Surface waves and crustal structure on Mars

D. Kim; W. B. Banerdt; S. Ceylan; D. Giardini; V. Lekić; P. Lognonné; C. Beghein; Beucler; S. Carrasco; C. Charalambous; J. Clinton; M. Drilleau; C. Durán; M. Golombek; R. Joshi; A. Khan; B. Knapmeyer-Endrun; J. Li; R. Maguire; W. T. Pike; H. Samuel; M. Schimmel; N. C. Schmerr; S. C. Stähler; E. Stutzmann; M. Wieczorek; Z. Xu; A. Batov; E. Bozdag; N. Dahmen; P. Davis; T. Gudkova; A. Horleston; Q. Huang; T. Kawamura; S. D. King; S. M. McLennan; F. Nimmo; M. Plasman; A. C. Plesa; I. E. Stepanova; E. Weidner; G. Zenhäusern; I. J. Daubar; B. Fernando; R. F. Garcia; L. V. Posiolova; M. P. Panning

doi:10.1126/science.abq7157

Surface waves and crustal structure on Mars

D. Kim, W. B. Banerdt, S. Ceylan, D. Giardini, V. Lekić, P. Lognonné, C. Beghein, Beucler, S. Carrasco, C. Charalambous, J. Clinton, M. Drilleau, C. Durán, M. Golombek, R. Joshi, A. Khan, B. Knapmeyer-Endrun, J. Li, R. Maguire, W. T. PikeH. Samuel, M. Schimmel, N. C. Schmerr, S. C. Stähler, E. Stutzmann, M. Wieczorek, Z. Xu, A. Batov, E. Bozdag, N. Dahmen, P. Davis, T. Gudkova, A. Horleston, Q. Huang, T. Kawamura, S. D. King, S. M. McLennan, F. Nimmo, M. Plasman, A. C. Plesa, I. E. Stepanova, E. Weidner, G. Zenhäusern, I. J. Daubar, B. Fernando, R. F. Garcia, L. V. Posiolova, M. P. Panning

Earth Science and Environmental Change

Research output: Contribution to journal › Article › peer-review

Abstract

We detected surface waves from two meteorite impacts on Mars. By measuring group velocity dispersion along the impact-lander path, we obtained a direct constraint on crustal structure away from the InSight lander. The crust north of the equatorial dichotomy had a shear wave velocity of approximately 3.2 kilometers per second in the 5- to 30-kilometer depth range, with little depth variation. This implies a higher crustal density than inferred beneath the lander, suggesting either compositional differences or reduced porosity in the volcanic areas traversed by the surface waves. The lower velocities and the crustal layering observed beneath the landing site down to a 10-kilometer depth are not a global feature. Structural variations revealed by surface waves hold implications for models of the formation and thickness of the martian crust.

Original language	English (US)
Pages (from-to)	417-421
Number of pages	5
Journal	Science
Volume	378
Issue number	6618
DOIs	https://doi.org/10.1126/science.abq7157
State	Published - Oct 28 2022

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Kim, D., Banerdt, W. B., Ceylan, S., Giardini, D., Lekić, V., Lognonné, P., Beghein, C., Beucler, Carrasco, S., Charalambous, C., Clinton, J., Drilleau, M., Durán, C., Golombek, M., Joshi, R., Khan, A., Knapmeyer-Endrun, B., Li, J., Maguire, R., ... Panning, M. P. (2022). Surface waves and crustal structure on Mars. Science, 378(6618), 417-421. https://doi.org/10.1126/science.abq7157

Kim, D, Banerdt, WB, Ceylan, S, Giardini, D, Lekić, V, Lognonné, P, Beghein, C, Beucler, Carrasco, S, Charalambous, C, Clinton, J, Drilleau, M, Durán, C, Golombek, M, Joshi, R, Khan, A, Knapmeyer-Endrun, B, Li, J, Maguire, R, Pike, WT, Samuel, H, Schimmel, M, Schmerr, NC, Stähler, SC, Stutzmann, E, Wieczorek, M, Xu, Z, Batov, A, Bozdag, E, Dahmen, N, Davis, P, Gudkova, T, Horleston, A, Huang, Q, Kawamura, T, King, SD, McLennan, SM, Nimmo, F, Plasman, M, Plesa, AC, Stepanova, IE, Weidner, E, Zenhäusern, G, Daubar, IJ, Fernando, B, Garcia, RF, Posiolova, LV & Panning, MP 2022, 'Surface waves and crustal structure on Mars', Science, vol. 378, no. 6618, pp. 417-421. https://doi.org/10.1126/science.abq7157

