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Space Science Reviews

, 214:132 | Cite as

Impact-Seismic Investigations of the InSight Mission

  • Ingrid DaubarEmail author
  • Philippe Lognonné
  • Nicholas A. Teanby
  • Katarina Miljkovic
  • Jennifer Stevanović
  • Jeremie Vaubaillon
  • Balthasar Kenda
  • Taichi Kawamura
  • John Clinton
  • Antoine Lucas
  • Melanie Drilleau
  • Charles Yana
  • Gareth S. Collins
  • Don Banfield
  • Matthew Golombek
  • Sharon Kedar
  • Nicholas Schmerr
  • Raphael Garcia
  • Sebastien Rodriguez
  • Tamara Gudkova
  • Stephane May
  • Maria Banks
  • Justin Maki
  • Eleanor Sansom
  • Foivos Karakostas
  • Mark Panning
  • Nobuaki Fuji
  • James Wookey
  • Martin van Driel
  • Mark Lemmon
  • Veronique Ansan
  • Maren Böse
  • Simon Stähler
  • Hiroo Kanamori
  • James Richardson
  • Suzanne Smrekar
  • W. Bruce Banerdt
Article
First Online:
Part of the following topical collections:
  1. The InSight Mission to Mars II

Abstract

Impact investigations will be an important aspect of the InSight mission. One of the scientific goals of the mission is a measurement of the current impact rate at Mars. Impacts will additionally inform the major goal of investigating the interior structure of Mars.

In this paper, we review the current state of knowledge about seismic signals from impacts on the Earth, Moon, and laboratory experiments. We describe the generalized physical models that can be used to explain these signals. A discussion of the appropriate source time function for impacts is presented, along with spectral characteristics including the cutoff frequency and its dependence on impact momentum. Estimates of the seismic efficiency (ratio between seismic and impact energies) vary widely. Our preferred value for the seismic efficiency at Mars is \(5 \times 10^{- 4}\), which we recommend using until we can measure it during the InSight mission, when seismic moments are not used directly. Effects of the material properties at the impact point and at the seismometer location are considered. We also discuss the processes by which airbursts and acoustic waves emanate from bolides, and the feasibility of detecting such signals.

We then consider the case of impacts on Mars. A review is given of the current knowledge of present-day cratering on Mars: the current impact rate, characteristics of those impactors such as velocity and directions, and the morphologies of the craters those impactors create. Several methods of scaling crater size to impact energy are presented. The Martian atmosphere, although thin, will cause fragmentation of impactors, with implications for the resulting seismic signals.

We also benchmark several different seismic modeling codes to be used in analysis of impact detections, and those codes are used to explore the seismic amplitude of impact-induced signals as a function of distance from the impact site. We predict a measurement of the current impact flux will be possible within the timeframe of the prime mission (one Mars year) with the detection of ∼ a few to several tens of impacts. However, the error bars on these predictions are large.

Specific to the InSight mission, we list discriminators of seismic signals from impacts that will be used to distinguish them from marsquakes. We describe the role of the InSight Impacts Science Theme Group during mission operations, including a plan for possible night-time meteor imaging. The impacts detected by these methods during the InSight mission will be used to improve interior structure models, measure the seismic efficiency, and calculate the size frequency distribution of current impacts.

Keywords

InSight Mars Impact cratering Seismology 
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Notes

Acknowledgements

We are grateful to Jay Melosh and an unnamed reviewer for thoughtful and helpful comments. We appreciate the hard work of the engineering and operations teams who are making the InSight mission possible. Elizabeth Barrett provided valuable input. Thank you to Matthew Siegler for helping to address a reviewer comment. A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. French co-authors thank the support of the French Space Agency CNES as well as ANR SIMARS. IPGP coauthors (IPGP contribution number 3988) also received support from the UnivEarth Labex at Sorbonne Paris Cité (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). N. Teanby and J. Wookey are funded by the UK Space Agency. Swiss co-authors recognize the support of the (1) Swiss National Science Foundation and French Agence Nationale de la Recherche (SNF-ANR project 157133 “Seismology on Mars”) and (2) Swiss State Secretariat for Education, Research and Innovation (SEFRI project “MarsQuake Service—Preparatory Phase”). We gratefully acknowledge the developers of the iSALE hydrocode. A portion of this work was performed using HPC resources of CINES (Centre Informatique National de l’Enseignement Supérieur) under the allocation A0030407341 made by GENCI (Grand Equipement National de Calcul Intensif). KM research is fully supported by the Australian Government (project numbers DE180100584 and DP180100661). This is InSight Contribution Number 47.

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Copyright information

© Springer Nature B.V. 2018

Authors and Affiliations

  • Ingrid Daubar
    • 1
    Email author
  • Philippe Lognonné
    • 2
  • Nicholas A. Teanby
    • 3
  • Katarina Miljkovic
    • 4
  • Jennifer Stevanović
    • 3
    • 5
  • Jeremie Vaubaillon
    • 6
  • Balthasar Kenda
    • 2
  • Taichi Kawamura
    • 2
    • 7
  • John Clinton
    • 8
  • Antoine Lucas
    • 2
  • Melanie Drilleau
    • 2
  • Charles Yana
    • 9
  • Gareth S. Collins
    • 10
  • Don Banfield
    • 11
  • Matthew Golombek
    • 1
  • Sharon Kedar
    • 1
  • Nicholas Schmerr
    • 12
  • Raphael Garcia
    • 13
  • Sebastien Rodriguez
    • 2
  • Tamara Gudkova
    • 14
  • Stephane May
    • 9
  • Maria Banks
    • 15
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  • Martin van Driel
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  • Veronique Ansan
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  • Maren Böse
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  1. 1.Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaUSA
  2. 2.Institut de Physique du Globe de Paris-Sorbone Paris CitéUniversité Paris Sorbonne, DiderotParisFrance
  3. 3.School of Earth SciencesUniversity of BristolBristolUK
  4. 4.School of Earth and Planetary ScienceCurtin UniversityPerthAustralia
  5. 5.Atomic Weapons EstablishmentAldermastonUK
  6. 6.IMCCEParisFrance
  7. 7.National Astronomical Observatory of JapanTokyoJapan
  8. 8.ETH ZurichZurichSwitzerland
  9. 9.Centre National d’Etudes SpatialesParisFrance
  10. 10.Dept. Earth Science & EngineeringImperial CollegeLondonUK
  11. 11.420 Space Sciences, Cornell Center for Astrophysics and Planetary ScienceCornell UniversityIthacaUSA
  12. 12.Department of GeologyUniversity of MarylandCollege ParkUSA
  13. 13.ISAE-SUPAEROToulouse UniversityToulouseFrance
  14. 14.Schmidt Institute of Physics of the Earth RASMoscowRussia
  15. 15.NASA Goddard Space Flight CenterGreenbeltUSA
  16. 16.Texas A&M Univ.College StationUSA
  17. 17.LPG Nantes, UMR6112CNRS-Université de NantesNantes cédex 3France
  18. 18.California Institute of TechnologyPasadenaUSA
  19. 19.Planetary Science InstituteTucsonUSA

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