescu, Mircea, additional, Sherrit, Stewart, additional, Panning, Mark, additional, Vance, Steven D., additional, and Lih, Shyh-Shiuh, additional
- Published
- 2024
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19. Seismic wave detectability on Venus using ground deformation sensors, infrasound sensors on balloons and airglow imagers
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Garcia, Raphael F., primary, Zelst, Iris van, additional, Kawamura, Taichi, additional, Näsholm, Sven Peter, additional, Horleston, Anna Catherine, additional, Klaasen, Sara, additional, Lefevre, Maxence, additional, Solberg, Céline Marie, additional, Smolinski, Krystyna T., additional, Plesa, Ana-Catalina, additional, Brissaud, Quentin, additional, Maia, Julia S., additional, Stähler, Simon C., additional, Lognonné, Philippe, additional, Panning, Mark Paul, additional, Gülcher, Anna, additional, Ghail, Richard, additional, and Toffoli, Barbara De, additional
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- 2024
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20. Seismic response of the Mars Curiosity Rover: Implications for future planetary seismology
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Panning, Mark P. and Kedar, Sharon
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Physics - Geophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
Seismic measurements are an important tool for exploration of planetary interiors, but may not be included in missions due to perceived complexity in placement of sensitive instruments on the surface. To help address this concern, we assess the fidelity of recordings of ground motion by an instrument placed on the deck of the engineering model of the Mars Science Laboratory compared with an identical instrument placed on the ground directly beneath. Comparison of the recordings reveals clear recordings of teleseismic earthquakes on both instruments. The transfer function between the instruments demonstrates the deck instrument is affected by resonance frequencies of the lander, and does not faithfully record ground motion at these frequencies or higher. In addition, additional decoherence is observed near 1 Hz during periods of strong airflow due to air conditioning cycling. However, excellent coherence and a transfer function near 1 can be observed in the important seismic band between 2 and 30 seconds at all times and extending up to the lander resonances during the night time when air conditioning was not running. This suggests a deck-mounted seismic instrument may be able to provide valuable science return without requiring additional deployment complexity., Comment: 18 pages, 7 figures, submitted to Icarus in April, 2018; Supplementary material included as a pdf file with 21 supplementary figures; To view the supplementary material, please download and extract the gzipped tar source file listed under "Other formats"
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- 2018
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21. The marsquake catalogue from InSight, sols 0–1011
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Ceylan, Savas, Clinton, John F., Giardini, Domenico, Stähler, Simon C., Horleston, Anna, Kawamura, Taichi, Böse, Maren, Charalambous, Constantinos, Dahmen, Nikolaj L., van Driel, Martin, Durán, Cecilia, Euchner, Fabian, Khan, Amir, Kim, Doyeon, Plasman, Matthieu, Scholz, John-Robert, Zenhäusern, Géraldine, Beucler, Eric, Garcia, Raphaël F., Kedar, Sharon, Knapmeyer, Martin, Lognonné, Philippe, Panning, Mark P., Perrin, Clément, Pike, William T., Stott, Alexander E., and Banerdt, William B.
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- 2022
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22. Geophysical tests for habitability in ice-covered ocean worlds
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Vance, Steven D., Panning, Mark P., Stähler, Simon, Cammarano, Fabio, Bills, Bruce G., Kedar, Sharon, Sotin, Christophe, Pike, William T., Lorenz, Ralph, Tsai, Victor, Huang, Hsin-Hua, Jackson, Jennifer M., and Banerdt, Bruce
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Astrophysics - Earth and Planetary Astrophysics ,Physics - Geophysics - Abstract
Geophysical measurements can reveal the structure of icy ocean worlds and cycling of volatiles. The associated density, temperature, sound speed, and electrical conductivity of such worlds thus characterizes their habitability. To explore the variability and correlation of these parameters, and to provide tools for planning and data analyses, we develop 1-D calculations of internal structure, which use available constraints on the thermodynamics of aqueous MgSO$_4$, NaCl (as seawater), and NH$_3$, water ices, and silicate content. Limits in available thermodynamic data narrow the parameter space that can be explored: insufficient coverage in pressure, temperature, and composition for end-member salinities of MgSO$_4$ and NaCl, and for relevant water ices; and a dearth of suitable data for aqueous mixtures of Na-Mg-Cl-SO$_4$-NH$_3$. For Europa, ocean compositions that are oxidized and dominated by MgSO$_4$, vs reduced (NaCl), illustrate these gaps, but also show the potential for diagnostic and measurable combinations of geophysical parameters. The low-density rocky core of Enceladus may comprise hydrated minerals, or anydrous minerals with high porosity comparable to Earth's upper mantle. Titan's ocean must be dense, but not necessarily saline, as previously noted, and may have little or no high-pressure ice at its base. Ganymede's silicious interior is deepest among all known ocean worlds, and may contain multiple phases of high-pressure ice, which will become buoyant if the ocean is sufficiently salty. Callisto's likely near-eutectic ocean cannot be adequately modeled using available data. Callisto may also lack high-pressure ices, but this cannot be confirmed due to uncertainty in its moment of inertia.
