Numerical Simulation of Lunar Seismic Wave Propagation: Investigation of Subsurface Scattering Properties Near Apollo 12 Landing Site

Onodera, Keisuke; Kawamura, Taïchi; Tanaka, Satoshi; Ishihara, Yoshiaki; Maeda, Takuto

doi:10.1029/2020je006406

Cited by 18 publications

(36 citation statements)

References 48 publications

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“…Surface waves are expected to have an increase in the excitation coefficients between 0.1 and 0.15 Hz for sources above 50 m altitude. The increase is not observed in the estimated S1094b spectra and may be due to attenuation and scattering, which is not unexpected given that scattering effects are predicted to generate increasing attenuation of surface waves with frequency on the Moon and Mars (40). Comparison of S1094b surface wave spectra with near-surface excitation coefficients (fig.…”

mentioning

confidence: 72%

Largest recent impact craters on Mars: Orbital imaging and surface seismic co-investigation

Posiolova

Lognonné

Banerdt

et al. 2022

Science

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Two >130-meter-diameter impact craters formed on Mars during the later half of 2021. These are the two largest fresh impact craters discovered by the Mars Reconnaissance Orbiter since operations started 16 years ago. The impacts created two of the largest seismic events (magnitudes greater than 4) recorded by InSight during its 3-year mission. The combination of orbital imagery and seismic ground motion enables the investigation of subsurface and atmospheric energy partitioning of the impact process on a planet with a thin atmosphere and the first direct test of martian deep-interior seismic models with known event distances. The impact at 35°N excavated blocks of water ice, which is the lowest latitude at which ice has been directly observed on Mars.

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mentioning

confidence: 72%

Largest recent impact craters on Mars: Orbital imaging and surface seismic co-investigation

Posiolova

Lognonné

Banerdt

et al. 2022

Science

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“…Compared with the Gaussian media, the Von Kármán media (including the exponential type) show more short-wavelength structures. Due to the intense sputtering and stacking process, the heterogeneity of the lunar regolith should be more consistent with the Von Kármán (including the exponential type) media [35,36,52]. However, we cannot well distinguish its difference from the exponential ACF due to the limited radar wave resolution, even though the zero-order Von Kármán model has greater heterogeneity at small scales.…”

Section: Self-organization Modelmentioning

confidence: 86%

“…Lv et al [16] constructed four typical models and performed numerical simulations using the time-domain finite-difference method, which can better present the wave propagation in the lunar regolith with strong heterogeneity. Some works noted the existence of weak heterogeneity of the lunar regolith [11,[33][34][35]. However, to date, no numerical simulation has been conducted specifically on the weak heterogeneity of the lunar regolith, probably due to three aspects: 1. lack of methods describing heterogeneous media; 2. technical difficulty in constructing random models; 3. excessive computational cost of numerical simulations [16] compared with traditional methods.…”

Section: Introductionmentioning

confidence: 99%

Self-Organization Characteristics of Lunar Regolith Inferred by Yutu-2 Lunar Penetrating Radar

Zhang

et al. 2021

Remote Sensing

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Most previous studies tend to simplify the lunar regolith as a homogeneous medium. However, the lunar regolith is not completely homogeneous, because there are weak reflections from the lunar regolith layer. In this study, we examined the weak heterogeneity of the lunar regolith layer using a self-organization model by matching the reflection pattern of both the lunar regolith layer and the top of the ejecta layer. After a series of numerical experiments, synthetic results show great consistency with the observed Chang’E-4 lunar penetrating radar data and provide some constraints on the range of controlling parameters of the exponential self-organization model. The root mean square permittivity perturbation is estimated to be about 3% and the correlation distance is about 5–10 cm. Additionally, the upper layer of ejecta has about 1–2 rocks per square meter, and the rock diameter is about 20–30 cm. These parameters are helpful for further study of structural characteristics and the evolution process of the lunar regolith. The relatively small correlation distance and root mean square perturbation in the regolith indicate that the regolith is mature. The weak reflections within the regolith are more likely to be due to structural changes rather than material composition changes.

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“…Since this work is the first attempt of full 3D simulation in this field, it is reasonable to start with the artificial impacts because of their well-constrained source locations, origin times, and impact parameters (e.g., kinetic energy, impact angle). Following Onodera et al (2021) who performed 2D simulation of the lunar seismic wave propagation, we adopted two SIVB rocket booster impacts: Apollo 16 SIVB and Apollo 14 SIVB impacts recorded at Apollo 12 station (Figure 2a). The computational space for each event is shown in Figure 2b-c.…”

Section: Reference Events and Work Spacementioning

confidence: 99%

“…As pointed out by Gillet et al (2017) and Onodera et al (2021), the energy growth part contains the information of the forward scattering while the decay-coda (i.e., from the peak energy to noise floor) more reflects the diffusion and intrinsic attenuation factors. Since this study focuses on the forward scattering effects, we paid closer attention to the energy growth part.…”

Section: Estimation Of Rise-timementioning

confidence: 99%

Quantitative evaluation of the lunar seismic scattering and comparison between the Earth, Mars, and the Moon

Onodera

Kawamura²,

Tanaka³

et al. 2022

Preprint

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The intense seismic scattering seen in Apollo lunar seismic data is one of the most characteristic features, making the seismic signals much different from those observed on the Earth. The scattering is considered to be attributed to subsurface heterogeneity. While the heterogeneous structure of the Moon reflects the past geological activities and evolution processes from the formation, the detailed description remains an open issue. Here we present a new model of the subsurface heterogeneity within the upper lunar crust derived through a full 3D seismic wave propagation simulation. Our simulation successfully reproduced the Apollo seismic observations, leading to a significant update of the scattering properties of the Moon. The results showed that the scattering intensity of the Moon is about ten times higher than that of the heterogeneous region on the Earth. The quantified scattering parameters could give us a constraint on the surface evolution process on the Moon and enable the comparative study for answering a fundamental question of why the seismological features are different on various planetary bodies.

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Numerical Simulation of Lunar Seismic Wave Propagation: Investigation of Subsurface Scattering Properties Near Apollo 12 Landing Site

Cited by 18 publications

References 48 publications

Largest recent impact craters on Mars: Orbital imaging and surface seismic co-investigation

Largest recent impact craters on Mars: Orbital imaging and surface seismic co-investigation

Self-Organization Characteristics of Lunar Regolith Inferred by Yutu-2 Lunar Penetrating Radar

Quantitative evaluation of the lunar seismic scattering and comparison between the Earth, Mars, and the Moon

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