Viscous Boundary-Layer Damping of r-Modes in Neutron Stars.

摘要: Recent work has raised the exciting possibility that r-modes (Rossby waves) in rotating neutron star cores might be strong gravitational-wave sources. We estimate effect of a solid crust on their viscous damping rate and show dissipation boundary layer between oscillating fluid nearly static is more than 105 times higher from shear throughout interior. This increases minimum frequency for onset gravitational r-mode instability to at least 500 Hz when core temperature less 1010 K. It eliminates conflict accretion-driven spin-up scenario millisecond radio pulsars makes it unlikely active accreting stars. For newborn stars, formation shortly after birth affects spin-down hence detectability by ground-based interferometric detectors.