Sub-photospheric fluctuations in magnetized radiative envelopes: contribution from unstable magnetosonic waves

TL;DR

This paper investigates how magnetosonic waves become unstable in the radiative envelopes of massive stars due to the Radiation-Driven Magneto-Acoustic Instability, revealing conditions that lead to sub-photospheric velocity fluctuations.

Contribution

It provides a detailed analysis of the RMI in stellar models across a wide mass range, showing how magnetic fields induce instabilities independent of convection zones.

Findings

Fast magnetosonic modes unstable down to optical depths of a few tens.

Unstable slow modes extend beyond the iron convection zone.

Predicted velocity fluctuations range from 0.1 to 10 km/s.

Abstract

We examine the excitation of unstable magnetosonic waves in the radiative envelopes of intermediate- and high-mass stars with a magnetic field of ~kG strength. Wind clumping close to the star and microturbulence can often be accounted for when including small-scale, sub-photospheric density or velocity perturbations. Compressional waves - with wavelengths comparable to or shorter than the gas pressure scale height - can be destabilized by the radiative flux in optically-thick media when a magnetic field is present, in a process called the Radiation-Driven Magneto-Acoustic Instability (RMI). The instability does not require radiation or magnetic pressure to dominate over gas pressure, and acts independently of sub-surface convection zones. Here we evaluate the conditions for the RMI to operate on a grid of stellar models covering a mass range $3-40M_\odot$ at solar metallicity. For a uniform 1kG magnetic field, fast magnetosonic modes are unstable down to an optical depth of a few tens, while unstable slow modes extend beyond the depth of the iron convection zone. The qualitative behavior is robust to magnetic field strength variations by a factor of a few. When combining our findings with previous results for the saturation amplitude of the RMI, we predict velocity fluctuations in the range ~0.1-10 km/s. These amplitudes are a monotonically increasing function of the ratio of radiation to gas pressure, or alternatively, of the zero-age main sequence mass.