The Global Seismic Moment Rate of Mars after Event S1222a

Martin Knapmeyer; Simon C. Stähler; Ana Catalina Plesa; Savas Ceylan; Constantinos Charalambous; John Clinton; Nikolaj  Dahmen; Anna C Horleston; al et

doi:10.1029/2022GL102296

The Global Seismic Moment Rate of Mars after Event S1222a

Martin Knapmeyer, Simon C. Stähler, Ana Catalina Plesa, Savas Ceylan, Constantinos Charalambous, John Clinton, Nikolaj Dahmen, Anna C Horleston, al et

Research output: Contribution to journal › Article (Academic Journal) › peer-review

7 Citations (Scopus)

Abstract

The seismic activity of a planet can be described by the corner magnitude, events larger than which are extremely unlikely, and the seismic moment rate, the long-term average of annual seismic moment release. Marsquake S1222a proves large enough to be representative of the global activity of Mars and places observational constraints on the moment rate. The magnitude-frequency distribution of relevant Marsquakes indicates a b-value of 1.17, but with its uncertainty and a volcanic region bias, b=1 is still possible. The moment rate is likely between 1.5e15 Nm/a and 1.6e18 Nm/a, with a marginal distribution peaking at 4.9e16 Nm/a. Comparing this with pre-InSight estimations shows that these tended to overestimate the moment rate, and that 30 % or more of the tectonic deformation may occur silently, whereas the seismicity is probably restricted to localized centers rather than spread over the entire planet.

Original language	English
Article number	e2022GL102296
Number of pages	9
Journal	Geophysical Research Letters
Volume	50
Issue number	7
DOIs	https://doi.org/10.1029/2022GL102296
Publication status	Published - 6 Apr 2023

Bibliographical note

Funding Information:
The authors gratefully acknowledge the advice of Maren Böse, ETH Zürich, concerning the treatment of magnitude uncertainties. The authors are also grateful to an anonymous reviewer whose questions and suggestions helped to improve our manuscript. The authors acknowledge NASA, CNES, partner agencies and Institutions (UKSA, SSO, DLR, JPL, IPGP‐CNRS, ETHZ, IC, MPS‐MPG) and the operators of JPL, SISMOC, MSDS, IRIS‐DMC and PDS for providing SEED SEIS data. N.D., C.D., and G.Z. would like to acknowledge support from ETH through the ETH+ funding scheme (ETH+02 19‐1: “Planet Mars”). M.P.P. and W.B.B were supported by the NASA InSight mission and funds from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). A.H. is funded by the UKSA under Grants ST/R002096/1 and ST/W002523/1. A.‐C.P. gratefully acknowledges the financial support and endorsement from the DLR Management Board Young Research Group Leader Program and the Executive Board Member for Space Research and Technology. This is InSight Contribution ICN 273. Open Access funding enabled and organized by Projekt DEAL.

Funding Information:
The authors gratefully acknowledge the advice of Maren Böse, ETH Zürich, concerning the treatment of magnitude uncertainties. The authors are also grateful to an anonymous reviewer whose questions and suggestions helped to improve our manuscript. The authors acknowledge NASA, CNES, partner agencies and Institutions (UKSA, SSO, DLR, JPL, IPGP-CNRS, ETHZ, IC, MPS-MPG) and the operators of JPL, SISMOC, MSDS, IRIS-DMC and PDS for providing SEED SEIS data. N.D., C.D., and G.Z. would like to acknowledge support from ETH through the ETH+ funding scheme (ETH+02 19-1: “Planet Mars”). M.P.P. and W.B.B were supported by the NASA InSight mission and funds from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). A.H. is funded by the UKSA under Grants ST/R002096/1 and ST/W002523/1. A.-C.P. gratefully acknowledges the financial support and endorsement from the DLR Management Board Young Research Group Leader Program and the Executive Board Member for Space Research and Technology. This is InSight Contribution ICN 273. Open Access funding enabled and organized by Projekt DEAL.

Publisher Copyright:
© 2023. The Authors.

