Circumstellar dust shells around long-period variables. X. Dynamics of envelopes around standard luminous, C-rich AGB stars

TL;DR

This study investigates the complex dynamics of circumstellar dust shells around carbon-rich, luminous AGB stars, revealing how stellar pulsations and dust formation influence envelope behavior, including multi-periodicity and irregular oscillations.

Contribution

It introduces a numerical model analyzing the dynamical response of dust shells to stellar pulsations, identifying normal modes and their relation to dust formation timescales.

Findings

CDSs exhibit multi-oscillatory behavior driven by stellar pulsations.

Normal modes have periods around 10^3 days linked to dust processes.

Envelope responses vary from periodic to irregular depending on star's oscillation.

Abstract

Long-period variables (LPVs) and Miras are highly evolved stars at the upper region of the asymptotic giant branch. They exhibit a pronounced variability of their luminosity with a more or less well defined period and suffer large mass loss in the form of stellar winds. Due to this extensive mass loss, LPVs and Miras are surrounded by extended circumstellar dust shells (CDSs). The dynamics of these envelopes is the result of a complex interplay via an external excitation by the pulsating central star, dust formation and radiative transfer. Our study is aimed at an understanding of the dynamics of CDSs around carbon-rich, standard luminous LPVs and Miras. These shells often show multiperiodicity with secondary periods as high as a few 10^4 d superimposed on a main period which is in the range of approximately 10^2-10^3 d. Such secondary periods may be caused at least in part by the presence of dust. We consider an excitation of the CDSs by either a harmonic force, provided by the oscillation of the central star, or by a stochastic force with a continuous power spectrum. The resulting numerically computed dynamical behaviour of the shell is analysed with the help of Fourier analysis and stroboscopic maps. CDSs may be described as multioscillatory systems which are driven by the pulsating stars. A set of normal modes can be identified. The obtained periods of these modes are of the order of some 10^3 d, which is a characteristic timescale for dust nucleation, growth and elemental enrichment in the dust formation zone. Depending on the oscillation period and strength of the central star, the envelope reacts periodically, multi- periodically or irregularly.