Japan Geoscience Union Meeting 2018

Presentation information

[EJ] Oral

P (Space and Planetary Sciences) » P-PS Planetary Sciences

[P-PS05] Lunar science and exploration

Wed. May 23, 2018 9:00 AM - 10:30 AM A01 (Tokyo Bay Makuhari Hall)

convener:Hiroshi Nagaoka(Waseda Univ.), Tomokatsu Morota(Graduate School of Environmental Studies, Nagoya University), Masaki N (名古屋大学宇宙地球環境研究所, 共同), Masahiro KAYAMA(Department of Earth and Planetary Material Sciences, Faculty of Science, Tohoku University), Chairperson:Morota Tomokatsu(名古屋大学大学院 環境学研究科), Ohtake Makiko(JAXA)

10:15 AM - 10:30 AM

[PPS05-06] Scattering Effects of Lunar Surface and Moho Topographies on the Propagation of Deep Moonquakes

*Keisuke Onodera1,2, Taichi Kawamura3,4, Yoshiaki Ishihara2, Takuto Maeda5, Satoshi Tanaka2 (1.SOKENDAI (The Graduate University for Advanced Studies), 2.Institute of Space and Astronautical Science/Japan Aerospace Exploration Agency, 3.Institut de Physique du Globe de Paris, 4.National Astronomical Observatory of Japan, 5.Earthquake Research Institute, The University of Tokyo)

Keywords:Moon, Moonquake, Internal structure, Planetary seismology

The internal structure of the Moon is one of the most essential information to understand its origin and evolution. To elucidate the lunar inner structure, seismic observation is one of the most effective ways. In Apollo missions, some seismometers were deployed on the Moon and carried out the observation for about eight years. Since then, the lunar internal structure has been estimated using Apollo seismic data. Although several lunar interior models were proposed so far (e.g. [1][2][3]), each model shows different structure. However, all proposed models can explain the Apollo data. As the uncertainties in arrival time of seismic phases and resulting source locations are quite large, we can obtain several solutions for the inner structure of the Moon.

Low S/N ratio and long coda make it difficult to pick the seismic phases up in lunar seismograms. It is said long coda is caused by intense scattering and low attenuation within the lunar crust. So, understanding the scattering mechanism might improve the determination of the internal structure. Although the source of the lunar coda is not well understood, several ideas are suggested in previous studies (e.g. regolith and mega-regolith layer, local structure, velocity inhomogeneity [4][5]). There are theoretical and experimental studies on the scattering by regolith and mega-regolith [4][5]. However, there are few studies as for the effect of the local structure of the Moon. Recent studies of earthquakes suggested that, besides velocity inhomogeneity, local topographies scatter the seismic wave and develop the long-duration coda [6]. So, in this study, we investigated the scattering effects of the local topographies (surface & Moho) of the Moon on the seismic wave propagation. We assumed 1D velocity model and SELENE moon structure model based on [7] and simulated the propagation of deep moonquakes using OpenSWPC (an Open-source Seismic Wave Propagation Code) [8]. Then, we compared results of both models and evaluated how much surface and Moho topographies scatter the seismic wave.

In the presentation, we will show the results of simulation and discuss the effects of local topographies.

[1] Nakamura et al. (1982), Proc. LPSC, 13th, 117-123.
[2] Lognonne et al. (2003), EPSL, 211, 27-44.
[3] Garcia et al. (2011), PEPI, 188, 96-113.
[4] Toksoz et al. (1974), RGSP, 12, 539-567.
[5] Blanchette-Guertin et al. (2012), JGR, 117, E06003.
[6] Takemura et al. (2015), GJI, 201, 459-474.
[7] Ishihara et al. (2009), GRL, 36, L19202.
[8] Maeda et al. (2017), EPS, 69:112.