Modelling the post-Newtonian test-mass gravitational wave flux function for compact binary systems using Chebyshev polynomials

摘要: We introduce a new method for modelling the gravitational wave flux function of test-mass particle inspiralling into an intermediate mass Schwarzschild black hole which is based on Chebyshev polynomials first kind. It believed that these ratio inspiral events (IMRI) are expected to be seen in both ground- and space-based detectors. Starting with post-Newtonian expansion from perturbation theory, we approximation function, due process called economization gives model faster convergence than either post-Newtonian- or Pade-based methods. As well as having excellent properties, also very closely related elusive minimax polynomial. find at last stable orbit, error between numerically calculated reduced, 0.99, smaller errors, <1/10%, estimation chirp when compared fiducial exact waveform, constructed using numerical expression orbital energy again all orders approximation. show case, template superior PN Pade approximant templates, especially lower