Amplitudes of low frequency modes in rotating B type stars

TL;DR

This paper estimates the amplitudes of low frequency oscillation modes in rotating B-type stars using non-linear theory, highlighting the role of r-modes and non-linear coupling in amplitude determination.

Contribution

It introduces a method to compute equilibrium amplitudes of low frequency modes in rotating B stars considering non-linear coupling and rotation effects.

Findings

r-modes significantly influence amplitude determination

low m modes have surface luminosity amplitudes of 10^{-4} to 10^{-3}

rotation affects mode amplitudes through non-linear coupling

Abstract

Using weakly non-linear theory of oscillation, we estimate the amplitudes of low frequency modes in a slowly pulsating B (SPB) star, taking account of the effects of rotation on the modes. Applying the formulation by Schenk et al (2002), we compute non-linear coupling coefficient between the low frequency modes and estimate the equilibrium amplitudes of the modes excited in the star, assuming the amplitudes of the unstable modes are saturated as a result of non-linear coupling with stable modes, that is, as a result of parametric instability expected between one unstable mode and two stable modes. We use the traditional approximation to calculate adiabatic and non-adiabatic oscillations in a rotating star. We find $r$-modes in a rapidly rotating star play a significant role in the amplitude determination through non-linear coupling. We also find that for low $m$ modes, the fractional amplitudes of the radiative luminosity caused by the low frequency modes are of order $10^{-4}$ to $10^{-3}$ at the surface.