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14 results on '"N. Wójcicka"'

1. Numerical Simulations of the Apollo S‐IVB Artificial Impacts on the Moon

Author

A. Rajšić, K. Miljković, N. Wójcicka, G. S. Collins, K. Onodera, T. Kawamura, P. Lognonné, M. A. Wieczorek, and I. J. Daubar

Subjects
impact cratering, numerical modeling, seismic moment, seismic efficiency, Moon, artificial impacts, Astronomy, QB1-991, Geology, QE1-996.5
Abstract

Abstract The third stage of the Saturn IV rocket used in the five Apollo missions made craters on the Moon ∼30 m in diameter. Their initial impact conditions were known, so they can be considered controlled impacts. Here, we used the iSALE‐2D shock physics code to numerically simulate the formation of these craters, and to calculate the vertical component of seismic moment (∼4 × 1010 Nm) and seismic efficiency (∼10−6) associated with these impacts. The irregular booster shape likely caused the irregular crater morphology observed. To investigate this, we modeled six projectile geometries, with footprint area between 3 and 105 m2, keeping the mass and velocity of the impactor constant. We showed that the crater depth and diameter decreased as the footprint area increased. The central mound observed in lunar impact sites could be a result of layering of the target and/or low density of the projectile. Understanding seismic signatures from impact events is important for planetary seismology. Calculating seismic parameters and validating them against controlled experiments in a planetary setting will help us understand the seismic data received, not only from the Moon, but also from the InSight Mission on Mars and future seismic missions.

Published
2021
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2. A New Crater Near Insight: Implications for Seismic Impact Detectability on Mars

Author

I. J. Daubar, P. Lognonné, N. A. Teanby, G. S. Collins, J. Clinton, S. Stähler, A. Spiga, F. Karakostas, S. Ceylan, M. Malin, A. S. McEwen, R. Maguire, C. Charalambous, K. Onodera, A. Lucas, L. Rolland, J. Vaubaillon, T. Kawamura, M. Böse, A. Horleston, M. Van Driel, J. Stevanović, K. Miljković, B. Fernando, Q. Huang, D. Giardini, C. S. Larmat, K. Leng, A. Rajšić, N. Schmerr, N. Wójcicka, T. Pike, J. Wookey, S. Rodriguez, R. Garcia, M. E. Banks, L. Margerin, L. Posiolova, and B. Banerdt

Subjects
Exobiology, Geosciences (General)
Abstract

A new 1.5 m diameter impact crater was discovered on Mars only ~40 km from the InSight lander. Context camera images constrained its formation between 21 February and 6 April 2019; follow-up High Resolution Imaging Science Experiment images resolved the crater. During this time period, three seismic events were identified in InSight data. We derive expected seismic signal characteristics and use them to evaluate each of the seismic events. However, none of them can definitively be associated with this source. Atmospheric perturbations are generally expected to be generated during impacts; however, in this case, no signal could be identified as related to the known impact. Using scaling relationships based on the terrestrial and lunar analogs and numerical modeling, we predict the amplitude, peak frequency, and duration of the seismic signal that would have emanated from this impact. The predicted amplitude falls near the lowest levels of the measured seismometer noise for the predicted frequency. Hence, it is not surprising this impact event was not positively identified in the seismic data. Finding this crater was a lucky event as its formation this close to InSight has a probability of only ~0.2, and the odds of capturing it in before and after images are extremely low. We revisit impact-seismic discriminators in light of real experience with a seismometer on the Martian surface. Using measured noise of the instrument, we revise our previous prediction of seismic impact detections downward, from ~a few to tens, to just ~2 per Earth year, still with an order of magnitude uncertainty.

