Advanced algorithms for detection and modelling of newtonian noise for interferometric gravitational wave detectors
The Newtonian Noise (NN) is a phenomenon considered as a local change in the gravity field arising from the changes in the density of the ground due to seismic waves, as well as to the presence and motions of external masses. Considered gravitational field fluctuations have effectively very small range due to the quick fall off of the gravitational force on the reference masses of the Gravitational Wave (GW) detector. However, modern interferometric GW detectors like VIRGO and LIGO have such a high sensitivity, that taking into account the impact of the fluctuations in the gravity field, interacting in the immediate vicinity of the mirrors of the interferometer, becomes a necessity. Similarly, the major impact of the Newtonian Noise on the future gravitational wave detectors being designed, eg. Einstein Telescope (ET), seems one of the most limiting sensitivity factors at low frequencies that have direct impact on the science cases and the science quality.
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