@article{68439e5c08424ed1957305978f41aa7e,

title = "Surface waves and crustal structure on Mars",

abstract = "We detected surface waves from two meteorite impacts on Mars. By measuring group velocity dispersion along the impact-lander path, we obtained a direct constraint on crustal structure away from the InSight lander. The crust north of the equatorial dichotomy had a shear wave velocity of approximately 3.2 kilometers per second in the 5- to 30-kilometer depth range, with little depth variation. This implies a higher crustal density than inferred beneath the lander, suggesting either compositional differences or reduced porosity in the volcanic areas traversed by the surface waves. The lower velocities and the crustal layering observed beneath the landing site down to a 10-kilometer depth are not a global feature. Structural variations revealed by surface waves hold implications for models of the formation and thickness of the martian crust.",

author = "D. Kim and Banerdt, {W. B.} and S. Ceylan and D. Giardini and V. Leki{\'c} and P. Lognonn{\'e} and C. Beghein and Beucler and S. Carrasco and C. Charalambous and J. Clinton and M. Drilleau and C. Dur{\'a}n and M. Golombek and R. Joshi and A. Khan and B. Knapmeyer-Endrun and J. Li and R. Maguire and Pike, {W. T.} and H. Samuel and M. Schimmel and Schmerr, {N. C.} and St{\"a}hler, {S. C.} and E. Stutzmann and M. Wieczorek and Z. Xu and A. Batov and E. Bozdag and N. Dahmen and P. Davis and T. Gudkova and A. Horleston and Q. Huang and T. Kawamura and King, {S. D.} and McLennan, {S. M.} and F. Nimmo and M. Plasman and Plesa, {A. C.} and Stepanova, {I. E.} and E. Weidner and G. Zenh{\"a}usern and Daubar, {I. J.} and B. Fernando and Garcia, {R. F.} and Posiolova, {L. V.} and Panning, {M. P.}",

note = "This paper is InSight contribution number 266. The authors acknowledge the National Aeronautics and Space Administration (NASA), Centre National d\u2019\u00C9tudes Spatiales (CNES), their partner agencies and institutions (UKSA, SSO, DLR, JPL, IPGP-CNRS, ETHZ, IC, and MPS-MPG), and the flight operations team at JPL, SISMOC, MSDS, IRIS-DMC, and PDS for providing the SEED SEIS data. We acknowledge the thorough and thoughtful reviews from the editor and from three anonymous reviewers that greatly improved the manuscript. D.K., S.C., D.G., J.C., C.D., A. K., S.C.S., N.D., and G.Z. were supported by the ETH+ funding scheme (ETH+02 19-1: \u201CPlanet Mars\u201D). Marsquake Service operations at ETH Z\u00FCrich were supported by ETH Research grant ETH-06 17-02. N.C.S. and V.L. were supported by NASA PSP grant no. 80NSSC18K1628. Q.H. and E.B. are funded by NASA grant 80NSSC18K1680. C.B. and J.L. were supported by NASA InSight PSP grant no. 80NSSC18K1679. S.D.K. was supported by NASA InSight PSP grant no. 80NSSC18K1623. P.L., E.B., M.D., H.S., E.S., M.W., Z.X., T.W., M.P., R.F.G. were supported by CNES and the Agence Nationale de la Recherche (ANR-19-CE31-0008-08 MAGIS) for SEIS operation and SEIS Science analysis. A.H., C.C. and W.T.P. were supported by the UKSA under grant nos. ST/R002096/1, ST/ W002523/1 and ST/V00638X/1. Numerical computations of McMC Approach 2 were performed on the S-CAPAD/DANTE platform (IPGP, France) and using the HPC resources of IDRIS under the allocation A0110413017 made by GENCI. A.H. was supported by the UKSA under grant nos. ST/R002096/1 and ST/W002523/1. F.N. was supported by InSight PSP 80NSSC18K1627. I.J.D. was supported by NASA InSight PSP grant no. 80NSSC20K0971. L.V.P. was funded by NASANNN12AA01C with subcontract JPL-1515835. The research was carried out in part by W.B.B., M.G. and M.P.P. at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004).",

year = "2022",

month = oct,

day = "28",

doi = "10.1126/science.abq7157",

language = "English (US)",

volume = "378",

pages = "417--421",

journal = "Science",

issn = "0036-8075",

publisher = "American Association for the Advancement of Science",

number = "6618",

}

TY - JOUR

T1 - Surface waves and crustal structure on Mars

AU - Kim, D.

AU - Banerdt, W. B.

AU - Ceylan, S.

AU - Giardini, D.

AU - Lekić, V.

AU - Lognonné, P.

AU - Beghein, C.

AU - Beucler,

AU - Carrasco, S.

AU - Charalambous, C.

AU - Clinton, J.

AU - Drilleau, M.

AU - Durán, C.

AU - Golombek, M.

AU - Joshi, R.

AU - Khan, A.

AU - Knapmeyer-Endrun, B.

AU - Li, J.

AU - Maguire, R.

AU - Pike, W. T.