Published
2020
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3. Seismic efficiency and seismic moment for small craters on mars formed in the layered uppermost crust

Author

A. Rajšić, K. Miljković, N. Wójcicka, G. S. Collins, R. F. Garcia, C. Bredemeyer, A. Lagain, I. J. Daubar, and P. Lognonné

Subjects
Geophysics, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous)
Abstract

Seismic activity generated by impacts depends on impact conditions and properties of the impact site. Here, we combined mapping of the regolith thickness with numerical impact simulations to better estimate the seismic efficiency and seismic moment generated in small impact events in the uppermost crust on Mars. We used mapping of crater morphology to determine the regolith thickness that craters formed in. We found that local regolith thickness in the late Amazonian units is between 4 and 9 m. Combined with previous estimates for the NASA InSight landing site, we composed a more realistic uppermost crust analog and implemented it in numerical impact simulations. We estimated the seismic efficiency and seismic moment for small craters on Mars impacting a non-porous or fractured bedrock overlaid by 5, 10, or 15 m thick regolith. Seismic energy showed more dependence on target properties. Three orders of magnitude more energy were produced in stronger targets. The seismic moment does not depend on target properties, and we confirm that seismic moment is almost proportional to impact momentum. The resulting seismic moment is in agreement up to a factor of 4 between different target types. We improved the scaling relationships developed from numerical simulations used in seismic moment approximations by constraining its dependence on more realistic target properties.

Published
2023

4. Largest recent impact craters on Mars: Orbital imaging and surface seismic co-investigation

Author

L. V. Posiolova, P. Lognonné, W. B. Banerdt, J. Clinton, G. S. Collins, T. Kawamura, S. Ceylan, I. J. Daubar, B. Fernando, M. Froment, D. Giardini, M. C. Malin, K. Miljković, S. C. Stähler, Z. Xu, M. E. Banks, É. Beucler, B. A. Cantor, C. Charalambous, N. Dahmen, P. Davis, M. Drilleau, C. M. Dundas, C. Durán, F. Euchner, R. F. Garcia, M. Golombek, A. Horleston, C. Keegan, A. Khan, D. Kim, C. Larmat, R. Lorenz, L. Margerin, S. Menina, M. Panning, C. Pardo, C. Perrin, W. T. Pike, M. Plasman, A. Rajšić, L. Rolland, E. Rougier, G. Speth, A. Spiga, A. Stott, D. Susko, N. A. Teanby, A. Valeh, A. Werynski, N. Wójcicka, G. Zenhäusern, Malin Space Science Systems (MSSS), UAR-Institut de physique du globe de Paris (IPGP-UAR / UAR3454), Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Swiss Seismological Service [ETH Zurich] (SED), Institute of Geophysics [ETH Zürich], Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)-Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Earth Science and Engineering [Imperial College London], Imperial College London, Institut für Geophysik [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Earth, Environmental and Planetary Sciences [Providence], Brown University, Department of Earth Sciences [Oxford], University of Oxford, Earth and Environmental Sciences Division [Los Alamos], Los Alamos National Laboratory (LANL), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), NASA Goddard Space Flight Center (GSFC), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), University of California [Los Angeles] (UCLA), University of California (UC), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), California Institute of Technology (CALTECH), University of Bristol [Bristol], Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), ANR-18-IDEX-0001,Université de Paris,Université de Paris(2018), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), and Science and Technology Facilities Council (STFC)

Subjects
[PHYS]Physics [physics], Multidisciplinary, General Science & Technology, [SDU]Sciences of the Universe [physics], [NLIN]Nonlinear Sciences [physics]
Abstract

International audience; Two >130-meter-diameter impact craters formed on Mars during the later half of 2021. These are the two largest fresh impact craters discovered by the Mars Reconnaissance Orbiter since operations started 16 years ago. The impacts created two of the largest seismic events (magnitudes greater than 4) recorded by InSight during its 3-year mission. The combination of orbital imagery and seismic ground motion enables the investigation of subsurface and atmospheric energy partitioning of the impact process on a planet with a thin atmosphere and the first direct test of martian deep-interior seismic models with known event distances. The impact at 35°N excavated blocks of water ice, which is the lowest latitude at which ice has been directly observed on Mars.

Published
2022
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5. Seismic constraints from a Mars impact experiment using InSight and Perseverance