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- 2017
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23. Seismic wave propagation in icy ocean worlds
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Stähler, Simon C., Panning, Mark P., Vance, Steve D., Lorenz, Ralph, van Driel, Martin, Nissen-Meyer, Tarje, and Kedar, Sharon
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Physics - Geophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Seismology was developed on Earth and shaped our model of the Earth's interior over the 20th century. With the exception of the Philae lander, all in situ extraterrestrial seismological effort to date was limited to other terrestrial planets. All have in common a rigid crust above a solid mantle. The coming years may see the installation of seismometers on Europa, Titan and Enceladus, so it is necessary to adapt seismological concepts to the setting of worlds with global oceans covered in ice. Here we use waveform analyses to identify and classify wave types, developing a lexicon for icy ocean world seismology intended to be useful to both seismologists and planetary scientists. We use results from spectral-element simulations of broadband seismic wavefields to adapt seismological concepts to icy ocean worlds. We present a concise naming scheme for seismic waves and an overview of the features of the seismic wavefield on Europa, Titan, Ganymede and Enceladus. In close connection with geophysical interior models, we analyze simulated seismic measurements of Europa and Titan that might be used to constrain geochemical parameters governing the habitability of a sub-ice ocean., Comment: 47 pages, 14 figures, accepted for publication in JGR Planets
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- 2017
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24. Expected seismicity and the seismic noise environment of Europa
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Panning, Mark P., Stähler, Simon C., Huang, Hsin-Hua, Vance, Steven D., Kedar, Sharon, Tsai, Victor C., Pike, W. T., and Lorenz, Ralph D.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
Seismic data will be a vital geophysical constraint on internal structure of Europa if we land instruments on the surface. Quantifying expected seismic activity on Europa both in terms of large, recognizable signals and ambient background noise is important for understanding dynamics of the moon, as well as interpretation of potential future data. Seismic energy sources will likely include cracking in the ice shell and turbulent motion in the oceans. We define a range of models of seismic activity in Europa's ice shell by assuming each model follows a Gutenberg-Richter relationship with varying parameters. A range of cumulative seismic moment release between $10^{16}$ and $10^{18}$ Nm/yr is defined by scaling tidal dissipation energy to tectonic events on the Earth's moon. Random catalogs are generated and used to create synthetic continuous noise records through numerical wave propagation in thermodynamically self-consistent models of the interior structure of Europa. Spectral characteristics of the noise are calculated by determining probabilistic power spectral densities of the synthetic records. While the range of seismicity models predicts noise levels that vary by 80 dB, we show that most noise estimates are below the self-noise floor of high-frequency geophones, but may be recorded by more sensitive instruments. The largest expected signals exceed background noise by $\sim$50 dB. Noise records may allow for constraints on interior structure through autocorrelation. Models of seismic noise generated by pressure variations at the base of the ice shell due to turbulent motions in the subsurface ocean may also generate observable seismic noise., Comment: 24 pages, 11 figures, Added in supplementary information from revision submission, including 3 audio files with sonification of Europa noise records. To view attachments, please download and extract the gzipped tar source file listed under "Other formats"
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- 2017
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25. Empirical Recurrence Rates for Seismic Signals on Planetary Surfaces
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Lorenz, Ralph and Panning, Mark
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Astrophysics - Earth and Planetary Astrophysics - Abstract