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Exploring the Seismicity of Mars with InSight (YR2+YR3)
Teanby, N. A. (Principal Investigator)
1/04/22 → 31/03/24
Project: Research
Exploring the Seismicity of Mars with InSight (YR2+YR3)
Teanby, N. A. (Principal Investigator)
1/04/21 → 31/03/22
Project: Research, Parent
Exploring the Seismicity of Mars with InSight (YR1)
Teanby, N. A. (Principal Investigator)
1/04/21 → 31/03/23
Project: Research

Cite this

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title = "The Global Seismic Moment Rate of Mars after Event S1222a",

abstract = "The seismic activity of a planet can be described by the corner magnitude, events larger than which are extremely unlikely, and the seismic moment rate, the long-term average of annual seismic moment release. Marsquake S1222a proves large enough to be representative of the global activity of Mars and places observational constraints on the moment rate. The magnitude-frequency distribution of relevant Marsquakes indicates a b-value of 1.17, but with its uncertainty and a volcanic region bias, b=1 is still possible. The moment rate is likely between 1.5e15 Nm/a and 1.6e18 Nm/a, with a marginal distribution peaking at 4.9e16 Nm/a. Comparing this with pre-InSight estimations shows that these tended to overestimate the moment rate, and that 30 % or more of the tectonic deformation may occur silently, whereas the seismicity is probably restricted to localized centers rather than spread over the entire planet.",

author = "Martin Knapmeyer and St{\"a}hler, {Simon C.} and Plesa, {Ana Catalina} and Savas Ceylan and Constantinos Charalambous and John Clinton and Nikolaj Dahmen and Horleston, {Anna C} and al et",

note = "Funding Information: The authors gratefully acknowledge the advice of Maren B{\"o}se, ETH Z{\"u}rich, concerning the treatment of magnitude uncertainties. The authors are also grateful to an anonymous reviewer whose questions and suggestions helped to improve our manuscript. The authors acknowledge NASA, CNES, partner agencies and Institutions (UKSA, SSO, DLR, JPL, IPGP‐CNRS, ETHZ, IC, MPS‐MPG) and the operators of JPL, SISMOC, MSDS, IRIS‐DMC and PDS for providing SEED SEIS data. N.D., C.D., and G.Z. would like to acknowledge support from ETH through the ETH+ funding scheme (ETH+02 19‐1: “Planet Mars”). M.P.P. and W.B.B were supported by the NASA InSight mission and funds from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). A.H. is funded by the UKSA under Grants ST/R002096/1 and ST/W002523/1. A.‐C.P. gratefully acknowledges the financial support and endorsement from the DLR Management Board Young Research Group Leader Program and the Executive Board Member for Space Research and Technology. This is InSight Contribution ICN 273. Open Access funding enabled and organized by Projekt DEAL. Funding Information: The authors gratefully acknowledge the advice of Maren B{\"o}se, ETH Z{\"u}rich, concerning the treatment of magnitude uncertainties. The authors are also grateful to an anonymous reviewer whose questions and suggestions helped to improve our manuscript. The authors acknowledge NASA, CNES, partner agencies and Institutions (UKSA, SSO, DLR, JPL, IPGP-CNRS, ETHZ, IC, MPS-MPG) and the operators of JPL, SISMOC, MSDS, IRIS-DMC and PDS for providing SEED SEIS data. N.D., C.D., and G.Z. would like to acknowledge support from ETH through the ETH+ funding scheme (ETH+02 19-1: “Planet Mars”). M.P.P. and W.B.B were supported by the NASA InSight mission and funds from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). A.H. is funded by the UKSA under Grants ST/R002096/1 and ST/W002523/1. A.-C.P. gratefully acknowledges the financial support and endorsement from the DLR Management Board Young Research Group Leader Program and the Executive Board Member for Space Research and Technology. This is InSight Contribution ICN 273. Open Access funding enabled and organized by Projekt DEAL. Publisher Copyright: {\textcopyright} 2023. The Authors.",

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AU - Knapmeyer, Martin

AU - Stähler, Simon C.