Author

Manish R. Patel, Nicholas A Teanby, Taichi Kawamura, Matthieu Plasman, Marouchka Froment, Tarje Nissen-Meyer, N. Wójcicka, Philippe Lognonné, Constantinos Charalambous, Nikolaj Dahmen, Lilya Posiolova, A. Stott, Simon Stähler, Géraldine Zenhäusern, Anna Horleston, Benjamin Fernando, Aymeric Spiga, Lucie Rolland, Ingrid Daubar, Bruce Banerdt, Ross Maguire, John Clinton, Carene Larmat, Özgür Karatekin, Gareth S. Collins, Savas Ceylan, Matthew P. Golombek, Domenico Giardini, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Science and Technology Facilities Council (STFC), Department of Earth Sciences [Oxford], University of Oxford, Department of Earth Science and Engineering [Imperial College London], Imperial College London, Department of Geology [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Michigan State University [East Lansing], Michigan State University System, Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Department of Electrical and Electronic Engineering [London] (DEEE), Earth and Environmental Sciences Division [Los Alamos], Los Alamos National Laboratory (LANL), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), School of Earth Sciences [Bristol], University of Bristol [Bristol], Royal Observatory of Belgium [Brussels] (ROB), The Open University [Milton Keynes] (OU), Malin Space Science Systems (MSSS), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut Pierre-Simon-Laplace (IPSL (FR_636)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Department of Earth, Environmental and Planetary Sciences [Providence], Brown University, This paper constitutes InSight contribution number 218 and LA-UR-21-26319. B.F. and T.N.-M. are supported by the Natural Environment Research Council under the Oxford Environmental Research Doctoral Training Partnership, and the UK Space Agency Aurora grant ST/S001379/1. M.R.P. acknowledges support from the UK Space Agency (grants ST/S00145X/1 and ST/V002295/1). A.H. is funded by the UK Space Agency (grant ST/R002096/1). N.W. and G.S.C. are funded by UK Space Agency grants ST/S001514/1 and ST/T002026/1. S.C.S., G.Z., J.C. and N.D. acknowledge support from ETH Zürich through the ETH+ funding scheme (ETH+02 19-1: ‘Planet Mars’). N.A.T. is funded by UK Space Agency grants ST/R002096/1 and ST/T002972/1. M.F. and C.L. are funded by the Center for Space and Earth Science of Los Alamos National Laboratory. P.L., T.K., A.S., A.E.S., L.R. and M.F. acknowledge the support of CNES and of ANR (MAGIS, ANR-19-CE31-0008-08) for SEIS science support. I.J.D. is supported by NASA InSight Participating Scientist grant 80NM0018F0612. O.K. acknowledges the support of the Belgian Science Policy Office (BELSPO) through the ESA/PRODEX programme. A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA., and ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019)

Subjects
Martian, Spacecraft, business.industry, Mars landing, Mars, NASA InSight Mission, Astronomy and Astrophysics, Atmosphere of Mars, Mars Exploration Program, Seismic wave, Planet, [SDU]Sciences of the Universe [physics], Inner planets, Martian surface, Impacts, Traitement du signal et de l'image, business, Seismology, Geology
Abstract

NASA's InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission has operated a sophisticated suite of seismology and geophysics instruments on the surface of Mars since its arrival in 2018. On 18 February 2021, we attempted to detect the seismic and acoustic waves produced by the entry, descent and landing of the Perseverance rover using the sensors onboard the InSight lander. Similar observations have been made on Earth using data from both crewed(1,2) and uncrewed(3,4) spacecraft, and on the Moon during the Apollo eras(5), but never before on Mars or another planet. This was the only seismic event to occur on Mars since InSight began operations that had an a priori known and independently constrained timing and location. It therefore had the potential to be used as a calibration for other marsquakes recorded by InSight. Here we report that no signal from Perseverance's entry, descent and landing is identifiable in the InSight data. Nonetheless, measurements made during the landing window enable us to place constraints on the distance-amplitude relationships used to predict the amplitude of seismic waves produced by planetary impacts and place in situ constraints on Martian impact seismic efficiency (the fraction of the impactor kinetic energy converted into seismic energy)., Nature Astronomy, 6 (1), ISSN:2397-3366

Published
2022
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6. Numerical Simulations of the Apollo S‐IVB Artificial Impacts on the Moon

Author

Taichi Kawamura, A. Rajsic, N. Wójcicka, Katarina Miljković, Mark A. Wieczorek, P. H. Lognonné, Ingrid Daubar, Gareth S. Collins, and Keisuke Onodera

Subjects
QE1-996.5, biology, Astronomy, Apollo, artificial impacts, QB1-991, Geology, seismic efficiency, Environmental Science (miscellaneous), biology.organism_classification, numerical modeling, Impact crater, impact cratering, General Earth and Planetary Sciences, Seismic moment, Moon, Seismology, seismic moment
Abstract

