The red giant branch phase transition: Implications for the RGB luminosity function bump and detections of Li-rich red clump stars

TL;DR

This study investigates the red giant branch phase transition, revealing critical ages affecting luminosity features and suggesting a connection to Li-rich red clump stars, with implications for stellar evolution understanding.

Contribution

It provides detailed stellar models across the transition, identifying critical ages and luminosity behaviors, and explores links to Li-rich star observations.

Findings

Critical age of 1.1-1.2 Gyr causes sharp luminosity drop.

Narrow age range where RGB bump exceeds He ignition luminosity.

Potential link between luminosity features and Li-rich red clump stars.

Abstract

We performed a detailed study of the evolution of the luminosity of He-ignition stage and of the red giant branch bump luminosity during the red giant branch phase transition for various metallicities. To this purpose we calculated a grid of stellar models that sample the mass range of the transition with a fine mass step equal to ${\rm 0.01M_\odot}$. We find that for a stellar population with a given initial chemical composition, there is a critical age (of 1.1-1.2~Gyr) around which a decrease in age of just 20-30 million years causes a drastic drop in the red giant branch tip brightness. We also find a narrow age range (a few $10^7$ yr) around the transition, characterized by the luminosity of the red giant branch bump being brighter than the luminosity of He ignition. We discuss a possible link between this occurrence and observations of Li-rich core He-burning stars.