AU - Plesa, Ana Catalina

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AU - Charalambous, Constantinos

AU - Clinton, John

AU - Dahmen, Nikolaj

AU - Horleston, Anna C

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N1 - Funding Information: The authors gratefully acknowledge the advice of Maren Böse, ETH Zürich, concerning the treatment of magnitude uncertainties. The authors are also grateful to an anonymous reviewer whose questions and suggestions helped to improve our manuscript. The authors acknowledge NASA, CNES, partner agencies and Institutions (UKSA, SSO, DLR, JPL, IPGP‐CNRS, ETHZ, IC, MPS‐MPG) and the operators of JPL, SISMOC, MSDS, IRIS‐DMC and PDS for providing SEED SEIS data. N.D., C.D., and G.Z. would like to acknowledge support from ETH through the ETH+ funding scheme (ETH+02 19‐1: “Planet Mars”). M.P.P. and W.B.B were supported by the NASA InSight mission and funds from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). A.H. is funded by the UKSA under Grants ST/R002096/1 and ST/W002523/1. A.‐C.P. gratefully acknowledges the financial support and endorsement from the DLR Management Board Young Research Group Leader Program and the Executive Board Member for Space Research and Technology. This is InSight Contribution ICN 273. Open Access funding enabled and organized by Projekt DEAL. Funding Information: The authors gratefully acknowledge the advice of Maren Böse, ETH Zürich, concerning the treatment of magnitude uncertainties. The authors are also grateful to an anonymous reviewer whose questions and suggestions helped to improve our manuscript. The authors acknowledge NASA, CNES, partner agencies and Institutions (UKSA, SSO, DLR, JPL, IPGP-CNRS, ETHZ, IC, MPS-MPG) and the operators of JPL, SISMOC, MSDS, IRIS-DMC and PDS for providing SEED SEIS data. N.D., C.D., and G.Z. would like to acknowledge support from ETH through the ETH+ funding scheme (ETH+02 19-1: “Planet Mars”). M.P.P. and W.B.B were supported by the NASA InSight mission and funds from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). A.H. is funded by the UKSA under Grants ST/R002096/1 and ST/W002523/1. A.-C.P. gratefully acknowledges the financial support and endorsement from the DLR Management Board Young Research Group Leader Program and the Executive Board Member for Space Research and Technology. This is InSight Contribution ICN 273. Open Access funding enabled and organized by Projekt DEAL. Publisher Copyright: © 2023. The Authors.

PY - 2023/4/6

Y1 - 2023/4/6

N2 - The seismic activity of a planet can be described by the corner magnitude, events larger than which are extremely unlikely, and the seismic moment rate, the long-term average of annual seismic moment release. Marsquake S1222a proves large enough to be representative of the global activity of Mars and places observational constraints on the moment rate. The magnitude-frequency distribution of relevant Marsquakes indicates a b-value of 1.17, but with its uncertainty and a volcanic region bias, b=1 is still possible. The moment rate is likely between 1.5e15 Nm/a and 1.6e18 Nm/a, with a marginal distribution peaking at 4.9e16 Nm/a. Comparing this with pre-InSight estimations shows that these tended to overestimate the moment rate, and that 30 % or more of the tectonic deformation may occur silently, whereas the seismicity is probably restricted to localized centers rather than spread over the entire planet.

AB - The seismic activity of a planet can be described by the corner magnitude, events larger than which are extremely unlikely, and the seismic moment rate, the long-term average of annual seismic moment release. Marsquake S1222a proves large enough to be representative of the global activity of Mars and places observational constraints on the moment rate. The magnitude-frequency distribution of relevant Marsquakes indicates a b-value of 1.17, but with its uncertainty and a volcanic region bias, b=1 is still possible. The moment rate is likely between 1.5e15 Nm/a and 1.6e18 Nm/a, with a marginal distribution peaking at 4.9e16 Nm/a. Comparing this with pre-InSight estimations shows that these tended to overestimate the moment rate, and that 30 % or more of the tectonic deformation may occur silently, whereas the seismicity is probably restricted to localized centers rather than spread over the entire planet.

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DO - 10.1029/2022GL102296

M3 - Article (Academic Journal)

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VL - 50

JO - Geophysical Research Letters

JF - Geophysical Research Letters

IS - 7

M1 - e2022GL102296

ER -

The Global Seismic Moment Rate of Mars after Event S1222a

Abstract

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Exploring the Seismicity of Mars with InSight (YR2+YR3)

Exploring the Seismicity of Mars with InSight (YR2+YR3)

Exploring the Seismicity of Mars with InSight (YR1)

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