The third stage of the Saturn IV rocket used in the five Apollo missions made craters on the Moon ∼30 m in diameter. Their initial impact conditions were known, so they can be considered controlled impacts. Here, we used the iSALE‐2D shock physics code to numerically simulate the formation of these craters, and to calculate the vertical component of seismic moment (∼4 × 1010 Nm) and seismic efficiency (∼10−6) associated with these impacts. The irregular booster shape likely caused the irregular crater morphology observed. To investigate this, we modeled six projectile geometries, with footprint area between 3 and 105 m2, keeping the mass and velocity of the impactor constant. We showed that the crater depth and diameter decreased as the footprint area increased. The central mound observed in lunar impact sites could be a result of layering of the target and/or low density of the projectile. Understanding seismic signatures from impact events is important for planetary seismology. Calculating seismic parameters and validating them against controlled experiments in a planetary setting will help us understand the seismic data received, not only from the Moon, but also from the InSight Mission on Mars and future seismic missions.

Published
2021

7. Listening for the Landing: Seismic Detections of Perseverance's Arrival at Mars With InSight

Author

Foivos Karakostas, N. Wójcicka, Tarje Nissen-Meyer, Nicholas A Teanby, Eleanor K. Sansom, Carene Larmat, Gareth S. Collins, Ross Maguire, Bruce Banerdt, Kuangdai Leng, Marouchka Froment, Benjamin Fernando, Aymeric Spiga, Özgür Karatekin, Philippe Lognonné, Taichi Kawamura, Lucie Rolland, Ingrid Daubar, Simon Stähler, Domenico Giardini, University of Oxford, Imperial College London, Los Alamos National Laboratory (LANL), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Maryland [College Park], University of Maryland System, Michigan State University [East Lansing], Michigan State University System, Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Royal Observatory of Belgium [Brussels] (ROB), Curtin University [Perth], Planning and Transport Research Centre (PATREC), University of Bristol [Bristol], Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), California Institute of Technology (CALTECH), Brown University, ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), University of Oxford [Oxford], Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris)

Subjects
QE1-996.5, 010504 meteorology & atmospheric sciences, seismoacoustics, Astronomy, Mars, QB1-991, Geology, Mars Exploration Program, Environmental Science (miscellaneous), seismology, 01 natural sciences, impacts, InSight, 13. Climate action, [SDU]Sciences of the Universe [physics], 0103 physical sciences, General Earth and Planetary Sciences, Active listening, 010303 astronomy & astrophysics, Seismology, 0105 earth and related environmental sciences
Abstract

International audience; The entry, descent, and landing (EDL) sequence of NASA's Mars 2020 Perseverance Rover will act as a seismic source of known temporal and spatial localization. We evaluate whether the signals produced by this event will be detectable by the InSight lander (3,452 km away), comparing expected signal amplitudes to noise levels at the instrument. Modeling is undertaken to predict the propagation of the acoustic signal (purely in the atmosphere), the seismoacoustic signal (atmosphere-to-ground coupled), and the elastodynamic seismic signal (in the ground only). Our results suggest that the acoustic and seismoacoustic signals, produced by the atmospheric shock wave from the EDL, are unlikely to be detectable due to the pattern of winds in the martian atmosphere and the weak air-to-ground coupling, respectively. However, the elastodynamic seismic signal produced by the impact of the spacecraft's cruise balance masses on the surface may be detected by InSight. The upper and lower bounds on predicted ground velocity at InSight are 2.0 × 10 −14 and 1.3 × 10 −10 m s −1. The upper value is above the noise floor at the time of landing 40% of the time on average. The large range of possible values reflects uncertainties in the current understanding of impact-generated seismic waves and their subsequent propagation and attenuation through Mars. Uncertainty in the detectability also stems from the indeterminate instrument noise level at the time of this future event. A positive detection would be of enormous value in constraining the seismic properties of Mars, and in improving our understanding of impact-generated seismic waves.