We review the recurrence intervals as a function of ground motion amplitude at several terrestrial locations, and make the first interplanetary comparison with measurements on the Moon, Mars, Venus and Titan. This empirical approach gives an intuitive guide to the relative seismicity of these locations, without invoking interior models and specific sources: for example a Venera-14 observation of possible ground motion indicates a microseismic environment mid-way between noisy and quiet terrestrial locations; quiet terrestrial regions see a peak velocity amplitude in mm/s roughly equal to 0.4*N(-0.7), where N is the number of events observed per year. The Apollo data show signals for a given recurrence rate are typically about 10,000 times smaller in amplitude than a quiet site on Earth, while Viking data masked for low-wind periods appears comparable with a quiet terrestrial site. Recurrence rate plots from in-situ measurements provide a convenient guide to expectations for seismic instrumentation on future planetary missions : while small geophones can discriminate terrestrial activity rates, observations with guidance accelerometers are typically too insensitive to provide meaningful constraints unless operated for long periods., Comment: 17 pages, 4 figures
- Published
- 2017
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26. Correction to: Instrumentation for Planetary Exploration
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Klonicki-Ference, Emily F., Malaska, Michael J., Panning, Mark P., Waller, Sarah E., Gasda, Patrick J., Badescu, Viorel, editor, Zacny, Kris, editor, and Bar-Cohen, Yoseph, editor
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- 2023
- Full Text
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27. Vital Signs: Seismology of ocean worlds
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Vance, Steven D., Kedar, Sharon, Panning, Mark P., Staehler, Simon C., Bills, Bruce G., Lorenz, Ralph D., Huang, Hsin-Hua, Pike, William T., Castillo, Julie C., Lognonne, Philippe, Tsai, Victor C., and Rhoden, Alyssa R.
- Subjects
Astrophysics - Earth and Planetary Astrophysics - Abstract
Ice-covered ocean worlds possess diverse energy sources and associated mechanisms that are capable of driving significant seismic activity, but to date no measurements of their seismic activity have been obtained. Such investigations could probe their transport properties and radial structures, with possibilities for locating and characterizing trapped liquids that may host life and yielding critical constraints on redox fluxes, and thus on habitability. Modeling efforts have examined seismic sources from tectonic fracturing and impacts. Here, we describe other possible seismic sources, their associations with science questions constraining habitability, and the feasibility of implementing such investigations. We argue, by analogy with the Moon, that detectable seismic activity on tidally flexed ocean worlds should occur frequently. Their ices fracture more easily than rocks, and dissipate more tidal energy than the <1 GW of the Moon and Mars. Icy ocean worlds also should create less thermal noise for a due to their greater distance and consequently smaller diurnal temperature variations. They also lack substantial atmospheres (except in the case of Titan) that would create additional noise. Thus, seismic experiments could be less complex and less susceptible to noise than prior or planned planetary seismology investigations of the Moon or Mars., Comment: 53 pages, 3 tables, 3 figures, accepted for publication in Astrobiology, 11/7/16: corrected lunar seismic dissipation number and associated reference; corrected radiogenic heat for Enceladus; no change to main arguments of the paper, 11/10/16: added figures omitted from previous revision, 06/12/17: substantially revised version accepted by Astrobiology
- Published
- 2016
28. The Farside Seismic Suite: A Novel Approach for Long-term Lunar Seismology
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Aboobaker, Asad, primary, Panning, Mark, additional, and Bugby, David, additional
- Published
- 2024
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29. The Last Days of Mars InSight
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Edgington, Scott G. C., primary, Ashley, James W., additional, Banerdt, W. Bruce, additional, Cameron, Jessica E., additional, Charlton, Blake R., additional, Garcia, Kathya Zamora, additional, Lever, Scott G., additional, Panning, Mark P., additional, Scott, Charles P., additional, and Stough, Emily Eelkema, additional
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- 2024
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30. Fiber Seismic Network on the Moon
