# Domains of pulsational instability of low-frequency modes in rotating upper main-sequence stars

## TL;DR

This study maps the pulsational instability regions of rotating main sequence stars with 2-20 solar masses, showing how rotation and stellar parameters influence mode stability and period spacing.

## Contribution

It provides a comprehensive analysis of how rotation and stellar properties affect pulsational instability domains in massive stars, incorporating the Coriolis force via the traditional approximation.

## Key findings

- Wider instability strips due to rotation compared to non-rotating models
- Extension of instability to hotter and more massive stars
- Rotation significantly influences period spacing patterns

## Abstract

We determine instability domains on the Hertzsprung-Russel diagram for rotating main sequence stars with masses 2-20 $\mathrm M_\odot$. The effects of the Coriolis force are treated in the framework of the traditional approximation. High-order g-modes with the harmonic degrees, $\ell$, up to 4 and mixed gravity-Rossby modes with $|m|$ up to 4 are considered. Including the effects of rotation results in wider instability strips for a given $\ell$ comparing to the non-rotating case and in an extension of the pulsational instability to hotter and more massive models. We present results for the fixed value of the initial rotation velocity as well as for the fixed ratio of the angular rotation frequency to its critical value. Moreover, we check how the initial hydrogen abundance, metallicity, overshooting from the convective core and the opacity data affect the pulsational instability domains. The effect of rotation on the period spacing is also discussed.