On the understanding of pulsations in the atmosphere of roAp stars: phase diversity and false nodes

TL;DR

This paper presents a theoretical analysis of pulsations in roAp stars, accounting for magnetic effects, and explains the observed diversity of pulsation behaviors, including false nodes, through wave solutions and observational effects.

Contribution

It introduces approximate analytical solutions for pulsations in magnetic stars and clarifies the origin of diverse pulsation behaviors, including false nodes, in the atmospheres of roAp stars.

Findings

Pulsation amplitude generally increases with atmospheric height.

Pulsation phase can be constant, increasing, or decreasing with height.

Zero amplitude with phase jumps can be visual effects, not true nodes.

Abstract

Studies based on high-resolution spectroscopic data of rapidly oscillating Ap stars show a surprising diversity of pulsation behavior in the atmospheric layers, pointing, in particular, to the co-existence of running and standing waves. The correct interpretation of these data requires a careful modelling of pulsations in these magnetic stars. In light of this, in this work we present a theoretical analysis of pulsations in roAp stars, taking into account the direct influence of the magnetic field. We derive approximate analytical solutions for the displacement components parallel and perpendicular to the direction of the magnetic field, that are appropriate to the outermost layer. From these, we determine the expression for the theoretical radial velocity for an observer at a general position, and compute the corresponding pulsation amplitude and phase as function of height in the atmosphere. We show that the integral for the radial velocity has contributions from three different types of wave solutions, namely, running waves, evanescent waves, and standing waves of nearly constant amplitude. We then consider a number of case studies to illustrate the origin of the different pulsational behaviour that is found in the observations. Concerning pulsation amplitude, we find that it generally increases with atmospheric height. Pulsation phase, however, shows a diversity of behaviours, including phases that are constant, increasing, or decreasing with atmospheric height. Finally, we show that there are situations in which the pulsation amplitude goes through a zero, accompanied by a phase jumps of $\pi$, and argue that such behaviour does not correspond to a pulsation node in the outermost layers of the star, but rather to a visual effect, resulting from the observers inability to resolve the stellar surface.