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Wu, Wenbo, primary, Zhan, Zhongwen, additional, Panning, Mark, additional, and Klesh, Andrew, additional
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- 2024
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31. Wind and surface roughness considerations for seismic instrumentation on a relocatable lander for Titan
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Lorenz, Ralph D., Shiraishi, Hiroaki, Panning, Mark, and Sotzen, Kristin
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- 2021
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32. Initial results from the InSight mission on Mars
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Banerdt, W. Bruce, Smrekar, Suzanne E., Banfield, Don, Giardini, Domenico, Golombek, Matthew, Johnson, Catherine L., Lognonné, Philippe, Spiga, Aymeric, Spohn, Tilman, Perrin, Clément, Stähler, Simon C., Antonangeli, Daniele, Asmar, Sami, Beghein, Caroline, Bowles, Neil, Bozdag, Ebru, Chi, Peter, Christensen, Ulrich, Clinton, John, Collins, Gareth S., Daubar, Ingrid, Dehant, Véronique, Drilleau, Mélanie, Fillingim, Matthew, Folkner, William, Garcia, Raphaël F., Garvin, Jim, Grant, John, Grott, Matthias, Grygorczuk, Jerzy, Hudson, Troy, Irving, Jessica C. E., Kargl, Günter, Kawamura, Taichi, Kedar, Sharon, King, Scott, Knapmeyer-Endrun, Brigitte, Knapmeyer, Martin, Lemmon, Mark, Lorenz, Ralph, Maki, Justin N., Margerin, Ludovic, McLennan, Scott M., Michaut, Chloe, Mimoun, David, Mittelholz, Anna, Mocquet, Antoine, Morgan, Paul, Mueller, Nils T., Murdoch, Naomi, Nagihara, Seiichi, Newman, Claire, Nimmo, Francis, Panning, Mark, Pike, W. Thomas, Plesa, Ana-Catalina, Rodriguez, Sébastien, Rodriguez-Manfredi, Jose Antonio, Russell, Christopher T., Schmerr, Nicholas, Siegler, Matt, Stanley, Sabine, Stutzmann, Eléanore, Teanby, Nicholas, Tromp, Jeroen, van Driel, Martin, Warner, Nicholas, Weber, Renee, and Wieczorek, Mark
- Published
- 2020
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33. Development of elastic wave analyzer for icy sub-surfaces (EWAIS) in water-bearing worlds
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Gyekenyesi, Andrew L., Shull, Peter J., Wu, H. Felix, Yu, Tzuyang, Lee, Hyeong Jae, Bar-Cohen, Yoseph, Badescu, Mircea, Sherrit, Stewart, Panning, Mark, Vance, Steve, and Lih, Shyh-Shiuh
- Published
- 2024
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34. Planetary Seismology: Nearly 3 years on Mars, and a return to the Moon
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Yana, Charles, Weber, Renee, Walsh, William, Standley, Ian, de Raucourt, Sebastien, Pont, Gabriel, Pike, W. Tom, Nunn, Ceri, Lognonné, Philippe, Kawamura, Taichi, Garcia, Raphael, Elliott, John, Cutler, James, Calcutt, Simon, Bugby, David, Bowles, Neil, Kedar, Sharon, Tharimena, S, Tauzin, B, Stutzmann, E, Schimmel, M, Schmelzbach, C, Nunn, C, Murdoch, N, Lekic, V, Brinkman, N, Kenda, B, Fayon, L, Spiga, A, Stott, A. E, Stähler, S, Orhand-Mainsant, G, Knapmeyer, M, Khan, A, Horleston, A, van Driel, M, Charalambous, C, Ceylan, S, Böse, M, Drilleau, M, Hurst, K, Weber, R, Teanby, N, Schmerr, N, Mimoun, D, Margerin, L, Knapmeyer-Endrun, B, Kedar, S, Kawamura, T, Irving, J, Garcia, R, Clinton, J, Bozdag, E, Lorenz, R, Giardini, D, Pike, W.T, Lognonné, P, Banerdt, W.B, and Panning, Mark
- Published
- 2021
35. Planetary Seismology: Nearly 3 years on Mars, and a return to the Moon
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Panning, Mark, Banerdt, W.B, Lognonné, P, Pike, W.T, Giardini, D, Lorenz, R, Bozdag, E, Clinton, J, Garcia, R, Irving, J, Kawamura, T, Kedar, S, Knapmeyer-Endrun, B, Margerin, L, Mimoun, D, Schmerr, N, Teanby, N, Weber, R, Hurst, K, Drilleau, M, Böse, M, Ceylan, S, Charalambous, C, van Driel, M, Horleston, A, Khan, A, Knapmeyer, M, Orhand-Mainsant, G, Stähler, S, Stott, A. E, Spiga, A, Fayon, L, Kenda, B, Brinkman, N, Lekic, V, Murdoch, N, Nunn, C, Schmelzbach, C, Schimmel, M, Stutzmann, E, Tauzin, B, Tharimena, S, Kedar, Sharon, Bowles, Neil, Bugby, David, Calcutt, Simon, Cutler, James, Elliott, John, Garcia, Raphael, Kawamura, Taichi, Lognonné, Philippe, Nunn, Ceri, Pike, W. Tom, Pont, Gabriel, de Raucourt, Sebastien, Standley, Ian, Walsh, William, Weber, Renee, and Yana, Charles
- Published
- 2021
36. Two Seismic Events from InSight Confirmed as New Impacts on Mars