Published
2021
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8. Seismic Efficiency for Simple Crater Formation in the Martian Top Crust Analog

Author

A. Rajsic, Katarina Miljković, Gareth S. Collins, N. Wójcicka, Mark A. Wieczorek, Kai Wünnemann, Ingrid Daubar, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France, and Science and Technology Facilities Council (STFC)

Subjects
010504 meteorology & atmospheric sciences, Mars, Numerical modeling, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, seismic efficiency, 01 natural sciences, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Impact crater, impact cratering, Geochemistry and Petrology, Simple (abstract algebra), 0103 physical sciences, 0201 Astronomical and Space Sciences, Earth and Planetary Sciences (miscellaneous), 0402 Geochemistry, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Martian, Crust, Mars Exploration Program, Geophysics, numerical modeling, 0403 Geology, 13. Climate action, Space and Planetary Science, iSALE‐2D code, InSight mission, Geology
Abstract

The first seismometer operating on the surface of another planet was deployed by the NASA InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission to Mars. It gives us an opportunity to investigate the seismicity of Mars, including any seismic activity caused by small meteorite bombardment. Detectability of impact generated seismic signals is closely related to the seismic efficiency, defined as the fraction of the impactor's kinetic energy transferred into the seismic energy in a target medium. This work investigated the seismic efficiency of the Martian near surface associated with small meteorite impacts on Mars. We used the iSALE‐2D (Impact‐Simplified Arbitrary Lagrangian Eulerian) shock physics code to simulate the formation of the meter‐size impact craters, and we used a recently formed 1.5 m diameter crater as a case study. The Martian crust was simulated as unfractured nonporous bedrock, fractured bedrock with 25% porosity, and highly porous regolith with 44% and 65% porosity. We used appropriate strength and porosity models defined in previous works, and we identified that the seismic efficiency is very sensitive to the speed of sound and elastic threshold in the target medium. We constrained the value of the impact‐related seismic efficiency to be between the order of ∼10‐7 to 10‐6 for the regolith and ∼10‐4 to 10‐3 for the bedrock. For new impacts occurring on Mars, this work can help understand the near‐surface properties of the Martian crust, and it contributes to the understanding of impact detectability via seismic signals as a function of the target media.

Published
2021
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9. Seismic efficiency of Martian upper crust simulant

