A Mass-Shell Model of Compact Binary Coalescence
Noah M. MacKay

TL;DR
This paper introduces a physical model of compact binary coalescence as a contracting mass shell, deriving the energy radiated as gravitational waves and comparing it with observed data from GW150914.
Contribution
It presents a novel mass-shell model based on Kerr metrics to estimate GW energy emission, providing a more physically grounded approach than previous ad hoc scalings.
Findings
Estimated GW energy for GW150914: 2.08 M_sun c^2 (simple assumptions)
Refined estimate for GW150914: 3.27 M_sun c^2, closer to observed 3.1 M_sun c^2
Derived gravitational waveforms depending on dynamic frequencies and separations
Abstract
The final pulse of gravitational wave (GW) emission is released at the peak of the chirp rise before compact binary merger. LIGO detections since GW150914 reveal a correlation between the radiated energy and the ad hoc scaling of one-tenth of the chirp mass , which begs to ask if this is physically grounded. Motivated by current effective one-body models, this work models compact binary coalescence (CBC) as a rotating, compact mass shell that is contracting towards the total mass horizon. Using a variational methodology, the Laplace-Beltrami formulation for the Ricci tensor is applied to a Kerr metric Ansatz, retrieving the energy density of the CB mass shell via the Einstein field equations. At the time of coalescence , the corresponding surface energy ultimately depends on the reduced mass of the CB, the symmetric mass ratio ,…
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Taxonomy
TopicsCosmology and Gravitation Theories · Pulsars and Gravitational Waves Research
