Comments on Barker and Astoul (2021)
(2021)
Abstract:
The tidal evolution of interacting binaries when the orbital period is short compared to the primary star's convective time scale is a problem of long-standing. Terquem (2021) has argued that, when this temporal ordering scheme is obeyed, the rate of energy transfer from tides to convection (denoted $D_R$) is given by the product of the averaged Reynolds stress associated with the tidal velocity and the mean shear associated with the convective flow. In a recent response, Barker and Astoul (2021, hereafter BA21) claim to show that $D_R$ (in this form) cannot contribute to tidal dissipation. Their analysis is based on a study of Boussinesq and anelastic models. Here, we demonstrate that BA21 misidentify the correct term responsible for energy transfer between tides and convection. As a consequence, their anelastic calculations do not prove that the $D_R$ formulation is invalidated as an energy-loss coupling between tides and convection. BA21 also carry out a calculation in the Boussinesq approximation. Here, their claim that $D_R$ once again does not contribute is based on boundary conditions that do not apply to any star or planet that radiates energy from its surface, which is a key dissipational process in the problem we consider.Tidally induced stellar oscillations: converting modelled oscillations excited by hot Jupiters into observables
Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2021)
Non–adiabatic tidal oscillations induced by a planetary companion
Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2019)
Abstract:
First-order mean motion resonances in two-planet systems: general analysis and observed systems
Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2019)
CoRoT 223992193: Investigating the variability in a low-mass, pre-main sequence eclipsing binary with evidence of a circumbinary disk
(2016)