TY - JOUR
T1 - Planned Products of the Mars Structure Service for the InSight Mission to Mars
AU - Panning, Mark P.
AU - Lognonné, Philippe
AU - Bruce Banerdt, W.
AU - Garcia, Raphaël
AU - Golombek, Matthew
AU - Kedar, Sharon
AU - Knapmeyer-Endrun, Brigitte
AU - Mocquet, Antoine
AU - Teanby, Nick A.
AU - Tromp, Jeroen
AU - Weber, Renee
AU - Beucler, Eric
AU - Blanchette-Guertin, Jean Francois
AU - Bozdağ, Ebru
AU - Drilleau, Mélanie
AU - Gudkova, Tamara
AU - Hempel, Stefanie
AU - Khan, Amir
AU - Lekić, Vedran
AU - Murdoch, Naomi
AU - Plesa, Ana Catalina
AU - Rivoldini, Atillio
AU - Schmerr, Nicholas
AU - Ruan, Youyi
AU - Verhoeven, Olivier
AU - Gao, Chao
AU - Christensen, Ulrich
AU - Clinton, John
AU - Dehant, Veronique
AU - Giardini, Domenico
AU - Mimoun, David
AU - Thomas Pike, W.
AU - Smrekar, Sue
AU - Wieczorek, Mark
AU - Knapmeyer, Martin
AU - Wookey, James
N1 - Funding Information:
Acknowledgements Research described in this paper was partially done by the InSight Project, Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work has been supported by CNES for all French institutions’ co-authors. S.H., J.B.G. and the IPGP, ISAE and Univ. Nantes teams have been also supported by ANR (ANR-14-CE36-0012 “Seismology on Mars”) and PL by Institut Universitaire de France. The Bayesian inversions of Sect. 3 were performed using HPC resources of CINES (Centre Informatique National de l’Enseignement Superieur) under the allocation 2015047341 made by GENCI (Grand Equipement National de Calcul Intensif). A.K. was supported by grants from the Swiss National Science Foundation (SNF-ANR project 157133 “Seismology on Mars”) and from the Swiss National Supercomputing Centre (CSCS) under project ID s628. N.T. and J.W. were supported by funding from the U.K. Space Agency. The open source spectral-element software packages SPECFEM3D GLOBE and AxiSEM are freely available via the Computational Infrastructure for Geodynamics (CIG; geodynamics.org). For SPECFEM3D GLOBE simulations computational resources were provided by the Princeton Institute for Computational Science & Engineering (PICSciE). This paper is InSight Contribution Number 22.
Funding Information:
Research described in this paper was partially done by the InSight Project, Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work has been supported by CNES for all French institutions? co-authors. S.H., J.B.G. and the IPGP, ISAE and Univ. Nantes teams have been also supported by ANR (ANR-14-CE36-0012 ?Seismology on Mars?) and PL by Institut Universitaire de France. The Bayesian inversions of Sect.?3 were performed using HPC resources of CINES (Centre Informatique National de l?Enseignement Superieur) under the allocation 2015047341 made by GENCI (Grand Equipement National de Calcul Intensif). A.K. was supported by grants from the Swiss National Science Foundation (SNF-ANR project 157133 ?Seismology on Mars?) and from the Swiss National Supercomputing Centre (CSCS) under project ID s628. N.T. and J.W. were supported by funding from the U.K. Space Agency. The open source spectral-element software packages SPECFEM3D GLOBE and AxiSEM are freely available via the Computational Infrastructure for Geodynamics (CIG; geodynamics.org). For SPECFEM3D GLOBE simulations computational resources were provided by the Princeton Institute for Computational Science & Engineering (PICSciE). This paper is InSight Contribution Number 22.
Publisher Copyright:
© 2016, Springer Science+Business Media Dordrecht.
PY - 2017/10/1
Y1 - 2017/10/1
N2 - The InSight lander will deliver geophysical instruments to Mars in 2018, including seismometers installed directly on the surface (Seismic Experiment for Interior Structure, SEIS). Routine operations will be split into two services, the Mars Structure Service (MSS) and Marsquake Service (MQS), which will be responsible, respectively, for defining the structure models and seismicity catalogs from the mission. The MSS will deliver a series of products before the landing, during the operations, and finally to the Planetary Data System (PDS) archive. Prior to the mission, we assembled a suite of a priori models of Mars, based on estimates of bulk composition and thermal profiles. Initial models during the mission will rely on modeling surface waves and impact-generated body waves independent of prior knowledge of structure. Later modeling will include simultaneous inversion of seismic observations for source and structural parameters. We use Bayesian inversion techniques to obtain robust probability distribution functions of interior structure parameters. Shallow structure will be characterized using the hammering of the heatflow probe mole, as well as measurements of surface wave ellipticity. Crustal scale structure will be constrained by measurements of receiver function and broadband Rayleigh wave ellipticity measurements. Core interacting body wave phases should be observable above modeled martian noise levels, allowing us to constrain deep structure. Normal modes of Mars should also be observable and can be used to estimate the globally averaged 1D structure, while combination with results from the InSight radio science mission and orbital observations will allow for constraint of deeper structure.
AB - The InSight lander will deliver geophysical instruments to Mars in 2018, including seismometers installed directly on the surface (Seismic Experiment for Interior Structure, SEIS). Routine operations will be split into two services, the Mars Structure Service (MSS) and Marsquake Service (MQS), which will be responsible, respectively, for defining the structure models and seismicity catalogs from the mission. The MSS will deliver a series of products before the landing, during the operations, and finally to the Planetary Data System (PDS) archive. Prior to the mission, we assembled a suite of a priori models of Mars, based on estimates of bulk composition and thermal profiles. Initial models during the mission will rely on modeling surface waves and impact-generated body waves independent of prior knowledge of structure. Later modeling will include simultaneous inversion of seismic observations for source and structural parameters. We use Bayesian inversion techniques to obtain robust probability distribution functions of interior structure parameters. Shallow structure will be characterized using the hammering of the heatflow probe mole, as well as measurements of surface wave ellipticity. Crustal scale structure will be constrained by measurements of receiver function and broadband Rayleigh wave ellipticity measurements. Core interacting body wave phases should be observable above modeled martian noise levels, allowing us to constrain deep structure. Normal modes of Mars should also be observable and can be used to estimate the globally averaged 1D structure, while combination with results from the InSight radio science mission and orbital observations will allow for constraint of deeper structure.
KW - InSight mission
KW - Interior structure
KW - Mars
KW - Seismology
UR - http://www.scopus.com/inward/record.url?scp=85000420237&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85000420237&partnerID=8YFLogxK
U2 - 10.1007/s11214-016-0317-5
DO - 10.1007/s11214-016-0317-5
M3 - Review article
AN - SCOPUS:85000420237
SN - 0038-6308
VL - 211
SP - 611
EP - 650
JO - Space Science Reviews
JF - Space Science Reviews
IS - 1-4
ER -