Stellar evolution along the AGB as revealed by the shape of Miras' visual light curves

TL;DR

This study analyzes decades of visual light curves of Mira variables to better understand their evolution along the AGB, revealing new correlations between light curve shapes and stellar evolution stages.

Contribution

It provides a systematic, quantitative analysis of Mira light curves, identifying a family of sinusoidal curves and new correlations with stellar evolution not previously documented.

Findings

Identification of a sinusoidal family of light curves linked to M spectral types

Discovery of a broader luminosity minimum as stars evolve along the AGB

Revealed correlations between light curve shape parameters and stellar evolutionary state

Abstract

A new analysis of a sample of visual light curves of Mira variables is presented. The curves cover the past four decades and are selected from the AAVSO database as including a very large number of high-density and high-quality observations. The aim of the analysis is to offer a more precise, more quantitative and more systematic picture than available from earlier studies. The results corroborate earlier descriptions and reveal new correlations between the shapes of the light curves and the evolution of the star along the Asymptotic Giant Branch (AGB). A family of nearly sinusoidal curves associated with M spectral types and displaying no sign of having experienced third-dredge-up events, is identified with good confidence. A detailed study of its properties is presented and used to suggest possible interpretations. All other curves are clearly distinct from this family and usually start departing from it by displaying a broader luminosity minimum, progressively taking the form of a hump climbing the ascending branch as the star evolves along the AGB. The properties displayed by this hump are studied in some detail and possible interpretations are considered. New correlations between parameters defining the shape of the light curve and the state of the star are revealed; while the average trend is established with good confidence, deviations from it cause a significant scatter of the parameters defining the shapes of the curves. Comments aimed at shedding light on the underlying physics are presented together with speculative interpretations, in the hope that they could encourage and inspire new studies, in particular based on simulations using state-of-the-art models of the inner star dynamics.