Longitudinal drift of Tayler instability eigenmodes as a possible explanation for super-slowly rotating Ap stars

Abstract

Context. Rotation periods inferred from the magnetic variability of some Ap stars are incredibly long, exceeding ten years in some cases. An explanation for such slow rotation is lacking. Aims. This paper attempts to provide an explanation of the super-slow rotation of the magnetic and thermal patterns of Ap stars in terms of the longitudinal drift of the unstable disturbances of the kink-type (Tayler) instability of their internal magnetic field. Methods. The rates of drift and growth were computed for eigenmodes of Tayler instability using stellar parameters estimated from a structure model of an A star. The computations refer to the toroidal background magnetic field of varied strength. Results. The non-axisymmetric unstable disturbances drift in a counter-rotational direction in the co-rotating reference frame. The drift rate increases with the strength of the background field. For a field strength exceeding the (equipartition) value of equal Alfven and rotational velocities, the drift rate approaches the proper rotation rate of a star. The eigenmodes in an inertial frame show very slow rotation in this case. Patterns of magnetic and thermal disturbances of the slowly rotating eigenmodes are also computed. Conclusions. The counter-rotational drift of Tayler instability eigenmodes is a possible explanation for the observed phenomenon of super-slowly rotating Ap stars.

Magnetic field measurements of sharp-lined Ap stars

“…It was also suggested that weak-field Ap stars may potentially represent a significant fraction of the group of very slowly rotating stars, with rotation periods reaching several hundred years (Mathys 2020a). An explanation for the extremely slow rotation of a fraction of Ap stars is currently missing, although a first theoretical attempt to understand this phenomenon was recently presented by Kitchatinov, Potravnov & Nepomnyashchikh (2020), who suggested a possible scenario in terms of a longitudinal drift of the unstable disturbances of a kink-type (Tayler) instability of the stellar internal magnetic field.…”