2020/08/31 by Parthasarathi Majumdar, Anarya Ray
Physics and Astronomy · #Astrophysics #Binary black hole #Binary number #Black Holes and Theoretical Physics #Black hole (networking) #Cosmology and Gravitation Theories #Gravitation #Gravitational wave #LIGO #Neutron star #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Upper and lower bounds #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.104.044036
published as Phys. Rev. D 104, 044036 (2021) · 8 pages Revtex with three figures in .png format
arxiv created 2021/05/03 · openalex publication_date 2021/08/17 · arxiv updated 2021/08/25 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Using concomitantly the generalized second law of black hole thermodynamics and the holographic Bekenstein entropy bound embellished by loop quantum gravity corrections to quantum black hole entropy, we show that the boundary cross sectional area of the postmerger remnant formed from the compact binary merger in gravitational wave detection experiments like GW150914 et seq., by the LIGO-VIRGO collaboration, is bounded from below. This lower bound is more general than the bound obtained from application of Hawking's classical area theorem for black holes, since it does not depend on whether the inspiralling compact binary pair or the postmerger remnant consists of black holes or other exotic compact objects. The derivation of the bound entails an estimate of the entropy of the gravitational waves emitted during the binary merger, which adapts to gravitational waves an extant formalism proposed originally for particle ensembles. The results for the minimal cross sectional area of the merger remnant due to binary compact mergers observed recently by the LIGO-VIRGO collaboration are discussed. While accurate measurement of the mass of the remnant for the binary neutron star merger GW170817 remains a challenge, we provide a proof of principle that for binary neutron star mergers our lower bound on the cross sectional area of the remnant provides an alternative approach to probe the validity of neutron star equations of state, independent of the tidal deformabilities of the components.