Seismic detection of the martian core

Stähler, Simon C.; Khan, Amir; Banerdt, B.; Lognonné, Philippe; Giardini, Domenico; Ceylan, Savas; Drilleau, M.; Durán, Cecilia; Garcia, Raphaël; Huang, Q.; Kim, Doyeon; Lekić, V.; Samuel, Henri; Schimmel, Martín; Schmerr, Nicholas; Sollberger, David; Stutzmann, E.; Xu, Zongbo; Antonangeli, Daniele; Charalambous, Constantinos; Davis, Paul M.; Irving, J. C. E.; Kawamura, Taïchi; Knapmeyer, Martin; Maguire, Ross; Marusiak, Angela G.; Panning, M. P.; Perrin, C.; Plesa, Ana‐Catalina; Rivoldini, Attilio; Schmelzbach, Cédric; Zenhäusern, Géraldine; Beucler, É.; Clinton, John; Dahmen, Nikolaj; Driel, Martin van; Гудкова, Т. В.; Horleston, Anna; Pike, W. T.; Plasman, Matthieu; Smrekar, S. E.

doi:10.1126/science.abi7730

Cited by 196 publications

(269 citation statements)

References 121 publications

Supporting

Mentioning

248

Contrasting

Order By: Relevance

“…The amount of light elements in the core, particularly important for a better understanding of Venus's magnetic field evolution and also informative about Venus's conditions during core formation, is not known. The two parameters together, k 2 and MOIF, help to better distinguish the models as has already been shown, for example, for Mars (Rivoldini et al 2011; and recently confirmed with InSight seismic data by Stähler et al 2021), and thus better than in the models of Dumoulin et al (2017), for which MOIFs were assumed to be unknown. The information about the density distribution from the MOIF is not unique, i.e., for the same MOIF the core can be small and dense or relatively larger and lighter.…”

Section: Resultssupporting

confidence: 62%

The Determination of the Rotational State and Interior Structure of Venus with VERITAS

Cascioli

Hensley

Marchi

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

Understanding the processes that led Venus to its current state and will drive its future evolution is a major objective of the next generation of orbiters. In this work we analyze the retrieval of the spin vector, the tidal response, and the moment of inertia of Venus with VERITAS, a NASA Discovery-class mission. By simulating a systematic joint analysis of Doppler tracking data and tie points provided by the onboard synthetic aperture radar, we show that VERITAS will provide accuracies (3σ) in the estimates of the tidal Love number k 2 to 4.6 × 10 −4 , its tidal phase lag to 0°. 05, and the moment of inertia factor to 9.8 × 10 −4 (0.3% of the expected value). Applying these results to recent models of the Venus interior, we show that VERITAS will provide much-improved constraints on the interior structure of the planet.

show abstract

Section: Resultssupporting

confidence: 62%

The Determination of the Rotational State and Interior Structure of Venus with VERITAS

Cascioli

Hensley

Marchi

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…Assuming an active context of dike and fracture propagation along Cerberus Fossae, we can expect that most of the seismicity will be located at shallow depth, since on Earth it occurs mostly between the upper dike top and the surface (Ágústsdóttir et al, 2016;Passarelli et al, 2015;Rubin & Gillard, 1998;Ukawa & Tsukahara, 1996). However, the estimated first results from the InSight mission suggest hypocentral depths of 20-30 km for the main events (e.g., Brinkman et al, 2021;Stähler et al, 2021). On the other hand, the lateral propagation of the system toward the east implies that the seismicity could be also located at depth near the propagating dike tips (Green et al, 2015;Rubin & Gillard, 1998;Sigmundsson et al, 2015).…”

Section: Regional and Local Stress Concentrations: Constraints On Marsquake Locations Recorded By The Insight Missionmentioning

confidence: 99%

Geometry and Segmentation of Cerberus Fossae, Mars: Implications for Marsquake Properties

et al. 2022

Self Cite

View full text Add to dashboard Cite

show abstract

“…Seismic recordings collected on the Moon and Mars by the Apollo and InSight mission (e.g., Banerdt et al, 2020;Lognonné et al, 2019Lognonné et al, , 2020Nunn et al, 2020) have provided direct information on the interior structure of both planetary bodies from crust (e.g., Kovach and Watkins, 1973;Toksöz et al, 1974) to core (Garcia et al, 2011;Stähler et al, 2021;Weber et al, 2011). RF analysis of these data has led to important insights.…”

Section: Introductionmentioning

confidence: 99%

Improving Constraints on Planetary Interiors With PPs Receiver Functions

et al. 2021

Self Cite

View full text Add to dashboard Cite

Seismological constraints obtained from receiver function (RF) analysis provide important information about the crust and mantle structure. Here, we explore the utility of the free‐surface multiple of the P‐wave (PP) and the corresponding conversions in RF analysis. Using earthquake records, we demonstrate the efficacy of PPs‐RFs before illustrating how they become especially useful when limited data is available in typical planetary missions. Using a transdimensional hierarchical Bayesian deconvolution approach, we compute robust P‐to‐S (Ps)‐ and PPs‐RFs with InSight recordings of five marsquakes. Our Ps‐RF results verify the direct Ps converted phases reported by previous RF analyses with increased coherence and reveal other phases including the primary multiple reverberating within the uppermost layer of the Martian crust. Unlike the Ps‐RFs, our PPs‐RFs lack an arrival at 7.2 s lag time. Whereas Ps‐RFs on Mars could be equally well fit by a two‐ or three‐layer crust, synthetic modeling shows that the disappearance of the 7.2 s phase requires a three‐layer crust, and is highly sensitive to velocity and thickness of intra‐crustal layers. We show that a three‐layer crust is also preferred by S‐to‐P (Sp)‐RFs. While the deepest interface of the three‐layer crust represents the crust‐mantle interface beneath the InSight landing site, the other two interfaces at shallower depths could represent a sharp transition between either fractured and unfractured materials or thick basaltic flows and pre‐existing crustal materials. PPs‐RFs can provide complementary constraints and maximize the extraction of information about crustal structure in data‐constrained circumstances such as planetary missions.

show abstract

Seismic detection of the martian core

Cited by 196 publications

References 121 publications

The Determination of the Rotational State and Interior Structure of Venus with VERITAS

The Determination of the Rotational State and Interior Structure of Venus with VERITAS

Geometry and Segmentation of Cerberus Fossae, Mars: Implications for Marsquake Properties

Improving Constraints on Planetary Interiors With PPs Receiver Functions

Contact Info

Product

Resources

About