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Daubar, Ingrid J., primary, Fernando, Benjamin A., additional, Garcia, Raphaël F., additional, Grindrod, Peter M., additional, Zenhäusern, Géraldine, additional, Wójcicka, Natalia, additional, Teanby, Nicholas A., additional, Stähler, Simon C., additional, Posiolova, Liliya, additional, Horleston, Anna C., additional, Collins, Gareth S., additional, Charalambous, Constantinos, additional, Clinton, John, additional, Banks, Maria E., additional, Froment, Marouchka, additional, Lognonné, Philippe, additional, Panning, Mark, additional, and Banerdt, W. Bruce, additional
- Published
- 2023
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37. Identifying deep moonquake nests using machine learning model on single lunar station on the far side of the Moon
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Majstorović, Josipa, primary, Lognonné, Philippe, additional, Kawamura, Taichi, additional, and Panning, Mark Paul, additional
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- 2023
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38. Description of Martian Convective Vortices Observed by InSight and Implications for Vertical Vortex Structure and Subsurface Physical Properties
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Onodera, Keisuke, primary, Nishida, Kiwamu, additional, Kawamura, Taichi, additional, Murdoch, Naomi, additional, Drilleau, Mélanie, additional, Otsuka, Ryoji, additional, Lorenz, Ralph, additional, Horleston, Anna, additional, Widmer‐Schnidrig, Rudolf, additional, Schimmel, Martin, additional, Rodriguez, Sebastien, additional, Carrasco, Sebastián, additional, Tanaka, Satoshi, additional, Perrin, Clement, additional, Lognonné, Philippe, additional, Spiga, Aymeric, additional, Banfield, Don, additional, Panning, Mark, additional, and Banerdt, William Bruce, additional
- Published
- 2023
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39. The rheology and thermal history of Mars revealed by the orbital evolution of Phobos
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Samuel, Henri, Lognonné, Philippe, Panning, Mark, and Lainey, Valéry
- Subjects
Rheology -- Observations ,Mars (Planet) -- Natural history ,Orbits (Astrophysics) ,Astronomy ,Silicon compounds ,Space missions ,Silicates ,Environmental issues ,Science and technology ,Zoology and wildlife conservation - Abstract
The evolution and internal structure of Mars are, by comparison to its present-day surface, poorly known--although evidence of recent volcanic activity.sup.1 suggests that its deep interior remains hot and convectively cooling. The cooling rate of Mars is related to its early thermal state and to its rheology, which determines its ability to deform and to dynamically evolve.sup.2. Attempts to reconstruct the dynamic history of Mars and reveal its present-day structure, by combining the study of thermal evolution with surface observations, are limited by the interplay between several key quantities--including temperature, composition and rheology. Here we show that by considering Phobos (the closest satellite of Mars)--the orbital evolution of which is governed by the thermochemical history of Mars, through tidal interactions--we can gain insight into the thermal history and rheology of the planet. We investigated the long-term evolution of the main envelopes of Mars; these comprise a liquid metallic core that is overlain by a homogeneous silicate convecting mantle underneath an evolving heterogeneous lithospheric lid that includes a crust enriched in radiogenic elements. By exploiting the relationship between Mars and Phobos within an established in situ scenario for the early origin of the moons of Mars.sup.3, we find that--initially--Mars was moderately hotter (100 to 200 kelvin) than it is today, and that its mantle sluggishly deforms in the dislocation creep regime. This corresponds to a reference viscosity of 10.sup.22.2 [plus or minus] 0.5 pascal seconds and to a moderate to relatively weak intrinsic sensitivity of viscosity to temperature and pressure. Our approach predicts a present-day average crustal thickness of 40 [plus or minus] 25 kilometres and a surface heat flow of 20 [plus or minus] 1 milliwatts per square metre. We show that combining these predictions with data from future and ongoing space missions--such as InSight--could reduce uncertainties in Martian thermal and rheological histories, and help to uncover the origin of Phobos. Insights into the thermal and rheological history of Mars are generated by considering the interplay between the thermochemistry of the planet and the orbital evolution of its closest satellite, Phobos., Author(s): Henri Samuel [sup.1] , Philippe Lognonné [sup.1] , Mark Panning [sup.2] , Valéry Lainey [sup.2] Author Affiliations: (1) Institut de Physique du Globe de Paris, CNRS, Université Sorbonne Paris [...]
