2D non-perturbative modeling of oscillations in rapidly rotating stars

TL;DR

This paper introduces a 2D non-perturbative computational method that accurately models oscillation modes in rapidly rotating stars by accounting for centrifugal distortion and Coriolis effects.

Contribution

The paper presents a novel 2D non-perturbative approach for modeling stellar oscillations in rapid rotators, improving accuracy over previous methods.

Findings

Successfully models oscillation modes in various types of rapidly rotating stars.

Accounts for centrifugal distortion and Coriolis acceleration effects.

Applicable to high order p-modes and low order p- and g-modes.

Abstract

We present and discuss results of a recently developped two dimensional non-perturbative method to compute accurate adiabatic oscillation modes of rapidly rotating stars . The 2D calculations fully take into account the centrifugal distorsion of the star while the non-perturbative method includes the full influence of the Coriolis acceleration. These characteristics allows us to compute oscillation modes of rapid rotators - from high order p-modes in $\delta$Scuti stars, to low order p- and g-modes in $\beta$ Cephei or Be stars.