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Your search keyword '"N. Wójcicka"' showing total 4 results
Start Over Author "N. Wójcicka" Topic earth and planetary sciences (miscellaneous)
4 results on '"N. Wójcicka"'

1. 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

2. 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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3. 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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4. 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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