Tidal dissipation in rotating fluid bodies: the presence of a magnetic field. Issue 2 (25th October 2017)

• Record Type: Journal Article
• Authors: Lin, Yufeng; Ogilvie, Gordon I.
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 474:Issue 2(2018)
• Page Start: 1644
• Page End: 1656
• Publication Date: 2017-10-25
• Subjects: MHD -- waves -- planet-star interactions stars: magnetic field; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stx2764
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: We investigate effects of the presence of a magnetic field on tidal dissipation in rotating fluid bodies. We consider a simplified model consisting of a rigid core and a fluid envelope, permeated by a background magnetic field (either a dipolar field or a uniform axial field). The wave-like tidal responses in the fluid layer are in the form of magnetic Coriolis waves, which are restored by both the Coriolis force and the Lorentz force. Energy dissipation occurs through viscous damping and Ohmic damping of these waves. Our numerical results show that the tidal dissipation can be dominated by Ohmic damping even with a weak magnetic field. The presence of a magnetic field smooths out the complicated frequency dependence of the dissipation rate, and broadens the frequency spectrum of the dissipation rate, depending on the strength of the background magnetic field. However, the frequency-averaged dissipation is independent of the strength and structure of the magnetic field, and of the dissipative parameters in the approximation that the wave-like response is driven only by the Coriolis force acting on the non-wavelike tidal flow. Indeed, the frequency-averaged dissipation quantity is in good agreement with previous analytical results in the absence of magnetic fields. Our results suggest that the frequency-averaged tidal dissipation of the wave-like perturbations is insensitive to detailed damping mechanisms and dissipative properties.