Assessing the validity of the anelastic and Boussinesq approximations to model solar inertial modes

¹ Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
² Institut für Astrophysik und Geophysik, Georg-August-Universtät Göttingen, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany

^⋆ Corresponding authors; zhux@mps.mpg.de; gizon@mps.mpg.de

Received: 30 December 2024
Accepted: 27 January 2025

Abstract

Context. Global-scale inertial modes of oscillations have been recently observed on the Sun. They might play an important dynamic and diagnostic role for the Sun.

Aims. This work aims to assess the validity of simplifying assumptions in the continuity equation, which have often been used in the linear models of solar inertial modes.

Methods. We compute the linear eigenmodes of the Sun’s convection zone in the inertial frequency range using the Dedalus code. This single framework enables us to compare the sensitivity of the modes to different model setups, such as the compressible setup and the Boussinesq and anelastic approximations. We consider both the cases of uniform rotation and solar differential rotation (as given by helioseismology).

Results. We find that the compressible and anelastic models have almost identical eigenmodes under uniform and solar differential rotation. On the other hand, the absence of density stratification in the Boussinesq model results in significantly different eigenmodes under this formulation. The differences are most prominent for the non-toroidal modes with significant radial motions mainly due to the absence of the compressional β effect.

Conclusions. The anelastic approximation simplifies the calculations and reduces the numerical cost without affecting the solar inertial modes. The Boussinesq or incompressible approximations cannot be used to model the solar inertial modes accurately. Given the strong influence of differential rotation on the eigenmodes, an acceptable setup is to use the anelastic approximation together with the solar differential rotation.