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Imaging seismic waves from space

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judd
18 diapositives · 340 Views · Aug 23, 2014

This study explores innovative methods for imaging seismic waves using space-based systems, focusing on the Mw 7.1 Duzce earthquake. It discusses the development of a kinematic source model based on the inversion of static ground displacement and seismograms. The research utilizes SPOT offsets, InSAR, GPS, and seismograms for data collection. Key simulations demonstrate the potential of airborne and geostationary optical telescopes for accurately measuring horizontal offsets during seismic events, offering new insights into earthquake physics and rupture dynamics.

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  1. Imaging seismic waves from space • Rémi Michel1,2, Sébastien Leprince1, Serge Primet3, S. Somala1, Jean-Paul Ampuero1, Nadia Lapusta1, Jean-Philippe Avouac1 1 California Institute of Technology, Pasadena, USA 2 Commissariat a l’EnergieAtomique, Saclay, France 3 Institutd’Optique, Palaiseau, France

  2. Motivation Source Model of the 1999, Mw 7.1 Duzce Earthquake. Data: SPOT offsets, inSAR, GPS, Seismograms (Konca et al, BSSA, 2010)

  3. Motivation (Konca et al, BSSA, 2010) Source Model of the 1999, Mw 7.1 Duzce Earthquake: An initial crack-like rupture which evolve into a super-shear pulse

  4. Motivation • Simulation of a seismic rupture: horizontal strike-parallel component of the velocity field), computed for a theoretical Mw 7.0 earthquake simulated using a rate&state friction law and the Spectral Element Method (e.g., Kaneko, Lapusta and Ampuero, 2009) t=15s 50km

  5. Motivation • The determination of a kinematic source model from the inversion of static ground displacement and seismograms measured at a sparse set of seismic stations is an ill-posed problem. • …but such models are needed to investigate Earthquake physics.

  6. Requirements 50km Mw7 -0.1 S-1 0.1 Mw6

  7. Airborne/Space Systems A Large Geostationary Optical Telescope?

  8. Photometry Essentials Wavelength (mm) Atmospheric Turbulence Wavelength (mm) Wavelength (mm) Ground Reflectance Sun Radiance Atmosphere Transmittance L:radiance, r: reflectance, S : atmosphere spherical reflectance Movie [0.4-2.5mm]

  9. Measurable quantities with Optical Systems

  10. Natural Light Fluctuations [10Hz-1Hz]

  11. Horizontal offsetsMeasured by Correlation or Optical Flow 1/100 of the pixel size. SNR 1000 (reflectance 0.15, back-illuminated CCD) : 0.03 s per frame for f 4m. Stability is an issue for data management and not for accuracy.

  12. Photoclinometry • Photoclinometry • Accuracy possible up to [10-4-10-5] (number of detected photons [1010 – 1011]) • r=0.15, pixel size : 100m, integration time 0.03s, most  unfavorable incidence angle # 11 degrees

  13. Simulations-Horizontal offsets Synthetic Mw 7.1, t=15s Telescope f10.m Telescope f4.0m Mw 6.0 t=4.22s Mw 6.0 t=4.22s Mw 6.0 t=4.22s Model (Mw 7.1, 30s, 2Hz, pixel:100m) and 2 critical telescope diameters (1Hz, pixel:100m)

  14. Simulations-Horizontal offsets Telescope f10.0m Telescope f4.0m -0.1 S-1 0.1 Accuracy 1/50th pixel

  15. f7.0m f4.0m Modele f10.0m

  16. Simulations-Photoclinometry 0.004 rad.s-1 Synthetic (Mw7) Simulation (4m)

  17. Conclusions

  18. A Accuracy of Optical Correlation = f(f telescope, geostationary) A’ Transect • Model of strike slip fault (Mw 7.1), Field of view 60*24km, 1Hz, ground resolution 100m f4.0m Ariane V Compatible Horizontal Velocities [-0.4,+1.9] (m.s-1) A Model f10.0m f7.0m f4.0m f7.0m Challenging A’ f10.0m Challenging