Author

A. Rajsic, Gareth S. Collins, Kai Wünnemann, N. Wójcicka, Mark A. Wieczorek, Katarina Miljković, and Ingrid Daubar

Subjects
Martian, Upper crust, Petrology, Geology
Abstract

Introduction: Meteoroid bombardment is one of the sources of seismic activity on planetary bodies. The very first seismometer operating on the surface of another planet was successfully deployed by the NASA InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission to Mars. It gives us an opportunity to investigate the seismicity of Mars, including impact-induced seismic activity. This work investigated the seismic efficiency associated with small meteorite impacts on Mars, using numerical methods in targets analogue to the Martian surface. The Martian crust was simulated as non-porous bedrock (0% porosity) or regolith with different porosities (25%, 44% and 65%) The seismic efficiency, k, is presented as a portion of impact energy that is transferred into seismic energy. It has been suspected that consolidated (bedrock) and non-consolidated (regolith) materials will have different values of seismic efficiency. Estimates of seismic efficiency range from k=10-2 to 10-6 (Schultz and Gault, 1975; Daubar et al., 2018; McGarr et al., 1969; Hoerth et al., 2014; Richardson & Kedar, 2013; Güldemeister & Wünnemann, 2017). High seismic efficiency is typical in bedrock or highly consolidated materials (k>10-3). Low seismic efficiency is typical for sediments or unconsolidated sands and soils (k-5) (e.g., Patton and Walter 1993). In this work, we used a simplified approach (e.g. Güldemeister & Wünnemann, 2017) that defines the seismic efficiency as: ; where x represents distance from the impact point, P is the amplitude of the pressure pulse, t is the duration of the pressure pulse, ρ is the density of the target, Cp is the speed of sound in the target and Ek is the kinetic energy of the impactor. Numerical impact modelling: All simulations were performed with the iSALE-2D shock physics hydrocode (Collins, et al., 2004; Wünnemann et al., 2006). The impact conditions were modelled to replicate recent fresh meter size impact that occurred on Mars since the landing of InSight (Daubar et al., 2020). Impact crater was estimated to be ~1.5 m in diameter. Impactor radius was 4.4 cm and kinetic energy of 1.8x106 J. To simulate bedrock and fractured bedrock (25% porosity) we used the ROCK strength model (Collins et al., 2004). To simulate the regolith (44% and 65% porosity) we used Lundborg strength model (Lundborg, 1968) (Table 1). We used the Tillotsen equation of state for basalt (Tillotson, 1962; Wójcicka et al., 2020). For porous cases, we used the ε-α porosity model (Wünnemann et al., 2006;) (Table 2). Table 1. Strength model parameters for targets with different porosity Parameter 0% 25% 44% 65% Strength model ROCK ROCK LUNDD LUNDD Strength (damaged) (kPa) 10 0 10 0.3 Friction (damaged) 0.6 0.67 0.7 0.7 Limiting strength (damaged) (GPa) 3.5 0.17 0.25 0.25 Strength (intact) (MPa) 10 0.2 Friction (intact) 1.2 1.8 Limiting strength (intact) (GPa) 3.5 0.17 Table 2. ε-α porosity model parameters (Borg et al., 2005; Wünnemann et al., 2006; Wójcicka et al, 2020). Parameter 25% 44% 65% Initial distension, α 1.33 1.8 2.8 Elastic threshold, ε0 -4x10-4 10-4 10-5 Distension at transition αx 1.1 1.15 1.0 The rate change of distension with respect to volumetric strain, k 0.98 0.98 0.98 Ratio of speed of sound in porous over non-porous medium, χ 0.6 0.33 0.21 All variables in the equation for the seismic efficiency were calculated from iSALE outputs. The pressure wave was observed via gauges cells, placed at 45° equidistantly throughout the target. The pressure wave amplitude and pulse duration were calculated at full width half maximum. The sound speed was calculated from assumed bulk modulus of basalt (Wójcicka et al, 2020). Results: Seismic efficiency was calculated for the same impact conditions in all four material models, representing the reference 1.5 m crater recently observed on Mars. There is a clear decrease in seismic efficiency with increasing porosity. It is of the order of 10-5 for porous and highly porous regolith and 10-4 for fractured bedrock. Estimates for the non-porous basalt bedrock are in the order of 10-3 (Figure 1). Porosity of the target affected pressure wave amplitudes, duration of the pressure pulse and speed of sound in the target. These are all parameters used in calculation of seismic efficiency. This implies that if impact occurs on very dusty parts of Mars with thick regolith cover, efficiency would be smaller than efficiency of the impact that occurred on the bedrock, or area with thinner regolith cover. Figure 1. Seismic efficiency calculated in targets with different porosity Conclusions. Impact cratering represents one of the most important geological processes in the Solar System. Defining relationship between target’s properties and seismic efficiency is of interest to the NASA InSight science, since it helps in understanding the properties of the uppermost crust on Mars. Previous approximations of seismic efficiency were of 2x10-5 with an order of magnitude uncertainty for seismic efficiency on Mars (Teanby and Wookey, 2011) and Daubar et al. (2018) adopted the seismic efficiency of 5x10-4 calculated from the seismic moment (Gudkova et al., 2011; 2015; Teanby 2015). In this work, we calculated the seismic efficiency in meter-size impacts on Mars to be different for bedrock (order of 10-3) and porous materials (order of 10-5).

Published
2020
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10. The seismic moment and seismic efficiency of small impacts on Mars

Author

Katarina Miljković, Ingrid Daubar, N. Wójcicka, Nicholas A Teanby, A. Rajsic, Gareth S. Collins, Ian D. Bastow, Philippe Lognonné, and Science and Technology Facilities Council (STFC)

Subjects
Mars Exploration Program, seismic efficiency, Geophysics, 0403 Geology, Space and Planetary Science, Geochemistry and Petrology, 0201 Astronomical and Space Sciences, Earth and Planetary Sciences (miscellaneous), impact, 0402 Geochemistry, Seismic moment, mars, Seismology, Geology, seismic activity, InSight
Abstract

