Reduced Model for Gravitational Wave Sources
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One of the most interesting and exotic systems in the universe is a system of two black holes. When black holes orbit each other, they will eventually collide, forming a single black hole with a mass less than the sum of the two initial masses. This missing ``mass," up to ten percent, is converted into gravitational waves (GW) making these systems one of the most energetic in the universe. In the last decade, numerical simulations of the coalescence of binary black hole spacetimes have become a possibility and have since then progressed. Each simulation, with a unique set of initial parameters, constructs a gravitational wave signal, also called a waveform. In this work, I study the modeling of the radiated energy of non-precessing and precessing systems as functions of the binary system' s initial parameters. Because constructing a template bank of these waveforms remains computationally intensive, the next step is to introduce the use of Principal Component Analysis (PCA), which will efficiently capture the essential features over a large parameter space of the simulations. It acts on collections of waveforms to find bulk features such as the energy and momentum radiated. These features may provide the ``smoking gun" of mergers for gravitational wave burst detection.