AU - Samuel, H.

AU - Schimmel, M.

AU - Schmerr, N. C.

AU - Stähler, S. C.

AU - Stutzmann, E.

AU - Wieczorek, M.

AU - Xu, Z.

AU - Batov, A.

AU - Bozdag, E.

AU - Dahmen, N.

AU - Davis, P.

AU - Gudkova, T.

AU - Horleston, A.

AU - Huang, Q.

AU - Kawamura, T.

AU - King, S. D.

AU - McLennan, S. M.

AU - Nimmo, F.

AU - Plasman, M.

AU - Plesa, A. C.

AU - Stepanova, I. E.

AU - Weidner, E.

AU - Zenhäusern, G.

AU - Daubar, I. J.

AU - Fernando, B.

AU - Garcia, R. F.

AU - Posiolova, L. V.

AU - Panning, M. P.

N1 - This paper is InSight contribution number 266. The authors acknowledge the National Aeronautics and Space Administration (NASA), Centre National d\u2019\u00C9tudes Spatiales (CNES), their partner agencies and institutions (UKSA, SSO, DLR, JPL, IPGP-CNRS, ETHZ, IC, and MPS-MPG), and the flight operations team at JPL, SISMOC, MSDS, IRIS-DMC, and PDS for providing the SEED SEIS data. We acknowledge the thorough and thoughtful reviews from the editor and from three anonymous reviewers that greatly improved the manuscript. D.K., S.C., D.G., J.C., C.D., A. K., S.C.S., N.D., and G.Z. were supported by the ETH+ funding scheme (ETH+02 19-1: \u201CPlanet Mars\u201D). Marsquake Service operations at ETH Z\u00FCrich were supported by ETH Research grant ETH-06 17-02. N.C.S. and V.L. were supported by NASA PSP grant no. 80NSSC18K1628. Q.H. and E.B. are funded by NASA grant 80NSSC18K1680. C.B. and J.L. were supported by NASA InSight PSP grant no. 80NSSC18K1679. S.D.K. was supported by NASA InSight PSP grant no. 80NSSC18K1623. P.L., E.B., M.D., H.S., E.S., M.W., Z.X., T.W., M.P., R.F.G. were supported by CNES and the Agence Nationale de la Recherche (ANR-19-CE31-0008-08 MAGIS) for SEIS operation and SEIS Science analysis. A.H., C.C. and W.T.P. were supported by the UKSA under grant nos. ST/R002096/1, ST/ W002523/1 and ST/V00638X/1. Numerical computations of McMC Approach 2 were performed on the S-CAPAD/DANTE platform (IPGP, France) and using the HPC resources of IDRIS under the allocation A0110413017 made by GENCI. A.H. was supported by the UKSA under grant nos. ST/R002096/1 and ST/W002523/1. F.N. was supported by InSight PSP 80NSSC18K1627. I.J.D. was supported by NASA InSight PSP grant no. 80NSSC20K0971. L.V.P. was funded by NASANNN12AA01C with subcontract JPL-1515835. The research was carried out in part by W.B.B., M.G. and M.P.P. at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004).

PY - 2022/10/28

Y1 - 2022/10/28

N2 - We detected surface waves from two meteorite impacts on Mars. By measuring group velocity dispersion along the impact-lander path, we obtained a direct constraint on crustal structure away from the InSight lander. The crust north of the equatorial dichotomy had a shear wave velocity of approximately 3.2 kilometers per second in the 5- to 30-kilometer depth range, with little depth variation. This implies a higher crustal density than inferred beneath the lander, suggesting either compositional differences or reduced porosity in the volcanic areas traversed by the surface waves. The lower velocities and the crustal layering observed beneath the landing site down to a 10-kilometer depth are not a global feature. Structural variations revealed by surface waves hold implications for models of the formation and thickness of the martian crust.

AB - We detected surface waves from two meteorite impacts on Mars. By measuring group velocity dispersion along the impact-lander path, we obtained a direct constraint on crustal structure away from the InSight lander. The crust north of the equatorial dichotomy had a shear wave velocity of approximately 3.2 kilometers per second in the 5- to 30-kilometer depth range, with little depth variation. This implies a higher crustal density than inferred beneath the lander, suggesting either compositional differences or reduced porosity in the volcanic areas traversed by the surface waves. The lower velocities and the crustal layering observed beneath the landing site down to a 10-kilometer depth are not a global feature. Structural variations revealed by surface waves hold implications for models of the formation and thickness of the martian crust.

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U2 - 10.1126/science.abq7157

DO - 10.1126/science.abq7157

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C2 - 36302020

AN - SCOPUS:85140860327

SN - 0036-8075

VL - 378

SP - 417

EP - 421

JO - Science

JF - Science

IS - 6618

ER -

Surface waves and crustal structure on Mars

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