Since landing in late 2018, the InSight lander has been recording seismic signals on the surface of Mars. Despite nominal pre-landing estimates of 1–3 meteorite impacts detected per Earth year, none have yet been identified seismically. To inform revised detectability estimates, we simulated numerically a suite of small impacts onto Martian regolith and characterized their seismic source properties. For the impactor size and velocity range most relevant for InSight, crater diameters are 1-30 m. We found that in this range scalar seismic moment is 106 − 1010 Nm and increases almost linearly with impact momentum. The ratio of horizontal to vertical seismic moment tensor components is ∼1, implying an almost isotropic P-wave source, for vertical impacts. Seismic efficiencies are ∼ 10−6, dependent on the target crushing strength and impact velocity. Our predictions of relatively low seismic efficiency and seismic moment suggest that meteorite impact detectability on Mars is lower than previously assumed. Detection chances are best for impacts forming craters of diameter >10m

Published
2020
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11. A New Crater Near InSight: Implications for Seismic Impact Detectability on Mars

Author

Domenico Giardini, Philippe Lognonné, Carene Larmat, Maria E. Banks, Jeremie Vaubaillon, Taichi Kawamura, Foivos Karakostas, L. Posiolova, Gareth S. Collins, Raphaël F. Garcia, Aymeric Spiga, Bruce Banerdt, K. Onodera, Michael C. Malin, Maren Böse, Sebastien Rodriguez, Ross Maguire, Savas Ceylan, Nicholas Schmerr, T. Pike, John Clinton, N. Wójcicka, M. van Driel, Quancheng Huang, Alfred S. McEwen, James Wookey, Benjamin Fernando, Kuangdai Leng, A. Rajsic, Antoine Lucas, Nicholas A Teanby, Lucie Rolland, Ingrid Daubar, Simon Stähler, Anna Horleston, Katarina Miljković, Jennifer Stevanović, Ludovic Margerin, Constantinos Charalambous, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut de Physique du Globe de Paris, School of Earth Sciences [Bristol], University of Bristol [Bristol], Department of Earth Science and Engineering [Imperial College London], Imperial College London, Swiss Seismological Service, Institute of Geophysics [ETH Zürich], Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), National Institute of Standards and Technology [Gaithersburg] (NIST), Los Alamos National Laboratory (LANL), Laboratoire de Génie Civil et Génie Mécanique (LGCGM), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA), Department of Geology [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Centre d'Etude de Saclay, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), NASA Goddard Space Flight Center (GSFC), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), DP180100661 and DE180100584, Australian Research Council, ST/S000615/1 and ST/S001514/1, Science and Technology Facilities Council, ETH‐06 17‐02, International Foundation for Ethical Research, ST/R002096/1, UK Space Agency, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Swiss Seismological Service [ETH Zurich] (SED), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)-Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), University of Arizona, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Institut de Physique du Globe de Paris (IPG Paris), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), ANR-14-CE36-0012,SEISMARS,Seismology on Mars(2014), and Science and Technology Facilities Council (STFC)

Subjects
Seismometer, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Mars, Context (language use), seismology, 01 natural sciences, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Impact crater, Geochemistry and Petrology, impact cratering, Martian surface, 0201 Astronomical and Space Sciences, Earth and Planetary Sciences (miscellaneous), 0402 Geochemistry, 0105 earth and related environmental sciences, Event (probability theory), InSight, crater, Mars Exploration Program, Geophysics, Amplitude, Mars cratering, 0403 Geology, 13. Climate action, Space and Planetary Science, Seismology, Geology, Noise (radio)
Abstract

A new 1.5 m diameter impact crater was discovered on Mars only ~40 km from the InSight lander. Context camera images constrained its formation between 21 February and 6 April 2019; follow‐up High Resolution Imaging Science Experiment images resolved the crater. During this time period, three seismic events were identified in InSight data. We derive expected seismic signal characteristics and use them to evaluate each of the seismic events. However, none of them can definitively be associated with this source. Atmospheric perturbations are generally expected to be generated during impacts; however, in this case, no signal could be identified as related to the known impact. Using scaling relationships based on the terrestrial and lunar analogs and numerical modeling, we predict the amplitude, peak frequency, and duration of the seismic signal that would have emanated from this impact. The predicted amplitude falls near the lowest levels of the measured seismometer noise for the predicted frequency. Hence, it is not surprising this impact event was not positively identified in the seismic data. Finding this crater was a lucky event as its formation this close to InSight has a probability of only ~0.2, and the odds of capturing it in before and after images are extremely low. We revisit impact‐seismic discriminators in light of real experience with a seismometer on the Martian surface. Using measured noise of the instrument, we revise our previous prediction of seismic impact detections downward, from ~a few to tens, to just ~2 per Earth year, still with an order of magnitude uncertainty. ISSN:0148-0227 ISSN:2169-9097 ISSN:2169-9100

Published
2020
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12. Seismically detected cratering on Mars: Enhanced recent impact flux?

