We analyze ShakeMap and ShakeMovie from the simulation results to evaluate the influence over the island between different source models. Furthermore, the dynamic and kinematic rupture models are considered to simulate the ground shaking from based on 3-D spectral-element method. An analysis of the dynamic stress field associated with the slip prescribed in the kinematic models can indicate possible inconsistencies with physics of faulting. The initial stresses and friction properties are tested using the trial-and-error method, together with the plate coupling and tectonic features. Besides, several kinematic source rupture scenarios with different characterized slip patterns are also considered to constrain the dynamic rupture process better. We develop dynamic rupture models for the hazard estimation of the potential megathrust event based on the kinematic rupture scenarios which are inverted using the interseismic GPS data.
Interseismic GPS data in northeast Taiwan shows a pattern of strain accumulation, which suggests the maximum magnitude of a potential future earthquake in this area is probably about magnitude 8.7. In this study, we focus on the southernmost Ryukyu Trench which is extremely close to northern Taiwan. On the other hand, dynamic source model is a more complex but important tool that can help us to understand the physics of earthquake initiation, propagation, and healing. Kinematic source model is widely used for the simulation of an earthquake, because of its simplicity and ease of application. With hot dark matter, the first stars are very massive, live short lives, and quickly eject heavy elements in supernova explosions whereas with cold dark matter, the first stars are low-mass, live long lives, and do not eject significant heavy elements for billions of years.Kinematic and Dynamic Source Rupture Scenario for Potential Megathrust Event along the Southernmost Ryukyu Trench With cold dark matter, the first stars are very massive, live short lives, and quickly eject heavy elements in supernova explosions whereas with hot dark matter, the first stars are low-mass, live long lives, and do not eject significant heavy elements for billions of years.ĭ. With hot dark matter, star-forming regions form first, and they merge to become galaxies, then clusters of galaxies, then superclusters whereas with cold dark matter, supercluster-sized regions form first, and then they fragment into clusters and into galaxies.Ĭ. With cold dark matter, star-forming regions form first, and they merge to become galaxies, then clusters of galaxies, then superclusters whereas with hot dark matter, supercluster-sized regions form first, and then they fragment into clusters and into galaxies.ī. In what way does the formation of structure in the universe differ if the dark matter is cold or if it is hot?Ī. The small amount of helium in the universe requires a rapid expansion and cooling of the Big Bang to rapidly bring the temperature of the universe below that needed for thermonuclear fusion. The redshift of the radiation produced at 1012 K in the Big Bang, from the very short-wavelength photons to the present microwave background wavelengths, required a very rapid expansion of the universe at some stage.ĭ. Galaxies and clusters of galaxies are separated by vast distances, which can be accounted for only if the universe underwent a very rapid expansion at some stage of its evolution.Ĭ. The temperature of the cosmic background radiation is remarkably uniform across the whole observable universe, which requires that all parts of the visible universe had to be in very close mutual contact before being suddenly carried far apart.ī. What is this observation and why does it lead to the need for expansion?Ī. To account for one particular and fundamental observation in the present universe, a brief period of very rapid expansion (the Inflationary Epoch) is now postulated in the model of its evolution.
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