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

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, $\Pi =67.6(5)$ 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, $\Pi \ge 100$ 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.

7 pages, accepted for publication in MNRAS

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Cited by in corpus (6)

• Modeling of Magneto-Rotational Stellar Evolution I. Method and first applications
• The accelerating rotation of the magnetic He-weak star HD 142990
• HST/STIS analysis of the first main sequence pulsar CU Vir
• Large amplitude change in spot-induced rotational modulation of the Kepler Ap star KIC 2569073
• HD 60431, the CP2 star with the shortest rotational period -- Physical parameters and period analysis
• Standing torsional Alfvén waves as the source of the rotational period variation in magnetic early-type stars