Author

Daubar IJ, Garcia RF, Stott AE, Fernando B, Collins GS, Dundas CM, Wójcicka N, Zenhäusern G, McEwen AS, Stähler SC, Golombek M, Charalambous C, Giardini D, Lognonné P, and Banerdt WB

Abstract

Seismic observations of impacts on Mars indicate a higher impact flux than previously measured. Using six confirmed seismic impact detections near the NASA InSight lander and two distant large impacts, we calculate appropriate scalings to compare these rates with lunar-based chronology models. We also update the impact rate from orbital observations using the most recent catalog of new craters on Mars. The snapshot of the current impact rate at Mars recorded seismically is higher than that found using orbital detections alone. The measured rates differ between a factor of 2 and 10, depending on the diameter, although the sample size of seismically detected impacts is small. The close timing of the two largest new impacts found on Mars in the past few decades indicates either a heightened impact rate or a low-probability temporal coincidence, perhaps representing recent fragmentation of a parent body. We conclude that seismic methods of detecting current impacts offer a more complete dataset than orbital imaging.

Published
2024
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13. An estimate of the impact rate on Mars from statistics of very-high-frequency marsquakes.

Author

Zenhäusern G, Wójcicka N, Stähler SC, Collins GS, Daubar IJ, Knapmeyer M, Ceylan S, Clinton JF, and Giardini D

Abstract

The number density of impact craters on a planetary surface is used to determine its age, which requires a model for the production rate of craters of different sizes. On Mars, however, estimates of the production rate of small craters (<60 m) from orbital imagery and from extrapolation of lunar impact data do not match. Here we provide a new independent estimate of the impact rate by analysing the seismic events recorded by the seismometer onboard NASA's InSight lander. Some previously confirmed seismically detected impacts are part of a larger class of marsquakes (very high frequency, VF). Although a non-impact origin cannot be definitively excluded for each VF event, we show that the VF class as a whole is plausibly caused by meteorite impacts. We use an empirical scaling relationship to convert between seismic moment and crater diameter. Applying area and time corrections to derive a global impact rate, we find that 280-360 craters >8 m diameter are formed globally per year, consistent with previously published chronology model rates and above the rates derived from freshly imaged craters. Our work shows that seismology is an effective tool for determining meteoroid impact rates and complements other methods such as orbital imaging., Competing Interests: Competing interestsThe authors declare no competing interests., (© The Author(s) 2024.)

Published
2024
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14. Largest recent impact craters on Mars: Orbital imaging and surface seismic co-investigation.

Author

Posiolova LV, Lognonné P, Banerdt WB, Clinton J, Collins GS, Kawamura T, Ceylan S, Daubar IJ, Fernando B, Froment M, Giardini D, Malin MC, Miljković K, Stähler SC, Xu Z, Banks ME, Beucler É, Cantor BA, Charalambous C, Dahmen N, Davis P, Drilleau M, Dundas CM, Durán C, Euchner F, Garcia RF, Golombek M, Horleston A, Keegan C, Khan A, Kim D, Larmat C, Lorenz R, Margerin L, Menina S, Panning M, Pardo C, Perrin C, Pike WT, Plasman M, Rajšić A, Rolland L, Rougier E, Speth G, Spiga A, Stott A, Susko D, Teanby NA, Valeh A, Werynski A, Wójcicka N, and Zenhäusern G

Abstract

Two >130-meter-diameter impact craters formed on Mars during the later half of 2021. These are the two largest fresh impact craters discovered by the Mars Reconnaissance Orbiter since operations started 16 years ago. The impacts created two of the largest seismic events (magnitudes greater than 4) recorded by InSight during its 3-year mission. The combination of orbital imagery and seismic ground motion enables the investigation of subsurface and atmospheric energy partitioning of the impact process on a planet with a thin atmosphere and the first direct test of martian deep-interior seismic models with known event distances. The impact at 35°N excavated blocks of water ice, which is the lowest latitude at which ice has been directly observed on Mars.

Published
2022
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