- Published
- 2019
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40. Farside Seismic Suite
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Yana, Charles, Weber, Renee, Walsh, William, Standley, Ian, de Raucourt, Sebastien, Pont, Gabriel, Pike, W. Tom, Nunn, Ceri, Lognonné, Philippe, Kawamura, Taichi, Garcia, Raphael, Elliott, John, Cutler, James, Calcutt, Simon, Bugby, David, Bowles, Neil, Kedar, Sharon, and Panning, Mark
- Published
- 2021
41. Farside Seismic Suite
- Author
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Panning, Mark, Kedar, Sharon, Bowles, Neil, Bugby, David, Calcutt, Simon, Cutler, James, Elliott, John, Garcia, Raphael, Kawamura, Taichi, Lognonné, Philippe, Nunn, Ceri, Pike, W. Tom, Pont, Gabriel, de Raucourt, Sebastien, Standley, Ian, Walsh, William, Weber, Renee, and Yana, Charles
- Published
- 2021
42. Europa Seismic Package
- Author
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Pierce, D, Blaes, B, Walsh, W, Vance, S, Stähler, S. C, Schmidt, B, Kedar, S, Hulbe, C, Calcutt, S, Bowles, N, Pike, W. T, and Panning, Mark
- Published
- 2021
43. Europa Seismic Package
- Author
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Panning, Mark, Pike, W. T, Bowles, N, Calcutt, S, Hulbe, C, Kedar, S, Schmidt, B, Stähler, S. C, Vance, S, Walsh, W, Blaes, B, and Pierce, D
- Published
- 2021
44. Solar System Pony Express: Data Mules on Cycler Orbits for High-Latency, Petabit-Scale Data Transfers
- Author
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Daubar, Ingrid, Woollands, Robyn, Panning, Mark, Parker, Wilson, Pellegrini, Etienne, Vander Hook, Joshua, and Sanchez Net, Marc
- Published
- 2021
45. Solar System Pony Express: Data Mules on Cycler Orbits for High-Latency, Petabit-Scale Data Transfers
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Sanchez Net, Marc, Vander Hook, Joshua, Pellegrini, Etienne, Parker, Wilson, Panning, Mark, Woollands, Robyn, and Daubar, Ingrid
- Published
- 2021
46. Systematic catalog of Martian convective vortices observed by InSight
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Onodera, Keisuke, primary, Nishida, Kiwamu, additional, Kawamura, Taichi, additional, Murdoch, Naomi, additional, Drilleau, Mélanie, additional, Otsuka, Ryoji, additional, Lorenz, Ralph D., additional, Horleston, Anna Catherine, additional, Widmer-Schnidrig, Rudolf, additional, Schimmel, Martin, additional, Rodriguez, Sebastien, additional, Carrasco, Sebastián, additional, Tanaka, Satoshi, additional, Perrin, Clement, additional, Lognonné, Philippe, additional, Spiga, Aymeric, additional, Banfield, Donald, additional, Panning, Mark Paul, additional, and Banerdt, William Bruce, additional
- Published
- 2023
- Full Text
- View/download PDF
47. Building a lunar network using a flexible, long-lived Lunar Geophysical Package (LGP)
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Walsh, William, Standley, Ian, Pike, W. Tom, Nunn, Ceri, Neal, Clive, Nagihara, Seichi, Lognonné, Philippe, Kawamura, Taichi, He, Yutao, Grimm, Robert E, Elliott, John, Currie, Doug, Calcutt, Simon, Bugby, David, Kedar, Sharon, Weber, Renee C, and Panning, Mark P
- Abstract
UNKNOWN
- Published
- 2020
48. The Influence and Detectability of Methane Clathrates on Seismic Velocity Structure: Applications to Titan and Icy Ocean Worlds
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Marusiak, Angela G, Vance, Steve, and Panning, Mark
- Published
- 2020
49. The Influence and Detectability of Methane Clathrates on Seismic Velocity Structure: Applications to Titan and Icy Ocean Worlds
- Author
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Panning, Mark, Vance, Steve, and Marusiak, Angela G
- Abstract
UNKNOWN
- Published
- 2020
50. The Influence and Detectability of Methane Clathrates on Seismic Velocity Structure: Applications to Titan and Icy Ocean Worlds
- Author
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Vance, Steve, Panning, Mark, and Marusiak, Angela G
- Abstract
UNKNOWN
- Published
- 2020
Catalog
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