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Tidal inertial waves in the differentially rotating convective envelopes of low-mass stars - I. Free oscillation modes | | M. Guenel
; C. Baruteau
; S. Mathis
; M. Rieutord
; | | Date: |
18 Jan 2016 | | Abstract: | Star-planet tidal interactions may result in the excitation of inertial waves
in the convective region of stars. In low-mass stars, their dissipation plays a
prominent role in the long-term orbital evolution of short-period planets.
Turbulent convection can sustain differential rotation in their envelope, with
an equatorial acceleration (as in the Sun) or deceleration, which can modify
the waves’ propagation properties. We explore in this first paper the general
propagation properties of free linear inertial waves in a differentially
rotating homogeneous fluid inside a spherical shell. We assume that the angular
velocity background flow depends on the latitudinal coordinate only, close to
what is expected in the external convective envelope of low-mass stars. We use
i) an analytical approach in the inviscid case to get the dispersion relation,
from which we compute the characteristic trajectories along which energy
propagates. This allows us to study the existence of attractor cycles and infer
the different families of inertial modes; ii) high-resolution numerical
calculations based on a spectral method for the viscous problem. We find that
modes that propagate in the whole shell (D modes) behave the same way as with
solid-body rotation. However, another family of inertial modes exists (DT
modes), which can propagate only in a restricted part of the convective zone.
Our study shows that they are less common than D modes and that the
characteristic rays and shear layers often focus towards a wedge - or
point-like attractor. More importantly, we find that for non-axisymmetric
oscillation modes, shear layers may cross a corotation resonance with a local
accumulation of kinetic energy. Their damping rate scales very differently from
what we obtain for standard D modes and we show an example where it is
independent of viscosity (Ekman number) in the astrophysical regime in which it
is small. | | Source: | arXiv, 1601.4617 | | Services: | Forum | Review | PDF | Favorites | |
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