Gravitational wave asteroseismology from rapidly rotating neutron stars
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The recent direct observations of gravitational waves from a binary black hole system and separately from a binary neutron star system are among the most exciting events in physics history. This is true not only because it provides another experimental proof for Einstein’s general theory of relativity, but also because it opens a new window towards future astronomical observations. More specifically it launches the branch of experimental gravitational wave asteroseismology, the objective of which is studying the physical characteristics of astrophysical systems through studying the gravitational radiation emitted by them. In some cases, like neutron stars, studying the gravitational waves emitted by such systems might be the only way to get an insight to the internal structure of such extreme systems. This thesis outlines a study of rapidly rotating neutron stars as sources of gravitational waves, using a three dimensional general relativistic hydrodynamical code.