Torsional oscillations and observed rotational period variations in early-type stars

TL;DR

This paper investigates how internal magnetohydrodynamic waves cause torsional oscillations in early-type stars, explaining observed rotational period variations in stars like CU Vir and HD 37776 through numerical modeling.

Contribution

It introduces a model linking internal wave propagation to rotational period changes, providing explanations for observed variations in specific chemically peculiar stars.

Findings

Models reproduce CU Vir's 67.6-year cycle with a 51-year prediction.

HD 37776's cycle length exceeds 100 years, longer than model predictions.

Torsional oscillations plausibly explain period variations in CU Vir.

Abstract

Some chemically peculiar stars in the upper main sequence show rotational period variations of unknown origin. We propose these variations are a consequence of the propagation of internal waves in magnetic rotating stars that lead to the torsional oscillations of the star. We simulate the magnetohydrodynamic waves and calculate resonant frequencies for two stars that show rotational variations: CU Vir and HD 37776. We provide updated analyses of rotational period variations in these stars and compare our results with numerical models. For CU Vir, the length of the observed rotational-period cycle, $\mathit\Pi=67.6(5)$ yr, can be well reproduced by the models, which predict a cycle length of 51 yr. However, for HD 37776, the observed lower limit of the cycle length, $\mathit\Pi\geq100$ yr, is significantly longer than the numerical models predict. We conclude that torsional oscillations provide a reasonable explanation at least for the observed period variations in CU Vir.