Gravitational Wave Heating

Abstract

It was shown in previous work that when a gravitational wave (GW) passes through a viscous shell of matter the magnitude of the GW will be damped and there are astrohysical circumstances in which the damping is almost complete. The energy transfer from the GWs to the fluid will increase its temperature. We construct a model for this process and obtain an expression for the temperature distribution inside the shell in terms of spherical harmonics. Further, it is shown that this effect is astrophysically significant: a model problem is constructed for which the temperature increase is of order $10^6{}^{\circ }$K.

References in corpus (16)

• Tests of general relativity with GW150914
• Foundations of Black Hole Accretion Disk Theory
• Fermi GBM Observations of LIGO Gravitational Wave event GW150914
• The Afterglow of Massive Black Hole Coalescence
• High-powered Gravitational News
• The eth formalism in numerical relativity
• Radio wave emissions due to gravitational radiation
• The incorporation of matter into characteristic numerical relativity
• Brightening of an Accretion Disk Due to Viscous Dissipation of Gravitational Waves During the Coalescence of Supermassive Black Holes
• Time-Dependent Models for the Afterglows of Massive Black Hole Mergers
• Linearized solutions of the Einstein equations within a Bondi-Sachs framework, and implications for boundary conditions in numerical simulations
• Photon frequency conversion induced by gravitational radiation
• Gravitational waveforms with controlled accuracy
• Initial data transients in binary black hole evolutions
• Gravitational Wave Heating of Stars and Accretion Disks
• Effect of a low density dust shell on the propagation of gravitational waves

Cited by in corpus (2)

• The interaction between gravitational waves and a viscous fluid shell on a Schwarzschild background
• Gravitational wave interactions with a viscous fluid: Core collapse supernova, binary neutron star merger, and accretion around a black hole merger